Author name code: kotov
ADS astronomy entries on 2022-09-14
author:"Kotov, Valery A."
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Title: The fine structure of the rotational periods of the solar
mean magnetic field
Authors: Haneychuk, Vasily Ivanovich; Kotov, Valery Alexandrovich
Bibcode: 2021OAst...30..176H
Altcode:
The data of mean magnetic field (MMF) of the Sun obtained at the Wilcox
Solar Observatory (Stanford, USA) in 1975-2020 are analysed. It was
concluded that the MMF maximum occurs, on average, 1.5-2 years later
relative to the maximum of Wolf numbers. To analyze the changes
in the MMF, a new method for searching for periodicities has been
developed, which takes into account the change in the sign of the
magnetic field from cycle to cycle. This method made it possible to
find the main synodic periods of rotation of the magnetic field with
values of 27d.021 ± 0d.008, 26d.796
± 0d.008 and 27d.260 ± 0d.008, each
of which has two splitting components associated with a change in the
polarity of the magnetic field during the transition from one cycle of
solar activity to another. The stability of these periodicities for more
than 45 years indicates that the Sun as a star looks like a horizontal
magnetic dipole (in addition to the observed vertical one), which
changes its sign every 11 years and rotates with different periods.
Title: Oscillations of solar photosphere: 45 years of observations
Authors: Kotov, Valery A.; Haneychuk, Vasilij I.
Bibcode: 2020AN....341..595K
Altcode:
A summary of the long-term, 1974-2018, measurements of the
line-of-sight velocity of the solar photosphere, performed at the
Crimean Astrophysical Observatory, is presented. The work shows that
the Sun is pulsating with two periods: P0 = 9,600.606(12)
s and P1 = 9,597.924(13) s. The new measurements, 1996-2018,
confirm the remarkable phase stability of the second period. The true
origin of both pulsations is unknown, but their beatings are noted to
have occurred with a period of 397.7(2.6) days, coinciding well with
the synodic period of Jupiter, 398.9 days. A hypothesis is advanced
that the shift from P0 to P1 is induced by the
gravity field of Jupiter.
Title: Rotation anomaly of the Sun
Authors: Kotov, Valery A.
Bibcode: 2020AN....341..588K
Altcode:
Does the Sun always rotate correctly? On the basis of the measurements
of its mean magnetic field (more than 27 thousand daily values,
obtained by seven observatories during 1968-2018) and resonance
relations of the solar system, the sidereal spin period of the Sun as
a star is determined as 25.165(6) days and that of the solar equator
as 25.081(7) days. After 1993, however, a remarkable violation of
the solar equatorial rate, through an unknown cause, has happened:
the spin coherency of the mean field disintegrated and made way for
nearly chaotic variations with quasi-periods of 24.7-25.4 days. The
phenomenon is thought to be tied to anomaly of the Wolf cycles 23 and
24, accompanied presumably by a global change of the Earth's climate
(with unclear mechanism of the Sun-Earth influence).
Title: Superfast Exoplanets and 9600 s
Authors: Kotov, V. A.
Bibcode: 2019EM&P..123....1K
Altcode: 2019EM&P..tmp....6K
Motion of a substantial part of the superfast exoplanets is found
to be in the close resonance with the well-known "solar" timescale
P0 ≈ 0.11 days and/or the timescale 2P_0/π ≈ 0.07 days
(at 99.9% confidence for exoplanet periods P < 2 days). There is
also a noticeable lack of the exoplanetary "unstable" orbits with
P ≈ 3 π P_0 ≈ 1.05 days, which copies the famous "period gap"
of the cataclysmic variables at P ≈ 0.11 days; strangely enough,
the ratio of the central periods of these two gaps is equal to π
^2. The exoplanet phenomenon is supposed to be caused by a coherent,
with the P_0 timescale, oscillation of gravity, operating within the
extra-solar planetary systems.
Title: Is the Earth's orbital motion linked to the spin rotation of
the Sun?
Authors: Kotov, V. A.
Bibcode: 2019AdSpR..63.3385K
Altcode:
Time variations of the magnetic field of the Sun, seen as a star (the
data 1968-2018, with more than 27 thousand daily measurements of the
solar mean magnetic field), allowed to specify the rotation period of
the gravitating solar mass: 27.027(6) days, synodic. This indicates
a presumably unknown physical connection between motions of the Sun
and the Earth: in the course of a year our star accomplishes nearly
27 half-revolutions, while the planet itself performs an identical
number of its spinnings during one complete axial revolution of the
Sun. True origin of this strange Sun-Earth resonance is unknown,
but it is supposed the phenomenon might be caused by slight coherent
perturbations of gravity within the solar system.
Title: Near-annual variation of the magnetic Sun
Authors: Kotov, V. A.
Bibcode: 2019Ap&SS.364...45K
Altcode:
Over past 51 years (1968-2018) the general magnetic field of the Sun
was measured nearly each day by the Crimean Astrophysical Observatory,
the Wilcox Solar Observatory and five others. It is shown that the
annual variation of this field (longitudinal component), thought to be
caused by the inclination of the Sun's axis to ecliptic, is splitted
into two components with periods 0.954(3) years and 1.034(4) years
(with mean amplitudes ≈ 0.044 G). But while the first one agrees
well with the expected period 0.957(4) years (caused by the 11-year
polar field reversals and coupled to the yearly projection effect),
the second one is shifted relative to its theoretical value, 1.047(4)
years, by Δ = 0.013(5) years (99% confidence). The beat period of the
two observed components, 12.3(7) years, agrees well with the Jovian
period 11.9 years, being close also to the length of the 11-year
cycle. Since the modern astronomy rejects a planetary influence on
the Sun, the origin of both the 1.034-year periodicity and the shift
Δ remains to be mysterious.
Title: Fast Spinning of Planets
Authors: Kotov, V. A.
Bibcode: 2018EM&P..122...43K
Altcode: 2018EM&P..tmp...15K
Spin periods of Jupiter, Saturn, Uranus and Neptune are specified by
the analysis of the resonant motion of large satellites: P = 0.445(2)
d, 0.448(1) d, 0.673(9) d and 0.561(7) d, respectively. They occur to
be near-commensurate with P_0=9600.606(12) s, the period of the "cosmic"
oscillation, discovered first in the Sun, then in other variable objects
of the Universe. The like analysis of spin rates of the total set of the
largest and fastest rotators of the Solar system (with mean diameters
≥ 500 km and P < 2 d,—of planets, asteroids and satellites)
resulted in the best commensurable, or "synchronizing", timescale
9594(65) s, coinciding fairly well with P_0 too (the probability that
the two timescales could agree by chance, is less than 10^{-5}). True
origin of this odd common resonance of our planetary system is unknown.
Title: Harmony of the solar system
Authors: Kotov, V. A.
Bibcode: 2018AN....339..513K
Altcode:
From 1968 to 2017, the Crimean Astrophysical Observatory, the Wilcox
Solar Observatory, and five other observatories performed more
than 27 thousand daily measurements of the mean magnetic field of
the Sun-as-a-star. These data reveal the presence of the long-term
coherent periodicity PS = 13.4582(25) days, characterizing
the four-sector pattern of the magnetic Sun. To clear up the origin
of this periodicity, motions of planets and massive satellites are
considered in detail. It is shown that the best commensurate timescale
of all those periodic motions is equal to PG = 13.4577(10)
days, which agrees fairly well with PS (the probability
of a chance coincidence is less than 2 × 10-9). Physical
nature of this odd PS-PG resonance is unknown,
but it is supposed that the phenomenon is caused by coherent periodic
fluctuations of the gravity field within the solar system.
Title: Motion of the fast exoplanets
Authors: Kotov, Valery A.
Bibcode: 2018Ap&SS.363...55K
Altcode:
It is shown that a number of superfast, with periods < 2 d,
exoplanets revolve around parent stars with periods, near-commensurate
with PE and/or 2 PE / π, where the exoplanet
resonance timescale PE=9603(85) s agrees fairly well with
the period P0= 9600.606(12) s of the so-called "cosmic
oscillation" (the probability that the two timescales would coincide
by chance is near 3 ×10^{-4}; the P0 period was discovered
first in the Sun, and later on—in other objects of Cosmos). True
nature of the exoplanet P0 resonance is unknown.
Title: Rotation of the Solar Equator
Authors: Kotov, V. A.
Bibcode: 2017SoPh..292...76K
Altcode:
Regular measurements of the general magnetic field of the Sun, performed
over about half a century at the Crimean Astrophysical Observatory,
the J. Wilcox Solar Observatory, and five other observatories, are
considered in detail for the time 1968 - 2016. They include more
than twenty-six thousand daily values of the mean line-of-sight field
strength of the visible solar hemisphere. On the basis of these values,
the equatorial rotation period of the Sun is found to be 26.926(9)
d (synodic). It is shown that its half-value coincides within error
limits with both the main period of the magnetic four-sector structure,
13.4577(25) d, and the best-commensurate period of the slow motions of
the major solar system bodies, 13.479(22) d (sidereal). The probability
that the two periods coincide by chance is estimated to be about
10−7. The true origin of this odd resonance is unknown.
Title: Solar 22 years cycle
Authors: Kotov, Valery A.; Sanchez, Francis M.
Bibcode: 2017Ap&SS.362....6K
Altcode:
Seven observatories performed in 1968-2015 numerous daily measurements
of general magnetic field of the Sun seen as a star (of a mean
line-of-sight field component of the visible solar hemisphere). The
new data 2013-2015 confirmed the recent prediction about saw-edged
profile of the mean curve of the Hale's 22 years magnetic cycle and,
thus, a hypothesis about its cosmological (partial) origin. This is
supported by a special analysis of epochs of extrema of Wolf's sunspot
number, demonstrating a remarkable stability, since Galileo's time,
of the initial phase of the cycle, which can hardly be explained by
dynamo theory exclusively.
Title: The Jovian period in the Sun?
Authors: Kotov, V. A.
Bibcode: 2015AdSpR..56.1276K
Altcode:
The 41-year measurements of the Doppler effect of the photosphere
performed at the Crimean Astrophysical Observatory, discovered
two periods of global oscillations of the Sun: 9600.606(12) s and
9597.929(15) s. Their beat period, 398.4(2.9) d, well agrees with a
synodic orbital period of Jupiter, PJ = 398.9 d, raising a
new problem for solar physics, cosmogony and cosmology. A hypothesis
is advanced that the PJ beating of the Sun is induced by
gravitation of Jupiter, revolving in a privileged reference system
"the Sun - the Earth".
Title: On the origin of the 22 years solar cycle
Authors: Kotov, V. A.
Bibcode: 2015AdSpR..55..979K
Altcode:
Measurements of the general magnetic field of the Sun seen as
a star were performed over last 45 years by the CrAO and five
other observatories (1968-2012, nearly 23 thousand daily strengths
B). Analysis of the B time series showed that the most substantial
long-term period of the field variation is the Hale's cycle 22 years,
which cannot be explained by dynamo theory. It reveals a saw-edged
profile, indicating perhaps a cosmic origin of the cycle.
Title: Extrasolar worlds: We should contact aliens?
Authors: Kotov, V. A.
Bibcode: 2013BCrAO.109..136K
Altcode:
More than 840 exoplanets have been discovered and many people
believe that on some of these planets there may be extraterrestrial
civilizations. Astronomers, however, warn against contacts with
aliens because of the possible dangers to humankind… In this paper
I show that the solar system is a unique phenomenon in the universe
and there cannot be any extraterrestrial civilizations. Being the
"anthropic center" of the world, the earth and the sun are "designed"
for the development of humankind and the cosmos as a supercomputer. This
conclusion follows from an analysis of exoplanet orbits that is based
on a coherent cosmic oscillation with a period of P 0 ≈
9600.6 s (discovered in the sun and some extragalactic sources). The
non-Doppler nature of the P 0 phenomenon is emphasized;
this phenomenon appears to be related to the absolute time of the
universe in the Newtonian sense.
Title: The newtonian constant
Authors: Kotov, V. A.
Bibcode: 2013BCrAO.109..142K
Altcode:
The data on the coherent cosmic oscillation (with a period of 9600.6 s)
and the finely tuned relationships between the constants of the micro-
and macroworlds is used to adjust the Newtonian constant: G = 6.67543(2)
× 10-8 cm3 g-1 s-2.
Title: Whether There is an Astrophysical Source in the Oscillations
of Geophysical Parameters with a Period of 160 Minutes?
Authors: Samsonov, S.; Miroshnichenko, L.; Kotov, V.; Skryabin, N.;
Timofeev, V.; Baishev, D.
Bibcode: 2013OAP....26..279S
Altcode:
Oscillations with a period of 160 minutes in the ground pressure and
Z-component of the geomagnetic field revealed by authors earlier are
studied the regular ground measurements. For the analysis the data
of five stations on the territory of Europe (Moscow, Apatity, Oulu)
and Siberia (Yakutsk, Tixie) obtained in December, 2003 are used. It
is shown that the specified oscillations revealed by authors earlier,
are manifested in Europe and Siberia synchronously. For December, 2003
the mean amplitude of oscillations in the ground pressure accounts for
0.012±0.002 mb; in a Z-component their value is equal to 0.323±0.070
nT. Authors discuss the possible nature of pulsations.
Title: Enigmas in measurements of solar magnetic field
Authors: Kotov, V. A.
Bibcode: 2012BCrAO.108...20K
Altcode:
The mean magnetic field (MMF) of the photosphere of the Sun as a star
was measured in 2001-2010 at the Crimean Astrophysical Observatory
using two Fe I absorption lines with λ = 524.7 nm and λ = 525.0
nm. The regression coefficient b for 1054 pairs of daily values measured
simultaneously on both lines equals 0.82 (a correlation coefficient is
0.94; magnetic field strengths determined by the line with λ = 525.0
nm are lower than those for the line with λ = 524.7 nm). However,
the b value varied significantly along with phases of the 11-year
cycle from 0.88 in 2003 to 0.49 in 2009. It is difficult to ascribe
these variations to purely instrumental or solar causes. Moreover,
the semiannual value of b decreased with the decrease in the absolute
strength of the MMF, which contradicts the model of thin magnetic flux
ropes of the photosphere. Similar behavior of b was also observed in
the comparison of MMF measured at the Crimean Astrophysical Observatory
and Stanford by the line with λ = 525.0 nm. The inconsistency of the
results obtained by these two iron lines on different instruments
has been noted. It has been concluded that the variance in and odd
behavior of b are predetermined not only by the instrument and the Sun
(by the so-called fine structure of the photosphere field), but also
by the act of measuring. When recording solar (and stellar) magnetic
fields and modeling atmospheric processes, quantum effects have to be
taken into account, such as nonlocality, indistinguishability, and the
entanglement of photons, as well as that a photon only acquires its
properties at the exact moment of its detection. The best approximation
to reality can be achieved by averaging the MMF measurements carried
out with different magnetographs and in different spectral lines.
Title: Comments on ultrafast neutrinos (December 2011)
Authors: Kotov, V. A.; Sanchez, F. M.
Bibcode: 2012BCrAO.108..115K
Altcode:
The striking news released in the fall of 2011 about the detection
of a neutrino travelling faster than light has stunned physicists
and cosmologists. We explain the phenomenon based on a holographic
stationary model of the Universe that implies the existence of
supraluminal speeds and Grand Cosmos external to the Hubble sphere.
Title: The sun and exoplanets: The solitude of man
Authors: Kotov, V. A.
Bibcode: 2012BCrAO.108...30K
Altcode:
Solar pulsations with a period of P 0 = 9600.606(12)
were discovered in 1974. A more recent discovery is that planetary
distances in the solar system are subject to spatial resonance with
the parameter L 0 ≡ cP 0 ≈ 9600 ls and that
the P 0 pulsation itself has cosmological significance
(coherent cosmic oscillation, or the pace of absolute time of the
universe; c is the speed of light). As of June 2011, 552 extrasolar
planets have been discovered. Statistical analysis shows that the
distribution of the semimajor axes of alien planets does not have
L 0 resonance. Moreover, it appears to have no resonance
at all. This frustrates the 20th-century hopes for the existence of
extraterrestrial civilizations and possible contact with them. They are
simply not there. This explanation of the Fermi paradox, or the Great
Silence, appears to rest on the triumph of the anthropic principle,
which has been successfully implemented by nature within our planetary
system. This leads to a vision whereby the cosmos seems to be created
specially for us. The scale L 0 indicates that the sun is
a special quantum object, where L 0 is a wave function
parameter that is not subject to the rational principles of the
classical world, but rather follows a peculiar, quantum logic.
Title: On possible cosmic origin of the 11-year solar cycle
Authors: Kotov, V. A.; Sanchez, F. M.; Bizouard, K.
Bibcode: 2012BCrAO.108...36K
Altcode:
In order to test Dicke's idea of a clock hidden inside the Sun and
determine the initial phase of the solar cycle, the epochs of the
extrema of the Wolf numbers observed over the past 400 years are
examined. It is shown that extrema that obey the period P W
equaled 11.07(4) years retain the initial phase, which cannot be
explained in terms of local physics and concepts of the past century
regarding the mechanism of the solar cycle based on the theory of a
magnetic dynamo and the phenomenological model of the Babcock-Leighton
cycle. It is suggested that the cycle has a cosmic (cosmological)
origin. This is clearly indicated by the correlation of the cycle
period with a holographic time-scale of the Universe, ( a 0
R 3)1/4/ c ≈ 11.0(4) years, where a 0
and R are the radii of the first Bohr orbit of a hydrogen atom and the
observable Universe, respectively, and c is the speed of light. It is
noted that there are other strict holographic relations that include
a 0, R, P W , the wavelength of the microwave
background radiation (with a temperature of 2.7 K), and a period of the
global solar pulsations equal to 9600.6 s. The true physical nature
of the governing mechanism for the 11-year cycle can perhaps only
be understood based on modern concepts about the nonlocality of our
world, which follows from Bell's theorem, which is grounded on the
achievements of quantum mechanics at the turn of the 20th and 21st
centuries, as well as using a model of a holographic Universe free of c.
Title: Commentary on the OPERA Superluminal Neutrinos
Authors: Sancheza, Francis M.; Kotov, Valery A.
Bibcode: 2012JCos...18.8081S
Altcode:
No abstract at ADS
Title: Towards a synthesis of two cosmologies: the steady-state
flickering Universe
Authors: Sanchez, Francis M.; Kotov, Valery A.; Bizouard, Christian
Bibcode: 2011JCos...17.7225S
Altcode:
A gravitation/electricity symmetry gives directly the Hubble radius
(within its 4% indetermination), while a "black atom" model confirms
the time-invariance of the radius of a critical steady-state
Universe. This refutes the Primordial Big Bang model and permits
to apply the holographic principle to the invariant Hubble sphere,
with the extension to a holophysics principle, introducing a tachyonic
scanning in a critical steady-state flickering Universe. This suggests a
transient validity of the Big Bang approach, announcing a reconciliation
of the two main cosmologies. Several main fine-tuning relations are
shown to be of a holophysical character, i.e. a topological conservation
involving the main physical lengths. The elimination of light speed
from the interaction formulae defines both a timescale 13.7 Gyr
(within 1% of the so-called age of the Universe, which is interpreted
rather as the temporal regeneration constant of the steady-state model)
and, within 10-4 uncertainty of 𝐺, the coherent cosmic oscillation
period 9600.61(3) s. The latter is shown to be intrinsically connected
by holophysics with the redshift periodicity 71.7 km/s and the Wolf
solar period 11.05 years. The flickering concept opens the door for
a cosmic interpretation of particle physics; for instance, the parity
violation would be tied to a scanning chirality.
Title: Cosmic vibration of the sun and quasar 3C 273
Authors: Kotov, V. A.
Bibcode: 2011BCrAO.107...70K
Altcode:
The hypothesis that some extragalactic objects pulsate with a period
of P 0 = 9600.606(12) s, which was first discovered in the
Sun, is tested with data on quasar 3C 273. Observations of its rapid
photometric variability were made by different observers in 1968-2005
within several spectral bands. At the 4σ confidence level, these data
show that there is a period of 9600.624(18) s, which is consistent,
within the error limits, with P 0 (mean harmonic amplitude
0.006 B magnitude). Its independence from the redshift z is a sign
of a cosmological origin of the P 0 pulsation, which is
sometimes understood as the "rhythm" of cosmos' absolute time. This
phenomenon is also shown to be deeply connected—via the Sanchez
formula—to the fundamental constants of physics and cosmology. This
refutes the standard Big Bang hypothesis and confirms the Steady State,
c-free model of the Universe ( c is the speed of light).
Title: Pulsations of the sun and a beat period of 399 days
Authors: Kotov, V. A.; Khaneichuk, V. I.
Bibcode: 2011BCrAO.107...67K
Altcode:
Measurements of the Doppler effect of the solar photosphere have
been carried out at the Crimean Astrophysical Observatory for 37
years, beginning in 1974 (in total, 2188 days or 13 247 h). The
measurements use the differential center-to-limb method of registration
of line-of-sight velocity with a solar magnetograph (in the iron
absorption line λ512.4 nm). As a result of the experiment, two global
pulsations of the sun with periods P 0 = 9600.606(12) and
P 1 = 9597.936(16) s have been discovered. The nature of
the periods is unknown. The first pulsation was detected in 1974-1982;
the second, during nearly all the 37 years. The 2008-2010 data confirm
the stability of the initial phase of the P 1 pulsation
with a mean (differential) amplitude of 0.25 m/s. The fact that the
beat period of the two pulsations coincides with the synodic period
of Jupiter's orbital revolution, i.e., 399 days, raises a new, complex
problem for solar physics and cosmogony.
Title: Minimum of 2008 or the ``quantum'' Sun-2
Authors: Kotov, V. A.
Bibcode: 2010BCrAO.106..137K
Altcode:
The prolonged 2007-2009 minimum is a big surprise for solar physics. In
order to reveal the causes, we analyze the variability of the general
magnetic field (GMF) of the Sun as a star measured by CrAO and five
other observatories since 1968 (more than 19000 daily field strengths
B were obtained in 41 years). Sharp yearly mean extrema of the negative
(S) field took place in 1969, 1990, and 2008, with the third extremum,
in contrast to the two previous ones, having coincided with the sunspot
minimum. This explains both the long duration of the minimum and the
record (over the last 100 years) increase in the length of the Wolf
cycle (no. 23) to 12 or more years. The S-field extrema followed with
a period of 19.5 ± 1.1 yr—some mean between the 22.1 ± 0.3-yr
sunspot cycle, the 18.6-yr saros, and the 19.9-yr Jupiter-Saturn
conjunction period. It is pointed out that, for some unclear reason,
the negative polarity dominated on the Sun in 1968-2008: the overall
mean B = -0.021 ± 0.015 G. The existence of a second Sun that obeys
the laws of quantum mechanics is hypothesized. The “quantum” model
of the Sun-2 explains many properties of the “classical” Sun-1,
including the coronal heating, cyclic activity, periodic variations
in GMF, and its sector structure.
Title: An absolute clock of the cosmos?
Authors: Kotov, V. A.; Lyuty, V. M.
Bibcode: 2010BCrAO.106..127K
Altcode:
In 1968-2005 different observers (mainly, one of the
authors—V.M. Lyuty) performed numerous measurements of luminosity
of the nucleus of the Seyfert galaxy NGC 4151. It is shown that (
a) luminosity of the object pulsated over 38 years with a period of
160.0106(7) min coinciding, within the error limits, with the well-known
period P 0 = 160.0101(2) min of the enigmatic “solar”
pulsations, and ( b) when registering oscillations of luminosity
of NGC 4151 nucleus with the P 0 period, time moments of
observations must be reduced to the earth instead of the sun, i.e.,
to the reference frame of the observer. The coherent P 0
oscillation is characterized, therefore, by invariability of both
frequency and phase with respect to redshift z and the earth’s orbital
motion, respectively. From these results it, thus, follows that the
coherent P 0 oscillation seems to be of a true cosmological
origin. The P 0 period itself might represent a course of
the “cosmic clock” related to the existence of an absolute time
of the Universe in Newton’s comprehension.
Title: Forty years of measurements of the mean magnetic field of
the Sun: View from today
Authors: Kotov, V. A.
Bibcode: 2009BCrAO.105...45K
Altcode:
No abstract at ADS
Title: Solar system, exoplanets, and anthropic principle
Authors: Kotov, V. A.
Bibcode: 2009BCrAO.105..119K
Altcode:
No abstract at ADS
Title: The Sun and the transcendental world of binaries
Authors: Kotov, V. A.
Bibcode: 2008BCrAO.104..125K
Altcode:
The theory of gravity says that a binary with orbital frequency ν
should be a source of gravitational waves at the double frequency and
higher harmonics. This implies that long-term exposure of an ensemble
of binaries to gravity waves with frequency νG can result in
(a) a lack of binaries with frequencies near frequency νG/2
and its higher harmonics (the effect of unstable orbits) and/or (b)
an excess of binaries whose orbital frequencies are "absolutely"
incommensurable with νG/2 and its higher harmonics
(the effect of stable orbits). It is assumed that the stable-orbit
frequencies are almost equal to multiples of πνG/2
and νG/2π, where π plays the role of a "perfect"
factor ensuring the best antiresonance of binaries. The statistical
analysis of frequencies of 5774 Galactic close binary systems (CBSs)
with periods P less than 10 days is based on calculating the resonance
spectrum that indicates the best common multiple for a given set of
frequencies with allowance for the factor π. The CBS distribution
turns out to be modulated by the frequency νG = 104.4(5)
μHz, and this effect is the most pronounced for superfast and compact
rotators, such as cataclysmic variables (CVs) and related objects. The
frequency νG is, within the error, equal to the "enigmatic"
frequency ν0 = 104.160(1) μHz com discovered earlier in the
power spectra of the Sun and brightness variations of some extragalactic
sources. This confirms the existence of a "coherent cosmic oscillation"
of the Universe with frequency ν0(νG). The
new astrophysical phenomenon naturally explains an "CV period gap"
at frequencies ≈πνG/3 (P ≈ 153 min) and maxima at the
neighboring frequencies ≈πνG/2 and ≈πνG/4
(P ≈ 102 and ≈204 min, respectively). The remarkable and
"mysterious" role of the transcendental number π for the world of
binaries is emphasized, and the mystery of physical nature of the
"universal" oscillation ν0(νG) is highlighted.
Title: A paradox in measuring the magnetic field of the Sun
Authors: Kotov, V. A.
Bibcode: 2008BCrAO.104...79K
Altcode:
Significant discrepancies are often observed among the values of the
mean magnetic field (MMF) of the Sun as a star observed by various
instruments using various spectral lines. This is conventionally
attributed to the measurement errors and "saturation" of a solar
magnetograph in fine-structure photospheric elements with a strong
magnetic field. Measurements of the longitudinal MMF performed in
1968-2006 at six observatories are compared in this paper. It is
shown that the degree of discrepancy (slopes b of linear regression
lines) varies significantly over the phase of the 11-year cycle. This
gives rise to a paradox: the magnetograph calibration is affected
by the state of the Sun itself. The proposed explanation is based
on quantum properties of light, namely, nonlocality and "coupling"
of photons whose polarization at the telescope-spectrograph output
is determined by spacious parts of the solar disk. In this case,
the degree of coupling, or "identity," of photons depends on the field
distribution in the photosphere and the instrument design (as Bohr said,
"the instrument inevitably affects the result"). The "puzzling" values
of slope b are readily explained by the dependence of the coupling
on the solar-cycle phase. The very statistical nature of light makes
discrepancies unavoidable and requires the simple averaging of data
to obtain the best approximation of the actual MMF. A 39-year time
series of the MMF absolute value is presented, which is indicative of
significant variations in the magnitude of the solar magnetic field
with a cycle period of 10.5(7) yr.
Title: Oscillations of the Sun: Results of observations in 1974 2007
Authors: Kotov, V. A.; Haneychuk, V. I.
Bibcode: 2008BCrAO.104...45K
Altcode:
Doppler measurements of the photosphere of the entire Sun carried out
at the Crimean Astrophysical Observatory (CrAO) in 1974-2007 by the
differential technique showed the presence of an enigmatic periodicity
of P1 = 159.967(4) min. The phase of this oscillation
was constant over the entire 34-year of surveys and interval. The
true nature of this phenomenon is unknown. Pulsation with the former
period P0 = 160.0101(15) min has been reliably detected
only in the first nine years, from 1974 to 1982. It is noted that (a)
the average amplitude of the P1 oscillation in the first
half of the data was nearly 34% higher than in the second half and (b)
the beat period of 400(14) d of these two pulsations is equal within
error to the Jovian synodic period (399 d). A hypothesis is discussed
relating the P1 oscillation to the superfast rotation of
the inner solar core.
Title: Mean absolute strength of the solar magnetic field in 1968 2006
Authors: Kotov, V. A.
Bibcode: 2008ARep...52..419K
Altcode: 2008AZh....85..471K
Measurements of the mean magnetic field of the Sun as a star (the
line-of-sight component of the magnetic field of the visible hemisphere
for a given day) carried out at six observatories are used to compile
a catalog of the mean magnetic field for 1968 2006 (containing about
18 000 daily values). The cataloged data are compared with direct
daily measurements of the absolute line-of-sight field made at the
Kitt Peak Observatory in 2003 2006 (original data with a resolution
of 1″ averaged over the solar disk). The true absolute mean field
strength averaged over the visible solar hemisphere is determined for
1968 2006 to be B 0 = 7.7 ± 0.2 G. This figure exceeds
previous estimates by almost a factor of four. B 0 exhibits
no appreciable slow trend over the entire 39-year interval, but varies
substantially with the cycle. The period of this variation is 10.5
± 0.7 yr, and its harmonic amplitude is 1.7 G. The magnetic flux of
spots and active regions makes B 0 almost twice the field
strength in the “normal” photosphere at the solar minimum, i.e.,
for the “quiet” Sun.
Title: The sun, the cosmic vibration, and the nucleus of the
galaxy 4151
Authors: Kotov, V. A.; Lyuty, L. M.
Bibcode: 2007BCrAO.103...69K
Altcode:
Numerous U and V magnitude measurements were performed for the nucleus
of the Seyfert galaxy NGC 4151 at the Crimean Laboratory of the SAI
(Moscow University) in 1994-2005. Adding them to the previous data for
1968-1997 has led to a substantial increase in the confidence level of
the light variations in NGC 4151 with a stable period of PG
= 160.0108(7) min and a mean amplitude of 0.007 U mag (in the "active"
state of the nucleus). The period of NGC 4151 agrees well with the
period of 160.0101(15) min found previously in the oscillations of the
Sun. It is treated as the period of a "coherent cosmic oscillation"
independent of redshift z or as the period of "free cosmic vibrations"
of the hydrogen atom, the main element of the Universe. The period and
initial phase of the PG oscillation have been constant for
38 years of NGC 4151 observations. The new astrophysical phenomenon
appears to be closely related to the quantum nonlocality of photons
and is of particular interest in physics and cosmology.
Title: There are ten, not eight planets
Authors: Kotov, V. A.
Bibcode: 2007BCrAO.103...75K
Altcode:
In 1946, E. Sevin postulated the global vibrations of the Sun with
a period P0 = 1/9 day and a "wavelength" L0
= c × P0 = 19.24 AU and predicted the tenth planet at
a mean distance of 4.0 × L0 ≈ 77.0 AU from the Sun (c
is the speed of light). The global vibrations of the Sun, precisely
with the period of 1/9 day, were actually detected in 1974. Recently,
the largest Kuiper Bell object 2003 UB313, or Eris, with
an orbital semimajor axis ≈ 3.5 × L0 ≈ 67.5 AU was
discovered. We adduce arguments for the status of Eris as our tenth
planet: (i) the object is larger and farther from the Sun than Pluto
and (ii) the semimajor axis of Eris agrees well with the sequence of
planetary distances that follows from the resonance spectrum of the
Solar system dimensions (with the scale L0 and for all 11
orbits, including those of Pluto, Eris, and the asteroid belt). We point
to a mistake of the Prague (2006) IAU Assembly, which excluded Pluto
from the family of planets by introducing a new, highly controversial
class of objects—"dwarf planets."
Title: On the Near-One-Year Variation of the Sun's Mean Magnetic Field
Authors: Kotov, V. A.
Bibcode: 2006SoPh..239..461K
Altcode: 2006SoPh..tmp...70K
The mean magnetic field (MMF) of the Sun-as-a-star was measured over the
last 38 years by six observatories (about 17 000 MMF daily records, 1968
- 2005). The MMF power spectrum reveals the presence of an enigmatic
1.029(7) year periodicity whose origin requires explanation. We show
that this quasi-annual variation is not produced by modulation of the
MMF signal due to the annual change of the Earth's helio-latitude
(one-year change of visibility of the Sun's polar regions) as
commonly accepted. The nature of this new solar phenomenon is open
for discussion.
Title: Pulsations of the sun: 30 years of measurements
Authors: Kotov, V. A.; Haneychuk, V. I.; Tsap, T. T.
Bibcode: 2004KFNT...20..408K
Altcode:
Regular measurements of oscillations of the Sun-as-a-star's photosphere
have been performed at the Crimean Astrophysical Observatory since
1974. In this experiment, a Babcock solar magnetograph detects Doppler
effect difference between the central part and the limb part of the
solar disk (using the Fraunhofer absorption line Fe I λ 512.4 nm). Over
last 30 years the measurements were made during 1807 days (in aggregate
more than 11 thousand hours). The most significant peak of the power
spectrum of the line-of-sight velocity variations corresponds to the
period P = 159.9655±0.0005 min. The period is in good agreement,
within the error limit, with the Stanford value 159.9663±0.0008
min, inferred before from the independent 1977-1994 measurements,
which supports strongly solar origin of the period. This oscillation
has nearly constant initial phase over the total 30-year interval and
reveals substantially non-harmonic mean profiles of both, velocity and
radius, perturbations. The true physical nature of the P phenomenon
and the source of its excitation are unknown. It is supposed that the
periodic oscillation of the Sun's photosphere is caused by superfast
rotation of the central solar core.
Title: On rotation of Uranus and Neptune
Authors: Kotov, V. A.
Bibcode: 2004KFNT...20..142K
Altcode:
The "resonance-spectra" of the revolution frequencies of massive
satellites are computed in order to determine the rotation periods of
gravitating masses of the giant planets. Based upon the tidal theory,
it is supposed that the best common multiple of the satellite sidereal
frequencies should be close to the rotation frequency of the central
planet. A new "dynamical" period of Uranus, 16.14± 0.20 h (95% C.L.),
coincides well, within the error limits, with the period 16.16± 0.33
h determined earlier by spectroscopic technique. The most probable
Neptune's period, 13.43± 0.16 h (99%), agrees with its dynamical
oblateness. It is shown that the frequencies of all six fast-rotating
planets and major asteroids occur to be in near-resonance with the
frequency ν0 = 103±2 μHz. The nature of the mysterious
ν0 -resonance in the solar system is unknown.
Title: Solar pulsation 1974-2003: the evidence for a fast rotating
core
Authors: Kotov, V. A.
Bibcode: 2004IAUS..223..115K
Altcode: 2005IAUS..223..115K
The measurements of the Doppler effect of the photosphere showed
the presence of the persistent periodicity 159.9655(5) min. It is
interpreted as by-product of the fast-rotating central solar core.
Title: On stability of rotation of the mean magnetic field of the Sun
Authors: Haneychuk, V. I.; Kotov, V. A.; Tsap, T. T.
Bibcode: 2003A&A...403.1115H
Altcode:
New data on the mean magnetic field of the Sun (MMFS) as a star measured
at the Crimean Astrophysical Observatory in 1998-2001 are presented. The
34-year time series of the MMFS using similar data from three other
observatories (1968-2001, with the total number of daily MMFS values N =
12 428), is considered. It is found that (a) the primary synodic period
of the equatorial rotation of solar magnetic field, Psun =
26.929 +/- 0.015 days, did not vary over the last 34 years, but (b)
the average intensity H0 of the photospheric large-scale
fields, by modulus, decreased by about 4.5% (with a confidence level
of about 80%). The conclusion is made that the longer, 90-year,
cycle might be responsible for this potential gradual decrease of
H0. The average curve of MMFS variation as plotted with
the primary rotational period Psun demonstrates an obvious
N-S asymmetry of polarities, perhaps associated with the quadrupole
component and ``magnetic disequilibrium'' of the Sun as a whole.
Title: Daily measurements of the mean magnetic field of the Sun,
1968-2001: Anomalous distribution?
Authors: Kotov, V. A.
Bibcode: 2003A&A...402.1145K
Altcode:
The mean magnetic field (MMF) of the Sun was measured in 1968-2001 by
four Babcock magnetographs: of the Crimean Astrophysical Observatory,
CrAO, of the Mount Wilson Observatory, MWO, of the Wilcox Solar
Observatory, WSO, and of the Sayan Solar Observatory, SSO (in all
nearly 13 thousand daily records). The MMF strengths recorded by these
instruments on the same day, often deviate substantially from each
other; this can hardly be explained by purely instrumental/solar causes
alone. It is pointed out that (a) each magnetograph represents a linear
electro-optical device detecting diminutive, { ~ } 10-5
- 10-4, Zeeman circular polarization of a solar spectral
line, with (b) no essential nonliner effects are expected, and (c)
the observed MMF daily values must be normally distributed around
a zero mean. The actual MMF distribution appears to be quite normal
for records of the CrAO and SSO. Those of the MWO and WSO, however,
deviate remarkably from the normal. The exact physical nature of this
abnormity is unknown. It is suggested that the true cause might be
connected with (a) the use of an image-slicer (at MWO and WSO), (b)
entanglement of photons, (c) the statistical origin of light itself
(due to the principle of uncertainty: ``the instrument inevitably
influences the output''), and (d) some instrumental/solar causes of
poorly known origin and action.
Title: Towards Calibration of the Mean Magnetic Field of the sun
Authors: Kotov, V. A.; Kotov, S. V.; Setyaev, V. V.
Bibcode: 2002SoPh..209..233K
Altcode:
The 1968-2000 data on the mean magnetic field (MMF, longitudinal
component) of the Sun are analysed to study long-time trends of
the Sun's magnetic field and to check MMF calibration. It is found
that, within the error limits, the mean intensity of photospheric
magnetic field (the MMF strength, |H|), did not change over the
last 33 years. It clearly shows, however, the presence of an 11-year
periodicity caused by the solar activity cycle. Time variations of |H|
correlate well with those of the radial component, |Br|,
of the interplanetary magnetic field (IMF). This correlation (r=0.69)
appears to be significantly higher than that between |Br|
and the results of a potential source-surface extrapolation, to the
Earth's orbit, of synoptic magnetic charts of the photosphere (using
the so-called `saturation' factor δ−1 for magnetograph
measurements performed in the line Fe i λ525.0 nm; Wang and Sheeley,
1995). It seems therefore that the true source surface of IMF is the
`quiet' photosphere - background fields and coronal holes, like those
for MMF. The average `effective' magnetic strength of the photospheric
field is determined to be about 1.9 G. It is also shown that there
is an approximate linear relation between |Br| and MMF
intensity |H| (in gauss)
Title: On the measurements of the magnetic disbalance of the Sun
Authors: Kotov, V. A.; Haneychuk, V. I.; Tsap, T. T.
Bibcode: 2002KFNT...18..205K
Altcode:
The 1968-2000 time sequence of the mean magnetic field of the Sun as a
star is analysed (MMF, more than 12 thousands of daily measurements). It
is shown that nominally -- on the basis of the total MMF measurements
set -- the southern polarity of the magnetic field predominates on the
Sun, with the average value -1.9± 1.1 μ T (the magnetic asymmetry
is significant at about 91%; however, its instrumental origin cannot
be completely excluded). The MMF changes with the 22-year cycle, so
that its predominant polarity tends to coincide with that of the Sun's
northern pole; the mean amplitude of this variation is equal to 6 μ
T. It is concluded that the northern pole polarity tends to "determine"
the dominant polarity of solar background fields for the most area of
the photosphere (at heliolatitudes higher than -500).
Title: Sources of the Global Magnetic Field of the Sun
Authors: Kotov, V. A.; Setyaeva, I. V.
Bibcode: 2002ARep...46..246K
Altcode:
Data on the global magnetic field (GMF) of the Sun as a star for
1968 1999 are used to determine the correlation of the GMF with the
radial component of the interplanetary magnetic field (IMF) |B r|;
all data were averaged over a half year. The time variations in the
GMF |H| are better correlated with variations in |B r|; than the
results of extrapolating the field from the “source surface” to
the Earth’s orbit in a potential model based on magnetic synoptic
maps of the photosphere. Possible origins for the higher correlation
between the GMF and IMF are discussed. For both the GMF and IMF, the
source surface actually corresponds to the quiet photosphere—i.e.,
background fields and coronal holes—rather than to a spherical surface
artificially placed ≈2.5 R ⊙ from the center of the Sun, as assumed
in potential models (R ⊙ is the solar radius). The mean effective
strength of the photospheric field is about 1.9 G. There is a nearly
linear dependence between |H| and |B r|. The strong correlation between
variations in |H| and |B r| casts doubt on the validity of correcting
solar magnetic fields using the so-called “saturation” factor δ-1
(for magnetograph measurements in the λ 525.0 nm FeI line).
Title: The active core of Seyfert galaxy NGC 4151 and the true origin
of the 160-minute oscillation.
Authors: Kotov, V. A.; Khaneichuk, V. I.; Merkulova, N. I.; Metik,
L. P.; Lyutyi, V. M.
Bibcode: 2002BCrAO..98...32K
Altcode:
No abstract at ADS
Title: Anomalous magnetic field of the sun at the beginning of
cycle 23
Authors: Kotova, I. V.; Kotov, S. V.; Kotov, V. A.
Bibcode: 2001A&AT...20..505K
Altcode:
Measurements of the mean magnetic field (MMF) of the Sun from
1968-1999 showed that (1) the Sun's magnetic field has a predominance
of S-polarity, (2) it changes with periods 1.04, 1.60 and 23 yr, (3)
the yearly-mean index of MMF energy reached the peak value in 1991,
and after that (4) a significant decrease of MMF was observed. It is
supposed that (a) the magnetic asymmetry of the Sun is a fundamental
property of solar magnetism, (b) there are near-resonances between
the MMF and orbital motions of Mercury, Venus and Earth which arose
at early stages of formation of the Solar system, and (c) cycle 23
will display an anomalously low magnetic and sunspot activity.
Title: On the Sun's magnetic field prior to maximum of the cycle 23
Authors: Kotov, V. A.; Haneychuk, V. I.; Tsap, T. T.
Bibcode: 2001IzKry..97...60K
Altcode:
The large number of measurements of the mean magnetic field (MMF) of
the Sun were made in the CrAO in 1999. These data are analysed together
with the like measurements performed at four solar observatories in
1968 - 1999. It is shown that (1) during total 32-year interval the
predominance of longitudinal magnetic field of southern polarity was
observed on the Sun with the mean value of -0.009±0.005 Gs, (2) in
1999, MMF exhibited 4-sector structure which is more characteristic
of epochs near minima of solar activity, (3) the standard deviation
of MMF in 1999 equals to 0.48 Gs was significantly lower than that
usually observed before solar activity maximum (≍0.82 Gs).
Title: On rotation of Jupiter and Saturn
Authors: Kotova, I. V.; Kotov, V. A.
Bibcode: 2001KFNT...17..157K
Altcode:
The method based on analysis of mean motion of massive satellites is
proposed to deduce rotation periods of giant planets. A computation of
the so-called "resonance-spectrum" is applied for analysis of satellite
frequencies. It is found that the Saturn's "dynamical" period is equal
to 10.76± 0.15(h) . It agrees fairly well with the value 10.66(h)
determined earlier by the Voyager-1 spacecraft (reflecting rotation of
magnetic field of the planet), and thus gives a good check-up of the
method. But the new period of Jupiter, 10.69±0.15(h) , significantly
differs from the commonly accepted value ≈ 9.9(h) , determined also
by the magnetic field rotation, or from radio-observations. It is
concluded that periods of giant planets determined by variations of
magnetic field, can not necessarily reflect rotation rate of the main
gravitating body of a planet. The cause might be differential rotation
of magnetosphere and magnetic field of a planet - the phenomenon
analogous to differential rotation of magnetic field of the Sun.
Title: Does the Solar Magnetic Field Increase?
Authors: Kotov, V. A.; Kotova, I. V.
Bibcode: 2001AstL...27..260K
Altcode:
We consider measurements of the general magnetic field (GMF) of the Sun
as a star at four world observatories from 1968 until 1999. We show
that, within the error limits, the mean strength of the photospheric
magnetic field H (of its longitudinal component, in magnitude) has
not changed over the last 32 years. This is in conflict with the
recent conclusion by Lockwood et al. (1999) that the solar coronal
magnetic field increased by 40% from 1964 until 1996 and has almost
doubled in the last 100 years. The causes of discrepancies in the
results are discussed. At the same time, the GMF exhibits a natural
11-year variation associated with the solar cycle. The strength of the
photospheric longitudinal magnetic field (in absolute value) averaged
over 32 years is 0.46 G (at an rms GMF strength of 0.57 G). The mean
GMF for all years of measurements had a south polarity: <H>
= - 0.030 +/- 0.018 G. The difference from zero is statistically
significant at 1.7 sigma (90%) and may be directly related to the
outstanding problem of the solar magnetic "monopole".
Title: Two states of the nucleus of the NGC 4151 Galaxy quiet
and active
Authors: Kotov, V. A.; Lyuty, V. M.; Metlov, V. G.; Haneychuk, V. I.
Bibcode: 2000KFNT...16..558K
Altcode:
The most interesting phenomenon in the studies of active galactic
nuclei is their rapid variability over one night whose origin remains
mysterious, and of special interest is the search for the presence of
a periodic component. The oscillation with the period P0
≈ 160.010 min was found earlier in the emission of the nucleus of
the Seyfert galaxy NGC 4151, but its authenticity is often doubted. The
reasons for the scepticism are a small amplitude of the signal and the
fact that the oscillation is absent during some nights. In 1985-1996 the
observers of the P. K. Sternberg State Astronomical Institute and the
Crimean Astrophysical Observatory carried out long series of photometric
observations of NGC 4151 (in all, 39 and 51 nights in the U and V bands,
respectively). Less than a half of the nights a significant variability
over a night which exceeded 0.03-mag threshold (it was treated with no
relation to any a priori periodicity). But the most important is that
the P0-oscillation was clearly seen exactly during those
"active" nights; other, "quiet", nights did not reveal any noticeable
periodic signal. The mean harmonic amplitude of the P0
-oscillation during the active state of the NGC 4151 nucleus is found
to be about 0.009m (U-band), while it is not larger than
0.0008m in the same band during the quiet state. The nature
of such a strange modulation is unknown. The arguments are given in
favour of a cosmological origin of the P0-oscillation.
Title: Solar oscillations in 1999
Authors: Kotov, V. A.; Haneychuk, V. I.; Tsap, T. T.
Bibcode: 2000BCrAO..96..166K
Altcode:
No abstract at ADS
Title: Oscillations of the sun with a period of 159.966 minutes in
the Crimean 25-year observations
Authors: Kotov, V. A.; Khaneychuk, V. I.; Tsap, T. T.
Bibcode: 2000KFNT...16...49K
Altcode:
Measurements of low-degree oscillations of the Sun were carried out
at the Crimean Astrophysical Observatory during 25 years (1974-1998;
in all 1530 days, about 9733 hours). These data showed that within
the frequency range near the 9th daily harmonic the most significant
oscillation corresponds to the period P1 = 159.9660±
0.0010 min. It agrees well with the main periodicity PSt =
159.9663±0.0014 min found earlier in the similar Doppler measurements
of the solar photosphere performed at the Stanford University in
1977-1994. The initial phase of the P1 oscillation is
found to be remarkably stable over the entire 25-year interval. This
phenomenon cannot be ascribed to some terrestrial cause or to an
artifact of the data reduction procedure. It presents a challenging
problem for the physics of the Sun and models of its interior structure.
Title: New measurements of the mean magnetic field of the Sun and
its rotation
Authors: Kotov, V. A.; Haneychuk, V. I.; Tsap, T. T.
Bibcode: 1999ARep...43..185K
Altcode:
A list of 152 new measurements of the mean magnetic field (MMF) of
the Sun as a star obtained at the Crimean Astrophysical Observatory
(CAO) in 1991-1997 are presented. They increase the total number of
CAO MMF measurements to N = 1549 (since 1968). This time series is
studied together with similar data from the Mount Wilson Observatory
(1970-1982, N = 2457). A (synodic) period P_R = 26.95 +/- 0.06 days
dominates in the power spectrum of the merged data for 1968-1997,
revealing remarkable phase coherence over 30 years. This stability of
the rotation of the "magnetic" Sun independent of the 11-year cycle
is difficult to explain in the framework of current theories for the
generation of the global solar magnetic field that gives rise to the
solar cycle. There are two other periods in the solar MMF (~161 days
and 1.0 year), whose origin is not yet clear.
Title: Is the 160-minute mode of oscillation of the sun returning?
Authors: Kotov, V. A.; Khaneichuk, V. I.; Tsap, T. T.
Bibcode: 1999BCrAO..95....1K
Altcode:
No abstract at ADS
Title: The mean magnetic field of the Sun and the Sun-Mercury
resonance.
Authors: Kotov, V. A.; Tsap, T. T.
Bibcode: 1999KPCB...15..313K
Altcode:
More than 11000 measurements of the mean magnetic field of the Sun as
a star (MMFS) were made at four observatories: Crimea, Mount Wilson,
Sayan, and Stanford. The main period of rotation of the solar magnetic
field (26.92±0.03d) which dominates these data reveals
a surprising phase stability. Such stability is incompatible with
the current phenomenological model of the solar cycle, which assumes
a polarity reversal in the dipole field every 11 years. The authors
ascribe this strict 27-day MMFS periodicity to the toroidal magnetic
field of the Sun which is concentrated under the convection zone. Of
particular interest also is the 7:2 resonance between the MMFS rotation
and the orbital motion of Mercury; this resonance might have arisen
in the distant past when the protoplanetary nebula existed.
Title: Observations of low-degree solar global oscillations at the
Crimean Astrophysical Observatory.
Authors: Tsap, T. T.; Haneychuk, V. I.; Kotov, V. A.
Bibcode: 1998KFNT...14..520T
Altcode: 1998KNFT...14..520T
Observations of low-degree p-modes obtained at the Crimean Astrophysical
Observatory are presented. The observed frequencies are found to
agree satisfactorily with the calculated frequencies of the standard
solar model.
Title: Magnetic Field of the Sun as a Star: The Mount Wilson
Observatory Catalog 1970-1982
Authors: Kotov, V. A.; Scherrer, P. H.; Howard, R. F.; Haneychuk, V. I.
Bibcode: 1998ApJS..116..103K
Altcode:
Measurements of the mean magnetic field of the Sun (MMFS) seen as
a star were regularly conducted at the Mount Wilson Observatory
from 1970 October through 1982 December. A listing is presented of
all these data (2457 daily values) suitable for comparison with
similar data of other observatories and for studies of magnetic
variability and rotation of the Sun. The scatter-plot diagrams and
power spectra of the Mount Wilson data and also of the total data
1968-1991 (collected from three observatories: Crimean Astrophysical
Observatory, Mount Wilson Observatory, and Wilcox Solar Observatory)
are also presented. Time variations of the MMFS connected with solar
rotation at periods ~27-28 days and also an enigmatic 1 yr variation
are briefly discussed. The power spectrum of the 24 yr data set
shows that the most significant and phase-coherent synodic periods of
the MMFS variations are 26.92 +/- 0.02 and 27.13 +/- 0.02 days (both
are thought to be associated with rotation of the large-scale surface
magnetic field near equator of the Sun) and 28.13 +/- 0.02 days. It
is suggested that the latter period reflects ``rigid'' rotation of
the global magnetic field concentrated under the bottom of the solar
convection zone. The arguments are given in favor of reality and high
confidence level of major periodicities exhibited by MMFS variations.
Title: Five Thousand Galactic Binaries as a Detector of Gravitational
Waves
Authors: Kotov, V. A.; Kotov, S. V.
Bibcode: 1998A&AT...15..185K
Altcode:
No abstract at ADS
Title: A common resonance of delta SCT stars and ellipsoidal binaries.
Authors: Kotov, S. V.; Kotov, V. A.
Bibcode: 1998KFNT...14..543K
Altcode: 1998KFNT...14f.543K
No abstract at ADS
Title: New data on the P0-oscillation of the nucleus of
the Seyfert galaxy NGC 4151.
Authors: Kotov, V. A.; Lyutyj, V. M.; Merkulova, N. I.; Metik, L. P.;
Metlov, V. G.; Khanejchuk, V. I.
Bibcode: 1998KFNT...14...67K
Altcode: 1998KNFT...14...67K; 1998KFNT...14a..67K
The presence of the periodicity P0 = 160.0101±0.0001
min in the brightness variations of active galactic nuclei is often
subjected to criticism by some astrophysicists. With the aim to
check the P0-effect, an extensive series of photometric
observations of the Seyfert galaxy NGC 4151 was obtained in 1987 -
1994 using two Crimean reflectors. These new data confirmed the
presence of the P0-periodicity with the stable (over 26
yr) initial phase and the mean harmonic amplitude ≍7 mmag (in the
V filter). This conclusion is supported by analysis of the X-ray data
(1975 - 1991) obtained by satellites Ariel-5, EXOSAT and Ginga. Since
just the same period has been detected earlier in the power spectrum
of global oscillations of the Sun, the conclusion is drawn about its
cosmological origin.
Title: 160-minute oscillations of active galactic nuclei: new data
for 3C 273 and NGC 4151
Authors: Kotov, V. A.; Merkulova, N. I.; Metik, L. P.; Khaneichuk,
V. I.; Lyutyi, V. M.
Bibcode: 1998BCrAO..94...83K
Altcode:
No abstract at ADS
Title: 25 years of investigating the magnetic field of the sun as
a star
Authors: Kotov, V. A.; Khaneichuk, V. I.; Tsap, T. T.; Demidov, M. L.;
Grigor'ev, V. M.
Bibcode: 1998BCrAO..94...79K
Altcode:
No abstract at ADS
Title: Observations of low-degree p-modes at the Crimean Astrophysical
Observatory.
Authors: Tsap, T. T.; Khaneichuk, V. I.; Kotov, V. A.
Bibcode: 1998BCrAO..94..129T
Altcode:
The results of observations of solar acoustic modes of low degree l
during the period 1978 - 1992 are presented. The observed frequencies
are compared with those calculated for the standard solar model.
Title: New data on the P0-oscillation of the nucleus of
the Seyfert galaxy NGC 4151.
Authors: Kotov, V. A.; Lyutyj, V. M.; Merkulova, N. I.; Metik, L. P.;
Metlov, V. G.; Khanejchuk, V. I.
Bibcode: 1998KPCB...14...52K
Altcode:
The periodicity P0 = 160.0101±0.0001 min in brightness
variations of active galactic nuclei is questioned by some
astrophysicists. Extensive photometric observations of the Seyfert
galaxy NGC 4151 were made with two reflectors at the Crimean Observatory
in an effort to verify the existence of the P0-effect. The
new data confirmed the presence of the P0-periodicity
with a phase stable over 26 years and a mean harmonic amplitude of
0.007m in the V band. This result is also substantiated
by an analysis of the X-ray observations from the Ariel-5, EXOSAT,
and Ginga satellites (1975 - 1991). Since the same period was found
in the power spectrum of global oscillations of the Sun, the authors
infer that it is of cosmological origin.
Title: Solar oscillations according to CrAO 1974 - 1994 data.
Authors: Kotov, V. A.; Khaneichuk, V. I.; Tsap, T. T.
Bibcode: 1998BCrAO..94..132K
Altcode:
Observations of solar oscillations as a whole were carried out at the
Crimean Astrophysical Observatory (CrAO) by the differential method in
1974 - 1994. The first nine years showed that the Sun oscillated with
period P0 = 160m0101±0m0016. Later, however,
a new value of the fundamental period was established, P0
= 159m9662±0m0007.
Title: Consistency of measurements of the magnetic field of the sun
as a star and its annual variation
Authors: Kotov, V. A.; Khaneichuk, V. I.; Tsap, T. T.; Demidov, M. L.
Bibcode: 1998BCrAO..94...71K
Altcode:
No abstract at ADS
Title: Upper limit for the amplitude of the solar 160-minute
oscillation in 1982 - 1989.
Authors: Kotov, V. A.; Khaneichuk, V. I.; Tsap, T. T.
Bibcode: 1998BCrAO..94..102K
Altcode:
Crimean observations of global solar oscillations show that in
1982 - 1989 the known 160-min oscillation was on average almost
absent. Arguments are given in behalf that after the "fading" interval,
the solar oscillation with a period of 160m010 can evidently
intensify in the next years to come.
Title: Evidence for a cosmological oscillation of the nucleus of
the Seyfert galaxy NGC 4151
Authors: Kotov, V. A.; Lyuty, V. M.; Haneychuk, V. I.; Merkulova,
N. I.; Metik, L. P.; Metlov, V. G.
Bibcode: 1998A&AT...16...15K
Altcode:
Long-term observations of global oscillations of the Sun revealed the
existence of the phasecoherent periodicity P0 = 160.0101 ± 0.0001
min seen in the Doppler shift of a photospheric spectral line. The
true nature of the phenomenon is yet unknown. But the most intriguing
aspect seems to be the recent discovery of the same periodicity in
luminosity variations of several AGNs which makes the puzzle of the
"ubiquitous" P0-oscillation much more mysterious. The present analysis
of all available data on the rapid variability of the nucleus of NGC
4151 fully confirms the AGN P0-oscillation (with a mean amplitude
0.01 mag). It is argued that this oscillation must have a cosmological
origin - due to, e.g., its independence of the AGN redshift. In terms
of general relativity the P0-oscillation is treated as a characteristic
time scale of metric fluctuations of the Universe. The conclusion is
made that this new astrophysical phenomenon severely contradicts today's
cosmological model of the Universe based on the Big Bang paradigm.
Title: Observations of solar global low-degree oscillations at the
Crimean Astrophysical Observatory.
Authors: Tsap, T. T.; Khanejchuk, V. I.; Kotov, V. A.
Bibcode: 1998KPCB...14..400T
Altcode:
Presents some results of the observations of the low-degree p-modes
made at the Crimean Astrophysical Observatory. The observed frequencies
are found to agree satisfactorily with the frequencies calculated for
the standard solar model.
Title: Investigation of the solar pulsation at the CrAO.
Authors: Kotov, V. A.; Haneychuk, V. I.; Tsap, T. T.
Bibcode: 1998IBUAA..12...19K
Altcode:
No abstract at ADS
Title: A resonance common to the δ Scuti stars and ellipsoidal
binaries.
Authors: Kotov, S. V.; Kotov, V. A.
Bibcode: 1998KPCB...14..419K
Altcode:
Is there a characteristic frequency common to a large number of variable
stars? Statistical analysis of 613 pulsation frequencies of 358 δ Sct
stars reveals the best resonance (the best commensurability) frequency -
νp = 104.4±0.7 μHz. The same frequency happens to be the
best resonant rotation frequency for 43 ellipsoidal binary systems
as well νR = 104.6±0.6 μHz (with a priori confidence
levels of 3.8σ and 3.4σ for both resonances, respectively). It
is intriguing that both these frequencies coincide, to within the
errors, with the frequency νsun = 104.1601±0.0001 μHz
of the global oscillations of the Sun discovered about two decades ago
(the oscillation period P0 = 160 min), the nature of these
oscillations still remains unknown. The observed P0-resonance
can hardly be reasonably explained within the scope of contemporary
astrophysical theories.
Title: The Splitting Or Disappearance of the Solar 160-Min Mode?
Authors: Kotov, V. A.; Haneychuk, V. I.; Tsap, T. T.; Hoeksema, J. T.
Bibcode: 1997SoPh..176...45K
Altcode:
The `CrAO-WSO'-network experiment was designed for detection of
low-degree oscillations of the Sun representing either its normal
g -modes or those driven by, e.g., rapid (hypothetical) rotation of
the central solar core. The Doppler-shift measurements were made in
1974-1995 at both sites during about 13600 hr, in all. Taking into
account the upper limit (≈0.08 m s-1) for amplitudes
of potential g-modes, attention is paid to the Sun's behaviour at
frequencies near the 9th daily harmonic (period P ≈160.
Title: The Long-Term Periodic Oscillation of the NGC 4151 Nucleus
Authors: Kotov, V. A.; Lyuty, V. M.; Haneychuk, V. I.; Merkulova,
N. I.; Metik, L. P.; Metlov, V. G.
Bibcode: 1997ApJ...488..195K
Altcode:
The hypothesis that the luminosity of the nucleus of the Seyfert
1 galaxy NGC 4151 varies with a period of P0 ~ 160.0101
minutes is revised. In 1987-1994 a series of photometric observations
of the NGC 4151 has been carried out in the U and V filters at several
instruments. In the total sample of 27 nights, the U data of 15 nights
showed an appreciable intranight variability of the AGN flux. Being
detrended and folded with the a priori period P0, those data
exhibited significant P0 signal coinciding in phase with
that found in previous studies. Nearly the same result is obtained
for 39 nights in the V-filter. The average harmonic amplitudes of
the P0 oscillation (for the total interval 1968-1994) are
found to be ~7 and ~2 mmag in the U and V filters, respectively. The power spectrum was computed for the total data series 1968-1994
(in all 2771 measurements including X-ray data from Ariel 5, EXOSAT,
and Ginga satellites). It reveals a prominent peak corresponding
to a period of 160.0104 +/- 0.0005 minutes (with the lower level
of confidence 3.6 σ). The latter fairly well coincides with the
P0 period discovered much earlier in the power spectrum of
global oscillations of the Sun. This analysis thus strongly supports
a cosmological interpretation of the ``ubiquitous'' oscillation with
the P0 period.
Title: The frequency 104μHz in the orbital motion of close binary
stars.
Authors: Kotov, V. A.; Kotov, S. V.
Bibcode: 1997A&A...322..177K
Altcode:
According to General Relativity, a stellar binary generates
gravitational waves at a primary frequency twice the orbital one; these
waves however have not yet been detected. If the Universe contains
gravitational radiation at discrete frequency(ies) - particularly
with the period of 160 minutes discovered in the 70-th in the Sun,
corresponding resonances might be found in the distribution of orbital
frequencies of binaries. With this in mind, we analyse all available
data on orbital frequencies of close binaries of the Galaxy. In the
frequency range 5 to 160μHz, we find one significant frequency
ν_0_=~104.2μHz - at the 4σ confidence level -which modulates
the distribution of about 5000 binaries with periods P<5.5d. The
corresponding ``resonant'' period, 160.0+/-0.5min, coincides with that
of solar pulsation P_0_=160.0+/-0.5min. The question on its origin and
also the hypothesis of a cosmological nature of the P_0_ oscillation
are briefly discussed.
Title: On rotation of ellipsoidal binary systems.
Authors: Kotov, S. V.; Kotov, V. A.; Kuvshinov, V. M.; Nikulin, I. F.
Bibcode: 1997CRASB.324..659K
Altcode: 1997CR2...324..659K
The origin of pulsation of the Sun with period P0 ≍
160 min is as yet unknown. Statistical treatment of data on the
rotation of 43 ellipsoidal binary systems with Porb <
7 days showed that the most resonant frequency of these stars equals
104.6±0.6 μHz. This agrees well with the frequency ν0
= P0-1 = 104.1601±0.0001 μHz found earlier
in global solar oscillations, and also in: (1) pulsation frequencies
of δ Sct stars and (2) in rapid variability of AGNs. These findings
thus strongly favour a cosmological interpretation of the "ubiquitous"
160-min periodicity.
Title: The most resonant pulsation frequency of delta Scuti stars
Authors: Kotov, S. V., Jr.; Kotov, V. A.
Bibcode: 1997AN....318..121K
Altcode:
Pulsation of the Sun with a period of P0 ~ 160 min
discovered about two decades ago, is still waiting explanation. In
view of the hypothesis about its cosmological origin, and attempting
to find signature of this \p\ periodicity among other (short--period
variable) stars, the pulsation frequencies of \del stars are subjected
to specific analysis. With a confidence level ~ 3.8sigma it is found
that the frequency nu_ {0} be the most ``resonant'' one for the total
sample of 318 pulsating stars of del type (the most commensurable, or
``synchronizing'', period for all these stars occurs to be 162 \pm 4
min). We conjecture that a) the p \ oscillation might be connected with
periodic fluctuations of gravity field (metrics), and b) the primary
excitation mechanism of pulsations of del stars, reflected by this
``ubiquitous'' p \ resonance, must be attributed perhaps to superfast
rotation of their inner cores (their rates tend to be in near--resonance
with the ``universal'' \nu0$ frequency). The arguments are
given favouring a cosmological nature of the \p\ oscillation.
Title: Modern Magnetooptics and Magnetooptical Materials: Studies
in Condensed Matter
Authors: Zvezdin, A. K.; Kotov, V. A.
Bibcode: 1997mmmm.book.....Z
Altcode:
No abstract at ADS
Title: The first results of solar observations made in the Crimean
Astrophysical Observatory using a magneto-optical filter
Authors: Didkovskii, L. V.; Dolgushin, A. I.; Kotov, V. A.; Khaneychuk,
V. I.; Tsap, T. T.; Rhodes, E. J.; Korzennik, S. G.; Johnson, N. M.;
Rose, P. J.
Bibcode: 1996R&QE...39..916D
Altcode:
The results of observations of Doppler velocities and solar magnetic
fields using a magneto- optical filter (MOF) are presented. The
MOF-based instrument was manufactured and supplied to the Crimean
Astrophysical Observatory (CrAO) by the University of Southern
California. It is one of three similar instruments designed to
establish the helioseismology network „Mount Wilson —CrAO —
AFiF” (Fesenkov Astrophysical Institute in Alma- Ata.) Apart from its
main purpose — obtaining a long time series of the Doppler velocity
measurements to study the internal solar structure and recording the
magnetic fields for the ground- based support of the SOHO project —
the instrument allows us to study different structural formations in
the solar atmosphere in Na D1 and D2 spectral lines. This conclusion
relies on the comparison between the magnetic field and beam velocity
maps calculated using the filtergram pairs, which were recorded twice
a minute by 512×512 video-camera (1024×1024 camera will be used in
the future studies).
Title: A pulsar inside the Sun?
Authors: Kotov, V. A.
Bibcode: 1996R&QE...39..811K
Altcode:
The Crimean observation of solar oscillations in 1974 1982 showed that
the basic period of pulsation of the Sun hidden in its deep interior
was equal to P 0=160.0101±0.0001 min. More recently, the
period was changed to the new value P 1=159.9662±0.0006 min,
which almost coincided with the annual sidelobe of the former period
P 0. The amplitude of the P1 oscillation has
increased considerably over 1994 1995. We substantiate the hypothesis
that a) the change in the period was caused by the interaction of the
P0 oscillation with the rapid rotation of the solar core
and that b) the latter has the form of a compact, highly magnetized
object like a neutron star rotating with sidereal period P1.
Title: From solar seismology to restrictions on the standard cosmology
Authors: Kotov, V. A.; Kotov, S. V.
Bibcode: 1996R&QE...39..807K
Altcode:
One and the same period, P 0=160.0101±0.0001 min, was
discovered in the global oscillation of the Sun and in the rapid
variability of several active galactic nuclei (AGN). According to
Kotov and Lyuty's hypothesis [1], the P 0 oscillation must
have a cosmological nature, since the period is independent of the AGN
redshift. The “universal” P0 osculation can represent a
fundamental scale of “cosmic time,” that is, a true cosmological
invariant which does not depend on the source moving with respect to
the observer. The phenomenon of the P0 oscillation (the
metrics of the Universe) brings the Big Bang paradigm into challenge.
Title: Oscillations of the Sun and AGN's: restrictions on the
standard cosmology
Authors: Kotov, V. A.
Bibcode: 1996cosm.conf..389K
Altcode:
No abstract at ADS
Title: The period P0 in the power spectrum of active
galactic nuclei.
Authors: Kotov, V. A.; Lyutyj, V. M.
Bibcode: 1996IzKry..93...79K
Altcode:
The high resolution power spectrum of rapid variations of luminosities
of four active galactic nuclei, NGC 3516, NGC 4151, BL Lac and PKS
2155-304, was computed near 160-min period on the basis of optical
and X-ray data 1968 - 1990. It is found that the maximal and only
statistically significant peak, within the frequency range considered,
corresponds to a period of 160.0102 (±6) min (with the confidence
level of nearly 5σ). Within the error limits it coincides with the
well-known period of global pulsation of the Sun, P0 =
160.0101 (±1) min, and thus strongly supports the hypothesis about
a cosmological nature of the P0-oscillation.
Title: Period P0 in the oscillation power spectrum of
active galactic nuclei
Authors: Kotov, V. A.; Lyuty, V. M.
Bibcode: 1996BCrAO..93...67K
Altcode:
No abstract at ADS
Title: Periodic P0 oscillations of the Sun and of ten
active galactic nuclei. A possible cosmological explanation
Authors: Kotov, V. A.; Khaneychuk, V. I.; Lyuty, V. M.
Bibcode: 1996BCrAO..93...77K
Altcode:
No abstract at ADS
Title: Oscillations of the Sun in 1974-1994
Authors: Kotov, V. A.
Bibcode: 1996MmSAI..67..973K
Altcode:
No abstract at ADS
Title: Periodic P0-oscillations of the Sun and ten AGN's
and possibility for cosmological explanation.
Authors: Kotov, V. A.; Lyutyj, V. M.; Chanejchuk, V. I.
Bibcode: 1996IzKry..93...90K
Altcode:
The photometric data on rapid, intranight variability of ten
AGN's are analysed with the aim to search for a phase-coherent
periodicity. To the Crimean 1968 - 1991 observations the authors
added all available (and suitable for analysis) world data including
X-ray measurements made by satellites HEAO-1, Ariel-5, EXOSAT
and Ginga (in total 4931 separate luminosity measurements for 10
extragalactic objects). Statistical analysis shows the presence of
the 160-min periodicity for each AGN. It fairly well coincides with
the value P0 = 160m0101±0m0001
known as period of global oscillations of the Sun, and therefore
gives more credit for a cosmological hypothesis about origin of the
"universal" P0-oscillation. A possible explanation of
the apparent independence of the observed frequency ν0 =
P0-1 on the AGN redshift is briefly discussed.
Title: Periodic P0-oscillations of the Sun and ten AGN'sa and
possibility for cosmological explanation.
Authors: Kotov, V. A.; Lyuty, V. M.; Haneychuk, V. I.
Bibcode: 1996IzKAO..93...90K
Altcode:
No abstract at ADS
Title: First Results of Solar Oscillations Made in Crimean
Astrophysical Observatory Using Magneto-Optical Filter
Authors: Didkovsky, L. V.; Rhodes, E. J., Jr.; Dolgushin, A. I.;
Haneychuk, V. I.; Johnson, N. M.; Korzennik, S. G.; Kotov, V. A.;
Rose, P. J.; Tasp, T. T.
Bibcode: 1996RaF....39...11D
Altcode:
No abstract at ADS
Title: From Solar Oscillations to Restrictions on the Standard
Cosmology
Authors: Kotov, V. A.
Bibcode: 1995ESASP.376b.305K
Altcode: 1995help.confP.305K; 1995soho....2..305K
No abstract at ADS
Title: A Superfast Rotation of the Central Solar Core?
Authors: Kotov, V. A.
Bibcode: 1995ESASP.376b.299K
Altcode: 1995help.confP.299K; 1995soho....2..299K
No abstract at ADS
Title: General magnetic field of the Sun as a star
Authors: Kotov, V. A.
Bibcode: 1995BCrAO..91..102K
Altcode:
No abstract at ADS
Title: A Cosmological Origin of the P_0 Oscillation of the Sun
Authors: Kotov, V. A.
Bibcode: 1995ASPC...76..220K
Altcode: 1995gong.conf..220K
No abstract at ADS
Title: Observation of the Sun as a star: cosmological aspect.
Authors: Kotov, V. A.
Bibcode: 1995BRASP..59.1612K
Altcode:
Measurements of the general magnetic field of the Sun in 1968 -
1992 revealed a predominance of two synodic rotation periods, 28.96
and 28.20 days. The first period is conditioned by the photosphere
magnetic structure rotation, the second one possibly reflects a
rigid-body rotation of the radiative zone. Of particular interest is
the yearly variation, which cannot be explained by any terrestrial
apparatus. It can be a consequence of the star rotation in an
inertial space if its interior structure radically differs from the
standard model. Observation of solar oscillations as a whole led to
the discovery of 160-min pulsations. Later the same period was found
in the brightness variations of galaxy's active nuclei, which shows
evidence for a cosmological origin of the oscillations.
Title: Academician A. B. Severnyi and his contribution to modern
astrophysics
Authors: Kotov, V. A.
Bibcode: 1995BCrAO..92....7K
Altcode:
No abstract at ADS
Title: Universal occultations of the Sun and active galactic nuclei
and an attempt of interpretation.
Authors: Kotov, V. A.; Larionov, M. G.; Lyuty, V. M.; Haneychuk, V. I.
Bibcode: 1995IzKry..92..126K
Altcode:
No abstract at ADS
Title: On Possible Resonance Frequency (4.9 Hz) of Neutron Stars
Authors: Kotov, V. A.; Fomin, V. P.
Bibcode: 1995pns..book..267K
Altcode:
No abstract at ADS
Title: The oscillations of the Sun and new evidence of rapid rotation
of the central core
Authors: Kotov, V. A.; Khaneichuk, V. I.; Tsap, T. T.
Bibcode: 1995BCrAO..92...94K
Altcode:
No abstract at ADS
Title: Summary of the Crimean 20-Year Observation of Solar Global
Oscillations
Authors: Kotov, V. A.; Haneychuk, V. I.; Tsap, T. T.
Bibcode: 1995ASPC...76...82K
Altcode: 1995gong.conf...82K
No abstract at ADS
Title: Universal oscillations of the Sun and active galactic nuclei
and an attempt at interpretation
Authors: Kotov, V. A.; Larionov, M. G.; Lyutyi, V. M.; Khaneichuk,
V. I.
Bibcode: 1995BCrAO..92..109K
Altcode:
No abstract at ADS
Title: Rapid variability of active galactic nuclei : the 160min
periodicity in NGC 3516, NGC 4151 and quasar 3C 273.
Authors: Kotov, V. A.; Haneychuck, V. I.; Lyuty, V. M.
Bibcode: 1994AN....315..333K
Altcode:
The analysis of tall the available data between 1968 and 1991 on rapid
variability of optical and X-ray luminosity of three Active Galactic
Nuclei (AGNs), NGC 3516, NGC 4151 and 3C 273, shows the presence
of small-amplitude (approximately 1%) but statistically confident
(approximately = 5(sigma) periodicity of 160.0105 (+/- 6) min. Within
the error limits it coincides with the period Po = 160.0101
(+/-1) min of global oscillations of the Sun. An independence of
the observed period on AGN red shift z favors the hypothesis about a
cosmological origin of the 160min oscillation.
Title: Ground-Based Near-Infrared Observations of Global Solar
Oscillations
Authors: Didkovsky, L. V.; Kotov, V. A.
Bibcode: 1994IAUS..154..277D
Altcode:
No abstract at ADS
Title: On Sunspot and Facular Contrast Variations Near 2 MU M and
4 MU M
Authors: Kotov, V. A.; Koutchmy, S.
Bibcode: 1994IAUS..154..265K
Altcode:
No abstract at ADS
Title: The general magnetic field of the Sun as a star.
Authors: Kotov, V. A.
Bibcode: 1994IzKry..91..124K
Altcode:
The author presents informations on measurements of the general magnetic
field of the Sun as a star and its correlations with the interplanetary
magnetic field. Results of an analysis of the magnetic asymmetry of
the Sun are given. The rotation of the global magnetic field of the Sun
and the interplanetary magnetic field is studied. Results of long-term
observations of the 160-min oscillations of the general magnetic field
of the Sun are discussed.
Title: A Puzzle of the 160-MINUTE Periodicity in the Sun Binaries
Rr-Lyrae Stars and Active Galactic Nuclei - the Signatures of a
Cosmological Origin
Authors: Kotov, V. A.; Lyuty, V. M.
Bibcode: 1993ASPC...42..289K
Altcode: 1993gong.conf..289K
No abstract at ADS
Title: The Search for 160-MINUTE Oscillations in the Stanford and
Crimean Solar Velocity Observations - 1974-1991
Authors: Kotov, V. A.; Scherrer, P. H.; Hoeksema, J. T.; Haneychuk,
V. I.; Tsap, T. T.
Bibcode: 1993ASPC...42..293K
Altcode: 1993gong.conf..293K
No abstract at ADS
Title: Oscillations of the active galactic nuclei with the 160 minute
period and antimatter hypothesis.
Authors: Kotov, V. A.; Lyuty, V. M.
Bibcode: 1993IzKry..87..144K
Altcode:
No abstract at ADS
Title: A Striking Similarity Between the Sun, Binaries and RR Lyrae
stars in globular clusters
Authors: Kotov, Valery A.
Bibcode: 1993npsp.conf..160K
Altcode: 1993IAUCo.139..160K
No abstract at ADS
Title: New evidences of the 160-minute oscillations in active
galactic nuclei.
Authors: Kotov, V. A.; Lyuty, V. M.; Haneychuk, V. I.
Bibcode: 1993IzKry..88...47K
Altcode:
No abstract at ADS
Title: New evidence of 160-minute oscillations in active galactic
nuclei
Authors: Kotov, V. A.; Lyutyi, V. M.; Khaneichuk, V. I.
Bibcode: 1993BCrAO..88...40K
Altcode:
No abstract at ADS
Title: Oscillations of active galactic nuclei with 160-minute period
and the antimatter hypothesis
Authors: Kotov, V. A.; Lyutyi, V. M.
Bibcode: 1993BCrAO..87..132K
Altcode:
No abstract at ADS
Title: Plans for MT.WILSON - Crimean Observatory High-Degree
Helioseismology Network
Authors: Rhodes, E. J., Jr.; Cacciani, A.; Dappen, W.; Didkovsky,
L. V.; Hill, F.; Korzennik, S. G.; Kosovichev, A. G.; Kotov, V. A.;
Scherrer, P. H.
Bibcode: 1993ASPC...42..477R
Altcode: 1993gong.conf..477R
No abstract at ADS
Title: On the Upper Limit for Detecting G-Mode Oscillations of the Sun
Authors: Scherrer, P. H.; Hoeksema, J. T.; Kotov, V. A.
Bibcode: 1993ASPC...42..281S
Altcode: 1993gong.conf..281S
No abstract at ADS
Title: Pulsations of active galactic nuclei and problem of antimatter
in the universe
Authors: Kotov, V. A.; Lyutyi, V. M.
Bibcode: 1992BCrAO..86..101K
Altcode:
No abstract at ADS
Title: Universal oscillations of active galactic nuclei and anomalous
distribution of the initial phases.
Authors: Kotov, V. A.; Lyuty, V. M.
Bibcode: 1992IzKry..85...91K
Altcode:
No abstract at ADS
Title: Short-period variations in the Sun's global magnetic field.
Authors: Demidov, M. L.; Kotov, V. A.; Grigor'ev, V. M.
Bibcode: 1992BCrAO..82..135D
Altcode:
Measurements have been made on the Sun's general magnetic field in 1975
- 1978 and in 1987 at the Crimean and Sayan observatories and at Mount
Wilson; these have shown that there are more or less stable oscillations
with periods of about 47, 60, 85, and 160 min with mean amplitudes of
about 1 μT. The new Sayan observations of 1987 confirm the previous
conclusion that there is long-time coherence in the oscillation with
period 160.0101 min.
Title: Solar pulsations: effects due to the 22-year activity cycle?
Authors: Kotov, V. A.; Tsap, T. T.; Didkovskij, L. V.
Bibcode: 1992BCrAO..82..127K
Altcode:
Regular measurements have been made on the differential Doppler
velocity in the Crimea between 1974 and 1987 (in all, 902 days, 5612 hr
of observation), which confirm the long-term phase-coherent pulsation
with a period of 160.01 min. The new data also suggest that the 160-min
pulsation may have a multiplet fine structure. In particular, there
have been large changes in the amplitude and phase of the pulsation
in the period 1983 - 1987, which may mean that after 1982 - 1983 one
has observed the 160 min oscillations related to the second half of
the 22-year magnetic activity cycle. This new and unexpected feature
opens up scope for probing the solar interior, and also for researching
the internal rotation and the 11 (22)-year solar cycle.
Title: On the 160-minute variability of NGC 4151: a rebuttal
Authors: Lyutyi, V. M.; Kotov, V. A.
Bibcode: 1992BCrAO..84...95L
Altcode:
No abstract at ADS
Title: Study of the Sun's interior: pulsation of the Sun and
22-year cycle
Authors: Kotov, V. A.; Kaneychuk, V. I.; Tsap, T. T.
Bibcode: 1992BCrAO..85....1K
Altcode:
No abstract at ADS
Title: Question of the 160-minute variability of the NGC 4151 :
the answer to opponents.
Authors: Lyuty, V. M.; Kotov, V. A.
Bibcode: 1992IzKry..84..104L
Altcode:
No abstract at ADS
Title: Universal oscillations of active galactic nuclei and anomalous
distribution of initial phases
Authors: Kotov, V. A.; Lyutyi, V. M.
Bibcode: 1992BCrAO..85...86K
Altcode:
No abstract at ADS
Title: Pulsations of the active galactic nuclei and problem of the
antimatter in the universe.
Authors: Kotov, V. A.; Lyuty, V. M.
Bibcode: 1992IzKry..86..108K
Altcode:
No abstract at ADS
Title: Fast periodic fluctuations of the Sun's general magnetic field
Authors: Kotov, V. A.; Demidov, M. L.; Grigor'ev, V. M.; Khaneichuk,
V. I.; Tsap, T. T.
Bibcode: 1992BCrAO..84..149K
Altcode:
No abstract at ADS
Title: 160-MINUTE Pulsation of the Sun - New Observational Results
Authors: Kotov, V. A.; Tsap, T. T.; Ganeichuk, V. I.
Bibcode: 1991SoPh..133...95K
Altcode:
The 1974-1988 Crimean measurements of the solar line-of-sight velocity
continue to show the presence of a statistically significant periodicity
P1 = 160.009 (±) min with an average harmonic amplitude
of about 21 cm s−1. The period is supposed to be that
of the global pulsation of the Sun but with a little-known physical
mechanism of excitation.
Title: 160-minute oscillations of certain extragalactic objects
Authors: Kotov, V. A.; Lyutyi, V. M.
Bibcode: 1991BCrAO..83..197K
Altcode:
No abstract at ADS
Title: The helioseismology experiment on the Phobos planetary
mission. Preliminary results
Authors: Frohlich, C.; Bonnet, R. M.; Bruns, A. V.; Vial, J. C.;
Delaboudiniere, J. P.; Domingo, V.; Kollath, Z.; Kotov, V. A.;
Rachkovskii, D. N.; Wehrli, Ch.; Toulain, T.; Shumko, S. M.
Bibcode: 1991BCrAO..83...18F
Altcode:
No abstract at ADS
Title: Solar gravity modes.
Authors: Hill, H.; Froehlich, C.; Gabriel, M.; Kotov, V. A.
Bibcode: 1991sia..book..562H
Altcode:
The internal gravity modes, or g-modes, of the Sun may be important
both in affecting the internal structure of the Sun and in furnishing a
diagnostic probe of the solar interior. The internal structure could be
altered by core mixing due to unstable g-modes or by nonlinear effects
due to large-amplitude g-modes located in the core. On the other hand,
small-amplitude g-modes operating in the linear regime offer the
possibility of studying in detail the present state of internal solar
structure such as the internal rotation rate, the Brunt-Väisälä
frequency, the speed of sound and the mean molecular weight. In all
of these roles, the solar g-modes may be important. The g-modes may
be a contributor to the solar neutrino paradox and/or they may be a
source of information leading to a more complete understanding of the
physics responsible for the paradox. The observational work on solar
g-modes does not exclude any of these possibilities at this time.
Title: The 160-minute period in differential measurements of the
brightness of the Sun (1976-1987)
Authors: Kotov, V. A.; Didkovskii, L. V.; Khaneichuk, V. I.
Bibcode: 1991BCrAO..83...27K
Altcode:
No abstract at ADS
Title: The helioseismological experiment at the Phobos interplanetary
station - Preliminary results
Authors: Froehlich, C.; Bonnet, R. M.; Bruns, A. V.; Vial, J. C.;
Delaboudiniere, J. P.; Domingo, V.; Kollath, Z.; Kotov, V. A.;
Rachkovskii, D. N.; Wehrli, Ch.
Bibcode: 1991IzKry..83...22F
Altcode:
Preliminary results obtained from IPHIR (Interplanetary Helioseismology
by Irradiance Measurements), a solar irradiance experiment on board
the Soviet planetary mission Phobos-2, are presented. During the
spacecraft's flight to Mars, the instrument gathered valuable data on
tiny variations of solar irradiance over the course of six months. The
data clearly show 5-min oscillations with relative amplitudes of about
10 exp -5 and with a well-defined pattern of discrete peaks in the
power spectrum. The data of the red channel (it exhibited the lowest
degradation of sensitivity over time) reveal remarkable temporal changes
of amplitudes of discrete peaks within a period range of about 5 min,
but with excellent frequency stability.
Title: The 160-minute oscillations of some extragalactic objects.
Authors: Kotov, V. A.; Liutyi, V. M.
Bibcode: 1991IzKry..83..216K
Altcode:
An analysis of the UBV photometric and X-ray data on the rapid
variability of active galactic nuclei (AGN) shows that there is a
statistically significant (from 2- to 5-sigma confidence level) period
of 160.1 min for several AGN, with an average harmonic amplitude of
about 4 percent for X-rays and 1 percent for optical data. EXOSAT
measurements showed the presence of 160-min periodicity in NGC 4051,
NGC 4151, Mrk 335, and possibly NGC 6814 and MCG-6-30-15. The initial
phases of this 160-min variability in the X-ray fluxes for five AGN are
found to coincide with the phase of the 160-min oscillations of the sun.
Title: A 160-minute period in differential measurements of solar
brightness (1976-1987)
Authors: Kotov, V. A.; Didkovskii, L. V.; Khaneichuk, V. I.
Bibcode: 1991IzKry..83...34K
Altcode:
Differential (center-to-limb) measurements of the sun's brightness
were performed at the Crimean Astrophysical Observatory with a solar
magnetograph, a near-IR brightness monitor, and photodiode arrays. An
analysis of all the measurements (487 days of observations, 2661 hours
in all) made from 1976 through 1987 in different spectral passbands
(from 0.51 to 1.65 micron) showed the presence of statistically
significant periodicity (160.009 +/- 2 min), with a confidence level
of 2 to 4 sigma. This value is in excellent agreement with the period
160.009 +/- 2 min found much earlier in Doppler shift measurements. The
mean relative amplitude of total irradiance variations for this
160.01-min period, as inferred from the data, is about 4 x 10 exp -6,
and therefore does not contradict the upper limit of about 5 x 10 exp
-6 established by the ACRIM-SMM bolometric measurements.
Title: Compact Extragalactic Objects - Search for 160-MIN Periodicity
in X-Ray Data
Authors: Lyutyi, V. M.; Kotov, V. A.
Bibcode: 1990SvAL...16..331L
Altcode:
No abstract at ADS
Title: Compact extragalactic objects : a search for 160-minute
periodicity in the X-ray data.
Authors: Lyuty, V. M.; Kotov, V. A.
Bibcode: 1990PAZh...16..771L
Altcode: 1990PisAZ..16..771L
Data on the X-ray variability of the Seyfert 1 galaxies NGC 4051 and
4151 collected by the Ariel-5 and Exosat satellites are examined. It
is revealed that a statistically significant 160.010 min period with
a harmonic amplitude of 4-9 percent exists. It is predicted that
the same periodicity exists for the nucleus of the third Seyfert,
MCG-6-30-15. Results from this study support with earlier theories
concerning the 'ubiquitous' status of the 160 min oscillations, based
on observations of the sun and the nuclei of other Seyfert galaxies
and the quasar 3C 273.
Title: Variation in the 160.010 m period of the solar relative
difference brightness
Authors: Li, Ru-Feng; Kotov, V. A.; Didkovskii, L. V.
Bibcode: 1990SCSMP..33.1100L
Altcode:
Two photoelectric diode arrays (16 x 16 and 32 x 32 pixels,
respectively) were used to measure the difference brightness of the
center of the sun with respect to the limb of the solar disk in 1986 at
wavelengths of 0.7-0.8 micron. The results indicate a period of 160 m
and an average amplitude of 0.00008 solar relative intensity unit. A
refined value of the oscillation period of 160.0099 m is obtained
from the periodic values of the difference brightness observed for 358
days (1870 hr) over the period 1976-1986 at the Crimean Astrophysical
Observatory. This is in good agreement with the IR observed value of
160.0100 m (+ or - 6) and a value of 160.010 m (+ or - 1) obtained at
the Doppler difference velocity.
Title: 160-MINUTE Solar Variations and the 22-YEAR Cycle
Authors: Kotov, V. A.; Tsap, T. T.
Bibcode: 1990SoPh..128..269K
Altcode: 1990IAUCo.121P.269K
Systematic measurements of the differential Doppler velocity of the Sun
have been performed in Crimea from 1974 through 1988 (total 987 days,
6197 hours of observations). They confirm the presence of a long-term
phase-coherent solar pulsation with a period of 160.010 min. On the
other hand, the analysis of new data suggests that solar 160 min
pulsation might, in frequency, have a multiplet fine structure. In
particular, large changes of amplitude and phase of the pulsation over
the years 1982-1986 may indicate that during the last few years we have
been observing the solar 160 min oscillation of the `second portion'
of the 22 year solar cycle.
Title: On short-term variations of the global magnetic field of
the Sun.
Authors: Demidov, M. L.; Kotov, V. A.; Grigor'ev, V. M.
Bibcode: 1990IzKry..82..147D
Altcode:
Measurements of the mean magnetic field of the Sun seen as a star
made in 1975 - 1978 and 1987 at the Crimean, Mount Wilson and Sayan
observatories show the presence of more or less persistent oscillations
with periods near 47, 60, 85 and 160 minutes and average amplitudes
≡1 mkT. The new Sayan-1987 observations appear to confirm the
previous conclusion [1976, 1985] about long-time coherency of the
famous 160,0101-minute oscillation of the Sun.
Title: Short-period variations in the Sun's global magnetic field
Authors: Demidov, M. L.; Kotov, V. A.; Grigor'ev, V. M.
Bibcode: 1990BCrAO..82..135D
Altcode:
No abstract at ADS
Title: A Problem with the 160-Minute Pulsation of the Sun
Authors: Kotov, V. A.
Bibcode: 1990LNP...367..235K
Altcode: 1990psss.conf..235K
Differential measurements (1974-1988) of the solar velocity and
photospheric brightness show the presence of long-term pulsation of the
Sun with a period of P o=160.0101(±1) min. Its nature is poorly known
since it seems hardly possible to explain the periodicity in terms
of solar g-modes. But the most fascinating appears to be the recent
discovery of the same 160-min periodicity in the light-flux variations
of several AGN (active galactic nuclei). This finding strongly supports
the hypothesis advanced much earlier about cosmological origin of
the oscillation.
Title: Variation in the 160.010 m period of the solar relative
difference brightness
Authors: Li, R. F.; Kotov, V. A.; Didkovskii, L. V.
Bibcode: 1990SSSMP..33.1100L
Altcode:
No abstract at ADS
Title: Pulsation of the Sun: remarkable change due to the 22-year
cycle of activity?
Authors: Kotov, V. A.; Tsap, T. T.; Didkovskii, L. V.
Bibcode: 1990IzKry..82..138K
Altcode:
Systematic measurements of differential Doppler velocity performed
at the Crimean Observatory from 1974 through 1987 (in all 902 days,
5612 hours of observations) confirm the presence of the long-term
phase-coherent solar pulsation with a period of 160.01 min. On the other
hand, the analysis of new data suggests that 160-min pulsation on the
Sun might have a multiplet (in frequency) fine structure. Particularly,
great changes of amplitude and phase of the pulsation over 1983 - 1987
years may indicate that since 1982 - 1983 years the authors observe
indeed 160-min oscillation pattern inherent in the "second part" of
the 22-year cycle of solar magnetic activity. Being verified, this
unpredicted property of the pulsation can offer a novel possibility
for probing the Sun's interior and perhaps for the study of the solar
internal rotation and 11(22)-year cycle.
Title: Solar pulsations: effects due to the 22-year activity cycle?
Authors: Kotov, V. A.; Tsap, T. T.; Didkovskii, L. V.
Bibcode: 1990BCrAO..82..127K
Altcode:
No abstract at ADS
Title: V1521 Cygni (Cygnus X-3)
Authors: Kotov, V.; Nesterov, N. S.
Bibcode: 1989IAUC.4826....2K
Altcode: 1989IAUC.4826....0K
V. Kotov, Crimean Astrophysical Observatory, reports that the recent
flare (cf. IAUC 4817) was independently detected by N. S. Nesterov,
who found the 8.2-mm flux to increase from < 0.5 Jy on July 19 to
11.32 +/- 0.1 Jy on July 21.
Title: Five HERZ - a characteristic frequency of neutron stars ?
Authors: Kotov, V. A.; Fomin, V. P.
Bibcode: 1989Afz....30..362K
Altcode:
No abstract at ADS
Title: Five hertz—A characteristic frequency of neutron stars?
Authors: Kotov, V. A.; Fomin, V. P.
Bibcode: 1989Ap.....30..221K
Altcode:
No abstract at ADS
Title: 5-HZ - a Characteristic Frequency of Neutron Stars
Authors: Kotov, V. A.; Fomin, V. P.
Bibcode: 1989Afz....30..221K
Altcode:
No abstract at ADS
Title: IPHIR: The helioseismology experiment on the PHOBOS mission.
Authors: Fröhlich, C.; Bonnet, R. M.; Bruns, A. V.; Delaboudinière,
J. P.; Domingo, V.; Kotov, V. A.; Kollath, Z.; Rashkovsky, D. N.;
Toutain, T.; Vial, J. C.; Wehrli, C.
Bibcode: 1988ESASP.286..359F
Altcode: 1988ssls.rept..359F
IPHIR (InterPlanetary Helioseismology by IRradiance measurements) is
a solar irradiance experiment on the USSR planetary mission PHOBOS to
Mars and its satellite Phobos. The experiment is a cooperative effort
of PMOD/WRC, LPSP, SSD/ESA, KrAO and CRIP. The sensor is a three channel
sunphotometer (SPM) which measures the solar spectral irradiance at 335,
500 and 865 nm with a precision of better than 1 ppm. A two axis solar
sensor (TASS) is added to monitor the moderate solar pointing of the
spacecraft. A microprocessor based data processing unit controls the
sensor operation, acquires the data, and performs the data compression
for the transmission at a mean rate of 1 bit/s. The two spacecrafts
have been launched on July 7th and 12th, 1988. The experiment on
PHOBOS I gathered data during 45 days before the S/C was lost, the
one on PHOBOS II is still operating. The data recovery is excellent
with virtually 100% coverage. Although the signal is disturbed by the
pointing of the spacecraft the results of a preliminary analysis in
the range of the 5-minutes oscillations demonstrate the improvement
achievable due to the fact that the time series is truly continuous
and the instrumental and sampling noise is very low.
Title: Book Review: The galaxy and the solar system. / U Arizona
Press, 1986.
Authors: Kotov, V. A.; Kostik, R.; Shchukina, N.; Švestka, Zdeněk;
Kotov, V. A.
Bibcode: 1988SoPh..115..203K
Altcode: 1988SoPh..115..203S
No abstract at ADS
Title: A. B. Severny (1913-1987)
Authors: Kotov, V. A.; Mozzerin, V. M.
Bibcode: 1988SoPh..115....1K
Altcode: 1988SoPh..115....1.
No abstract at ADS
Title: Observations of Solar Global Oscillations 1983-1985 and
Potential Influence of Terrestrial Sources of Errors
Authors: Severny, A. B.; Kotov, V. A.; Tsap, T. T.
Bibcode: 1988IAUS..123...33S
Altcode:
The Earth atmospheric pressure fluctuations in the 5-min range of
periods are analysed and their influence on observations of solar
5-min oscillations are briefly discussed. New series of observations
confirmed the oscillations of the Sun with period of 160.010 min.
Title: Five-minute oscillations of the solar brightness: observations
with a photodiode array
Authors: Didkovskii, L. V.; Kotov, V. A.; Tarasova, T. N.
Bibcode: 1988BCrAO..79..174D
Altcode: 1990BCrAO..79..174D
The authors present the results from six-days observations of
5m oscillations of the solar brightness in 1984 totaling
approximately 58 hours. With the aid of a photodiode array (16x16
pixels), temporal variations of solar intensity in the central portion
of the Sun's disk (≡0.2 Dsun) were measured within spectral
passband 0.82±0.13 μm with 1m integration time. Average
power spectrum shows the presence of 5m oscillations with
a discrete pattern of peaks and mean amplitudes ≡10-4
in relative units. A typical frequency splitting, 69.6±0.8 μHz, is
close to but yet significantly different from a well-known splitting
67.7 μHz inferred from Doppler observations. The authors also noted
that in 1984 observational season the mean power in 5m
range of periods was decreased by a factor of 3 in comparison with
analogous measurements made in 1983. It is supposed that these changes
probably reflect real changes of solar brightness oscillations which,
in turn, may be caused by the 11-year solar activity cycle.
Title: 160-minutes oscillations of the Sun: observations in 1974
- 1986.
Authors: Kotov, V. A.; Severnyj, A. B.; Tsap, T. T.
Bibcode: 1988IzKry..79....3K
Altcode:
Observations of global oscillations of the Sun were carried out at
the Crimean Astrophysical Observatory during 711 days (4345 hours in
total) in 1974 - 1986. These data confirm an existence and dominant
character of solar low frequency oscillations with a period of
160m0100(±6). The latter exhibits a remarkable long-time
phase stability. Observations show that the amplitude of the 160-minute
oscillation varies significantly during the observational season and
also from year to year. The most interesting seems to be the progressive
decrease of yearly-mean amplitude: from about 1.2 m/s in 1974 - 1975 to
about 0.3 m/s in 1984 - 1986. It is suggested that this decrease might
be connected with the 22-year cycle of solar activity and, therefore,
may throw additional light on the nature of the 160-minute periodicity
in the Sun.
Title: 160.01-Min oscillations of compact extragalactic objects and
plausible cosmological consequences
Authors: Kotov, V. A.; Lyutyi, V. M.
Bibcode: 1988BCrAO..79..130K
Altcode: 1990BCrAO..79..130K
The previous analysis of UBV-photometry of the quasar 3C 273 and the
Seyfert galaxy NGC 4151 is extended to nuclei of other Seyferts in
search of oscillations with a "ubiquitous" period P0 =
161.0101 (±1)m. Now the authors find the presence of the
same period, within errors, for three more Seyferts: NGC 1275 (period
160.0094 (±8)m), NGC 3516 (160.0100 (±9)m),
and NGC 7469 (159.98 (±3)m) - with more or less random
scattering of phases and total relative amplitudes (2-3%). It is argued
that the periodic effect can be accounted for by neither observational
biases nor some artifacts in the reduction procedure. For the NGC 4151
the result is strongly supported by analysis of X-ray data obtained on
board the Ariel-5 and EXOSAT satellites. It is pointed out that true
nature of the solar 160m oscillation with its seemingly
universal character is still an open question. It is hypothesized that
the P0 period may have a status of a preferred time-scale for
the Universe. The hypothesis can possibly help to avoid a singularity
present in the standard Big Bang cosmology.
Title: 160-Minute oscillations of the Sun: observations in 1974-1986
Authors: Kotov, V. A.; Severnyi, A. B.; Tsap, T. T.
Bibcode: 1988BCrAO..79....1K
Altcode: 1990BCrAO..79....1K
Observations of global oscillations of the Sun were carried out
at the Crimean Astrophysical Observatory during 711 days (4345
hours in total) in 1974 - 1986. These data confirm an existence and
dominant character of solar low frequency oscillations with a period
of 160.0100m (±6). The period exhibits a remarkable
long-time phase stability which appears to be persistent for more
than a decade. The period agrees perfectly well with the value
160.0101m (±1) established earlier from analysis of
onset times of solar flares observed on the Sun during 1947 - 1980
interval. Observations show that amplitude of the 160-minute oscillation
varies significantly during observational season and also from year to
year. The most interesting feature seems to be a progressive decrease
of yearly mean amplitude: from about 1.2 m/sec in 1974 - 1975 to about
0.3 m/sec in 1984 - 1986. It is suggested that this decrease might
be connected with the 22-year cycle of solar activity and, therefore,
may throw additional light on the nature of 160-minute periodicity in
the Sun.
Title: Space-time analysis of the Sun's brightness oscillations. I.
Authors: Didkovskii, L. V.; Kotov, V. A.
Bibcode: 1988BCrAO..80..114D
Altcode: 1990BCrAO..80..114D
A 1024-cell 32x32 photodiode array was used to register the global
oscillations of the Sun's brightness in a 0.73±0.10 μm spectral
band. A simple procedure for processing of the observational data
based on approximation of the "quiet Sun" brightness distribution by
Chebyshev polynomials is described. A dinstinct concentration of power
peaks in the range of periods around 5 minutes is seen in the power
spectra of the "oscillating Sun minus quiet Sun" remainders.
Title: Photometry of the Seyfert galaxy NGC 4151 and the quasar 3C
273: the 160.010 minutes period.
Authors: Kotov, V. A.; Lyutyj, V. M.
Bibcode: 1988IzKry..78...89K
Altcode: 1988IKryO..78...89K
A reanalysis of the U-photometric data (1968 - 1986) of the nucleus of
the Seyfert galaxy NGC 4151 fully confirmed the previous conclusion
about the presence of the period PG = 160.0098 (±5)
min with a harmonic amplitude 0.014 mag. Similar analysis of
the 18 year (1968 - 1986) photometry of the quasar 3C 273 also
reveals an existence of the same period: PQ = 160.0105
(±7) min (harmonic amplitude 0.015 mag.). Both periods coincide
with the well-known period P0 = 160.0106 (±6) min of
global oscillations of the Sun. Such ubiquitous character of the
160-min period may suggest its cosmological status and, perhaps,
indicates that this period may be a new astrophysical parameter
with intriguing inferences for cosmology. The authors propose a
simple relation between the Hubble constant H0 and the
period P0:dP0/dt = H0P0 =
1.9×10-14. The resulting life-time of the 160-min period
appears to be equal to ≡16×109years, i.e. the age of
the Universe.
Title: Spatially-temporal analysis of the solar brightness
oscillations. I.
Authors: Didkovskij, L. V.; Kotov, V. A.
Bibcode: 1988IzKry..80..118D
Altcode:
The 1024-channel (32×32) photodiode array is used for detection of the
global solar brightness oscillations within 0.73±0.10 μm passband. A
simple method of data reduction based on computation of the "quiet Sun",
approximated by the system of Chebychev polynomials, is described. Power
spectra of the residuals "oscillating Sun minus quiet Sun" clearly
show a concentration of power in the 5-minute range of periods.
Title: The 160.01 minutes oscillations of compact extragalactic
objects and plausible cosmological consequences.
Authors: Kotov, V. A.; Lyutyj, V. M.
Bibcode: 1988IzKry..79..139K
Altcode: 1988IKryO..79..139K
UBV-photometry is extended to nuclei of Seyferts in
search for oscillations with a «ubiquitous» period
P0 = 160.0101(±1)m: NGC 1275 (period
160.0094(±8)m), NGC 3516 (160.0100(±9)m) and NGC
7469 (159.98(±3)m) - with more or less random scattering
of phases and total relative amplitudes (2 - 4)%. It is argued that
the periodic effect can be accounted for by neither observational
biases nor some artefacts in the reduction procedure. For NGC 4151 the
results are strongly supported by analysis of X-ray data obtained on
board the Ariel-5 and EXOSAT satellites. It is pointed out that the
true nature of solar 160m-oscillations with its seemingly
universal character is still an open question. It is hypothesized that
the P0-period may have a status of a preferred time-scale
for the Universe. The latter can possibly help us to avoid a singularity
present in the standard big-bang cosmology.
Title: Periodic variations of solar brightness observed with the
1024-channel photodiode array.
Authors: Didkovskij, L. V.; Kotov, V. A.
Bibcode: 1988IzKry..80..124D
Altcode:
The observations of long-period brightness oscillations of the Sun
were carried out by using a photodiode array (32×32 pixels) within
the spectral passband 0.73±0.10 μm during 7 days in 1986. The spatial
resolution was about 53 arc sec and accumulation time 38 sec. The data
analysis showed that relative amplitudes of brightness variations
increase toward the centre of the solar disk. It suggests a real
(solar) origin of a significant part of the observed variations. For
the central part of the disk (0.3 Dsun in diameter) the
data reveal 160-min oscillations with the average relative amplitude
≡5×10-5. The phase of 160-min oscillations nicely agrees
with the one determined from earlier, 1976 - 1985, observations.
Title: Five-minute oscillations of the solar brightness: observations
with a photodiode array.
Authors: Didkovskij, L. V.; Kotov, V. A.; Tarasova, T. N.
Bibcode: 1988IzKry..79..184D
Altcode:
The authors present the results from 6-days observations of
5m-oscillations of the solar brightness in 1984 totalling
approximately 58 hours. Average power spectrum shows the presence of
5m-oscillations with a discrete pattern of peaks and mean
amplitudes ≡10-4 in relative units. A typical frequency
splitting, 69.5±0.8 mkHz, is close to but yet significantly
different from a well-known splitting 67.7 mkHz inferred from
Doppler observations. In 1984 observational season the mean power
in 5m-range of periods is decreased by factor of 3 in
comparison with analogous measurements made in 1983. It is supposed
that these changes reflect probably real changes of solar oscillations
seen in brightness which, in turn, may be caused by 11-year cycle of
solar activity.
Title: Periodic variations of the brightness of the Sun: experience
in observations with a 1024-channel array
Authors: Didkovskii, L. V.; Kotov, V. A.
Bibcode: 1988BCrAO..80..120D
Altcode: 1990BCrAO..80..120D
Oscillations of the Sun's brightness at 0.73±0.10 μm were observed
with a 32x32 photodiode array. The measurements were made on 7 days
in 1986 with a spatial resolution of ≡53″and an accumulation
time of 38 sec. The relative amplitude of the long-period brightness
variations rises significantly toward the center of the disk. It is
assumed that the variations are due in large part to oscillations of the
Sun. For a central region of the disk 0.3 Dsun
in diameter, 160-minute oscillations are detected with a relative
amplitude of ≡5·10-5. The phase of these variations for
the 160.010-min period practically coincides with the mean phase of
the differential-brightness oscillations from earlier (1976 - 1985)
observations.
Title: Photometry of the Seyfert galaxy NGC 4151 and the quasar 3C
273: the 160.010-minute period
Authors: Kotov, V. A.; Lyutyi, V. M.
Bibcode: 1988BCrAO..78..100K
Altcode: 1989BCrAO..78..100K
A new analysis of photometric data on the nucleus of the Seyfert
galaxy NGC 4151 (1968 - 1986, U filter) fully confirmed the conclusion
indicating a period PG = 160.0098m(±5) with
a harmonic amplitude of 0.014 magnitude. Analysis of 18 years of
photometric observations of the quasar 3C 273 (1968 - 1986) also
indicated that the same period is present here within the limits of
error: PQ = 160.0105m(±7), amplitude 0.015
magnitude. The two periods agreed with the known period P0
= 160.0106m(±6) detected earlier in the power spectrum
of the Sun's global oscillations. This "universal" nature of the
160m period may indicate that it is of cosmologic origin,
and the period itself appears to be a new astrophysical parameter
with definite implications for cosmology. In particular, a simple
relation is proposed to link Hubble's constant H0 to the
period P0:dP0/dt = H0P0 =
1.9.10-14. The corresponding lifetime of the 160m
period is found to be ≡16.109yr, i.e., equal to the age
of the Universe.
Title: The 160-minute period, internal rotation, and 11-year solar
cycle: are they related?
Authors: Kotov, V. A.; Levitskii, L. S.
Bibcode: 1987BCrAO..77...56K
Altcode: 1989BCrAO..77...56K
No abstract at ADS
Title: Differential observations of the photospheric brightness
oscillations of the Sun
Authors: Didkovskii, L. V.; Kotov, V. A.
Bibcode: 1987BCrAO..76..132D
Altcode: 1989BCrAO..76..132D
No abstract at ADS
Title: Rotation of the Sun and rotation of its general magnetic field.
Authors: Kotov, V. A.
Bibcode: 1987IzKry..77...39K
Altcode:
The author analysed the measurements of the solar mean magnetic
field (SMMF, 1968 - 1984) and also the time series of polarity
of the interplanetary magnetic field (IMF 1926 - 1983). Power
spectra of both sets show the presence of two dominant
periods of rotation: 26d.94±0d.02 and
28d.20±0d.02 (synodic). The first period is
interpreted as the most coherent period of rotation of the surface
magnetic fields near equator. The other period corresponds to
the highest peak in the IMF power spectrum and does not show any
splittings due to differential rotation and 22-year cycle. It is
conjectured that this 28d.20 period reflects rotation of
a deeply rooted solar magnetic field which penetrates the radiative
zone of the Sun. This tentative conclusion appears to be compatible
with recent helioseismological observations. The author notes that the
28d.20 period corresponds to rotation rate of the photosphere
at heliolatitudes of about 28° where spots usually originate at the
onset of each solar cycle.
Title: The rotation of the Sun and the rotation of its general
magnetic field
Authors: Kotov, V. A.
Bibcode: 1987BCrAO..77...42K
Altcode: 1989BCrAO..77...42K
No abstract at ADS
Title: On the possibility of rapid rotation of the solar core.
Authors: Kotov, V. A.; Kosovichev, A. G.
Bibcode: 1987IzKry..77...72K
Altcode:
The authors discuss a conjecture that the central core of the Sun
rotates plausibly with very short period near 160m. The
rotational splitting of low degree p-modes oscillations was calculated
for the standard solar model, but with the inner core of various size
spinning with the 160m period. The results of calculations
agree with the actual splitting of l = 1, 2 and 3 modes inferred by
Duvall et al. (1984) from observations of 5m-oscillations,
if one assumes that the radius of a rapidly spinning core is less than
0.08 R_sun;. Such small core contains about 6% of the total solar
mass. The resulting gravitational quadrupole moment J2
of the Sun, ⪉4×10-6, does not contradict the results of
observational data on solar oblateness.
Title: The frequency of 10 Hz in the distribution of radiopulsar
periods
Authors: Kotov, V. A.; Vladimirskii, B. M.
Bibcode: 1987BCrAO..76..104K
Altcode: 1989BCrAO..76..104K
No abstract at ADS
Title: The 160 minutes period, internal rotation and 11-year cycle
of the Sun: evidence for a relationship?
Authors: Kotov, V. A.; Levitskii, L. S.
Bibcode: 1987IzKry..77...51K
Altcode:
In order to specify an exact value of the 160m period of
solar oscillations, the authors analyse a sample of about 19,000
chromospheric flares on the Sun as observed by the world network
of solar observatories in 1947 - 1980. For the dominant peak in the
160m range studied the authors obtain the best period's
value of 160m.01015±0m.00008, which is in
excellent agreement with the result of Doppler observations. Some
physical relation between fine structure of the 160m
period and solar cycle might exist. The time sequence of flares
reveals also a strong peak in the 80m range. Discrete
frequencies of 160m oscillations (as seen in solar flares)
may be dependent on detailed structure of the deep solar interior
and therefore may be used to map out the interior rotation rate. It
is also pointed out that the model with a rapidly spinning small core
may reasonably explain the existence of a slower rotation zone inside
the Sun, near 0.3 R_sun;, deduced recently by Duvall et al. (1984)
from helioseismological observations.
Title: The oscillation period of Delta Scuti stars close to 160
minutes
Authors: Kotov, V. A.
Bibcode: 1987BCrAO..76...10K
Altcode: 1989BCrAO..76...10K
No abstract at ADS
Title: The frequency 10 Hz in the distribution of radiopulsar periods.
Authors: Kotov, V. A.; Vladimirskii, B. M.
Bibcode: 1987IzKry..76...93K
Altcode:
A special statistical procedure, based on computation of the so-called
"commensurability spectrum", being applied to the distribution of
periods of 330 pulsars revealed the dominant frequency ν0
= 10.05±0.07 Hz (period 0.0995±0.0007 s) of a quasiperiodic
modulation of the distribution. This modulation means the presence of a
statistically significant, at about 3.3 to 4.1-sigma confidence level,
deficit of a number of PSR with frequencies ν ≈ ν0/n,
where n is integer. The effect appears to be strongly pronounced for
PSR with periods from 0.4 to about 1.6 s and can not be ascribed to
some unknown observational selection effect.
Title: Differential observations of photospheric brightness
oscillations of the Sun.
Authors: Didkovskii, L. V.; Kotov, V. A.
Bibcode: 1987IzKry..76..119D
Altcode:
A photodiode array illuminated by the pin-hole image of the Sun is
used to measure relative (center-to-limb) brightness variations of the
photosphere at 0.82 μm, associated with global oscillations of the
Sun. The observations performed in 1983 and 1984 during 86 days yielded
about 448 hours of data on differential brightness oscillations. These
data were analysed in the frequency range from 55 to 165 μHz (100 to
300 min in period). The power spectra obtained vary significantly from
season to season. The data show the existence of global oscillations
with the well-known 160 min period. The mean brightness amplitude of
the data for this 160-min mode is found to be ≡5×10-5
in units of average solar brightness. It corresponds to ≡(0.2 -
2.0)×10-6 for a harmonic amplitude of the 160-min variations
in the solar irradiance in the 0.82 μm spectral range.
Title: The oscillation period of Delta Scuti stars close to 160
minutes.
Authors: Kotov, V. A.
Bibcode: 1987IzKry..76...10K
Altcode:
The so-called {resonance power spectrum} (or {commensurability
spectrum}) computed for 217 δ Sct stars shows that the dominant (the
most commensurate) period for the total set of oscillation periods of
these stars equals to 162.2±2.8 min. This value coincides fairly well,
within the limits of error, with the famous 160-min period of global
oscillations of the Sun. The finding appears to favour the nonlinear
mechanism of resonant interaction between different modes of stellar
oscillations, with the 160-min period being the most characteristic
(resonant) one.
Title: The 160-minutes period in extragalactic objects: the LMC
(RR Lyr stars) and NGC 4151.
Authors: Kotov, V. A.; Lyuty, V. M.
Bibcode: 1987IzKry..77..148K
Altcode: 1987IKryO..77..148K
According to the finding that the most characteristic ("resonant"
or commensurate) period for the orbital period distribution of close
binaries of the Galaxy and also for RR Lyr variables in globular
clusters is very near to 160 min, the authors computed a so-called
"resonance power spectrum" for the sample of 72 RR Lyr stars observed
in and around the two LMC globular clusters, NGC 2257 and 1786. It
is found that the "resonant" period for these stars, 159.9±1.5 min,
fairly agrees with the previous result. With the aim to extend the
search for traces of this "ubiquitous" 160-min periodicity among
various astrophysical objects, the authors analysed also the UBV
photometric measurements of the nucleus of the Seyfert galaxy NGC
4151, made in the 1968 - 1984 interval. Power spectrum of the data
clearly showed the presence of a significant, at the 4.1-sigma
confidence level, period 160.0099±0.0004 min with about ±2.5%
amplitude. The authors estimate the lifetime of the 160-min period to be
≡15×109years, which is nearly the age of the Universe. The
product P0H0, where H0 is the Hubble
constant, appears to be a dimensionless parameter ≡2×10-14
which might be of great interest for cosmology.
Title: On the possibility of rapid rotation of the solar core
Authors: Kotov, V. A.; Kosovichev, A. G.
Bibcode: 1987BCrAO..77...80K
Altcode: 1989BCrAO..77...80K
No abstract at ADS
Title: The 160-minute period in extragalactic objects: the LMC
(RR Lyr stars) and NGC 4151
Authors: Kotov, V. A.; Lyutyi, V. M.
Bibcode: 1987BCrAO..77..166K
Altcode: 1989BCrAO..77..166K
No abstract at ADS
Title: 160 min solar flare activity modulation.
Authors: Kotov, V. A.; Levitskij, L. S.
Bibcode: 1986BCrAO..75...54K
Altcode: 1987BCrAO..75...54K
No abstract at ADS
Title: Solar oscillations and rotation of close binary systems in
the Galaxy: the 160 minute period.
Authors: Kotov, V. A.
Bibcode: 1986BCrAO..74...65K
Altcode: 1987BCrAO..74...65K
No abstract at ADS
Title: The axial-rotation velocity distribution in the solar system
and the sun's 160-min oscillations.
Authors: Kotov, V. A.
Bibcode: 1986BCrAO..75...83K
Altcode: 1987BCrAO..75...83K; 1986BuCri..75...83K
No abstract at ADS
Title: Observations of 5-minute oscillations in the brightness of
the solar photosphere.
Authors: Didkovskij, L. V.; Kotov, V. A.
Bibcode: 1986BCrAO..74..123D
Altcode: 1987BCrAO..74..123D
No abstract at ADS
Title: The 160 min period in RR Lyr stars in globular clusters and
highly evolved close binary systems.
Authors: Kotov, V. A.
Bibcode: 1986BCrAO..75..104K
Altcode: 1987BCrAO..75..104K
No abstract at ADS
Title: Solar oscillations and the rotation of close binary systems
in the Galaxy - The 160-min period
Authors: Kotov, V. A.
Bibcode: 1986IzKry..74...69K
Altcode:
The previous conclusion that the 160m period of the global
oscillations of the sun might be related to the external 160m
gravitational wave from an unknown source is checked by statistical
analysis of the period distribution of close binary stars. It is
found that the observed distribution of about 4000 binaries shows a
significant (3.5 σ confidence) lack of periods ≡2mzmP0
and an excess (2.5 σ confidence) of periods ≡(2mz+1)mP0,
where z is integer and P0 = 160m. The overall
significance of this 160m effect is about 4.1 σ. A
precise determination of the characteristic period leads to the value
160m.0±0m.1 which is in fair agreement with the
solar oscillation period 160m.0101±0m.0007. A
similar analysis of the distribution of 97 catalysmic binaries
shows that the same frequency, P0-1, is
characteristic for these objects. It is conjectured that the frequency
P0-1 = 104.160 μHz in the distribution of orbital
rates of the galactic binaries is a consequence of the 160m
gravitational radiation which might be cosmological (relict) by nature.
Title: Observations of 5-minute oscillations of solar photospheric
brightness
Authors: Didkovskii, L. V.; Kotov, V. A.
Bibcode: 1986IzKry..74..132D
Altcode:
The results of ground-based observations of temporal variations of
the solar brightness at 0.82±0.13 μm are presented. The authors
find a statistically significant enhancement of the spectral power for
frequencies between 2.6 and 3.4 mHz. These variations are attributed to
global p-mode for solar intensity oscillations because 5-minute peaks
in the power spectrum reveal a discrete pattern with the well-known
equidistant spacing of 68 microHz. The frequencies agree well with the
values of 5-minute oscillations obtained from the total solar irradiance
measurements made on board the SMM satellite. Five minute oscillations
are seen in both "direct" (for the central area of the solar disk) and
"differential" (center-to-limb) brightness signals and are thought to
be associated with acoustic compression waves in the photosphere.
Title: The 160 min-period with regard to the frequency of occurrence
of chromospheric flares.
Authors: Kotov, V. A.; Levitskij, L. S.
Bibcode: 1986psf..conf..112K
Altcode:
No abstract at ADS
Title: Period of 160 minutes of RR Lyr variables in globular clusters
and highly evolved close binary systems.
Authors: Kotov, V. A.
Bibcode: 1986IzKry..75..113K
Altcode:
A statistical analysis based on computation of so-called
"commensurability spectra" is applied to periods of 1211 RR Lyr
variables in globular clusters and to a sample of highly evolved close
binaries with orbital periods less than 4 days. It is shown that for
the frequency range studied (from about 35 to 150 μHz) the period
of 160 min appears to be the most characteristic one, with respect
to commensurability, for both period distributions. The effect is
found to be significant at about 3.8 and 3.2σ levels of confidence
for RR Lyr variables and close binary systems correspondingly. It is
suggested that this particular status of the 160-min period, at first
discovered in the solar oscillations, then in galactic binary stars,
and which seems to be of "universal" character, might reflect some
unknown property of gravitational interaction.
Title: Modulation of the flare activity of the sun with a 160
minute period.
Authors: Kotov, V. A.; Levitskii, L. S.
Bibcode: 1986IzKry..75...59K
Altcode:
The authors subjected to a statistical analysis the complete set
of times of beginnings of chromospheric flares of importance B ≥
1 observed on the sun during 1955 - 1980 (about 16200 flares in
total). A high-resolution "power spectrum" of the time series was
calculated for a range near the 160.0-min period using the superposed
epoch technique and the χ2-criterion. It showed only
two significant (⪆99.9% confidence) peaks corresponding to periods
160.0056±2 and 160.0100±2 (min). It is supposed that the 160-min
global oscillations of the sun trigger, statistically, occurrences of
flares. A peak-to-peak amplitude of this 160-min effect is found to
be about 12% with respect to the statistical mean value which would be
expected in a random sample. It is noted that the spacing between the
frequencies of those two dominant peaks corresponds fairly well to the
11-year period. Nevertheless, some arguments are given in favour of a
real (i.e. not arisen merely from 11-year modulation) nature of the
duplicate structure of the 160-min period in solar flares. The same
seems to be true for Doppler observations of solar oscillations. This,
in turn, may lead to interesting conjectures on a possible physical
association between 160-min oscillations and the solar 11-year cycle.
Title: Spin rates distribution in the solar system and 160 minute
oscillations of the sun.
Authors: Kotov, V. A.
Bibcode: 1986IzKry..75...90K
Altcode:
The previous analysis and results as regards the effect of a preferable
commensurability of the spin rates (of planets and asteroids) with
the 160-min period is now extended to a much more complete data set
comprising 239 different bodies in the solar system: 223 asteroids
with diameters D ≥ 30 km, 6 planets and 10 nuclei of short-period
comets. It is found that for the frequency range studied (from about
30 to 200 μHz) there is a unique period, 160 min, which shows the
highest degree of overall commensurability with the entire sample of
spin rates. The statistical significance of the result is estimated
to be near 3.4σ to 5.8σ depending on one or another statistical
hypothesis. A preliminary conclusion is made that the apparent
"universal" behaviour of the 160-min periodicity can be classified,
perhaps, as some property of the gravitational field.
Title: The 160-MINUTES Oscillations
Authors: Kotov, V. A.
Bibcode: 1985SoPh..100..101K
Altcode:
We describe basic observational data regarding the 160-min oscillations
of the Sun as well as the implications for helioseismology. The
most acceptable theoretical interpretation seems to be a resonant
interaction of gravity g-mode oscillations of the solar model with
a slight modification to the equilibrium structure (with low heavy
element abundance).
Title: On the problem of magnetic field asymmetry of the Sun:
anomalous interplanetary magnetic field in 1970 - 1981.
Authors: Kotov, V. A.; Levitskii, L. S.
Bibcode: 1985IzKry..71...32K
Altcode:
Published data on solar magnetic asymmetry are reviewed, and it is
shown that polar asymmetry is a characteristic feature of the solar
magnetic field. Data on the daily AC-index of the IMF polarity
(collected between 1926 and 1982) were studied by means of power
spectrum analysis and the superposed epoch method. It is found that
the annual variation in polarity shows a significant phase shift with
respect to the change in the earth's heliolatitude in the course of a
year. Contrary to the 1930-1969 time interval, when in each 10-year
solar cycle the 1-year periodicity dominated the power spectra, the
1970-1981 time interval was anomalous; in the most recent solar cycle,
0.8- and 1.5-year periods dominated the power spectrum. This anomaly is
believed to be caused by changes in solar magnetic asymmetry over time.
Title: On a possible relation of the law of planetary distances to
the 160-minute pulsation of the sun.
Authors: Kotov, V. A.; Koutchmy, S.
Bibcode: 1985IzKry..72..199K
Altcode:
The discovery of the global solar pulsation with the period of
P0 = 160m enables to introduce characteristic
wavelength L = c×P0 = 19.24 A.U. for the solar system,
where c is the speed of light. A corresponding analysis of planetary
distances reveals the existence of a statistically significant
quasi-commensurability between L and 2πai for inner planets
and between 2ai and L for outer ones (ai being
the major semi-axis of a planetary orbit). It is suggested that this
L-commensurability can offer new approach to an explanation of the
well-known Titius-Bode law for planetary distances. The physical
mechanism enforcing the L-commensurability in the solar system is
presumably related with 160m-gravitational waves from some
external source of unknown nature.
Title: The 160-min period in the solar system: solar pulsation and
the spin rates of planets and asteroids
Authors: Kotov, V. A.; Koutchmy, S.
Bibcode: 1985BCrAO..70...37K
Altcode: 1985BuCri..70...37K; 1987BCrAO..70...37K
No abstract at ADS
Title: Solar oscillations with a 160-min period and other long period
solar oscillations: analysis of the power spectrum of nine-year
observations and their interpretation
Authors: Severnyi, A. B.; Kotov, V. A.; Tsap, T. T.
Bibcode: 1985BCrAO..71....1S
Altcode: 1985BCrAO..71....3S
No abstract at ADS
Title: A possible relation between planetary distances and the
160-minute solar pulsation.
Authors: Kotov, V. A.; Koutchmy, S.
Bibcode: 1985BCrAO..72..171K
Altcode: 1985BuCri..72..171K; 1987BCrAO..72..171K
No abstract at ADS
Title: The search for a 160-min period in sequences of X-ray bursts
and chromospheric flares of the sun
Authors: Kasinskii, V. V.; Kotov, V. A.; Levitskii, L. S.; Fomin, V. P.
Bibcode: 1985IzKry..73...43K
Altcode:
Statistical analysis of 533 hard X-ray bursts of the sun, recorded by
the Japanese satellite Hinotori in 1981 in the 17-40 keV range, reveals
a 160-min modulation with a confidence level of 98 percent. This finding
is confirmed by SMM satellite data where an analogous periodicity is
found at a 93 percent confidence level. The superposed epoch method,
applied to the time sequence of 16,000 solar flares with importance
B greater than or equal to 1 also reveals a 160-min modulation
with a 99 percent level of confidence. It is proposed that the
chromospheric perturbation induced by the global 160-min oscillations
can statistically trigger the occurrence of solar flares. However, this
effect is nearly insignificant (85 percent confidence) in the case of
strong (importance B greater than or equal to 2) flares, but highly
significant (99.9 percent) in the case of weak (B = 1) flares. The
peak amplitude of modulation of flare occurrences is about 7 percent.
Title: Period of 160 minutes in the solar system: solar pulsation
and spin rates of planets and asteroids.
Authors: Kovtchmy, S.; Kotov, V. A.
Bibcode: 1985IzKry..70...38K
Altcode:
It is proposed that the close correspondence between the period of
solar global pulsation (160 min) and the 9th and 4th harmonics of
the rotational periods of the earth and Saturn respectively cannot
be fortuitous. To test this hypothesis, a commensurability function
is examined, and the level of statistical certainty of the result is
determined. An analysis of commensurability with the period of solar
global pulsation was extended to all available data on the rotation of
planets and asteroids, and it is shown that quasi-commensurability with
this 160-min period is both dominant and statistically significant. The
probability of randomly obtaining such a quasi-commensurability is
equal to about 0.00001. On these grounds, it is proposed that there is
(or was in the past) some gravitational coupling between those main
bodies of the solar system having a 160-min period; this process could
have resulted from a periodic variation of the gravitational field.
Title: A search for the 160-min period in sequences of solar X-ray
bursts and chromospheric flares.
Authors: Kotov, V. A.; Kasinskij, V. V.; Levitskij, L. S.; Fomin, V. P.
Bibcode: 1985BCrAO..73...40K
Altcode: 1987BCrAO..73...40K
No abstract at ADS
Title: Global solar oscillations observed from relative near-IR
photosphericbrightness fluctuations.
Authors: Kotov, V. A.; Koutchmy, S.; Kononovich, Eh. V.; Ryzhikova,
N. N.; Tsap, T. T.
Bibcode: 1985BCrAO..73...24K
Altcode: 1987BCrAO..73...24K
No abstract at ADS
Title: Solar oscillations with a period of 160 min and other
long-period oscillations - Analysis of the power spectrum during
nine years of observations and interpretation
Authors: Severnyi, A. B.; Kotov, V. A.; Tsap, T. T.
Bibcode: 1985IzKry..71....3S
Altcode:
Doppler-velocity observations are used to investigate the power spectrum
of solar oscillations in the 110-210-min periodicity range. In order
to eliminate all power peaks of nonsolar origin, the present spectrum
is compared with an analogous power spectrum computed on the basis
of simultaneous telluric O2 6879-A line observations. This comparison
reveals that 39 of the peaks may indeed have their origin in the sun;
20 of these were compared with the theoretical periods of 'dirty' solar
models (Christensen-Dalsgaard et al., 1979) whereby enrichment with
heavy elements via accretion from interstellar space has occurred. Ten
of the observed periods agree well with the periods of g-modes. One
variation of the 'dirty' solar model (C) is characterized by a shallow
convective zone and a low neutrino flux of 1.7 SNU.
Title: Unbalance in the Sun's general magnetic field: anomalies in
the interplanetary magnetic field in 1970-1981
Authors: Kotov, V. A.; Levitskii, L. S.
Bibcode: 1985BCrAO..71...31K
Altcode: 1985BuCri..71...31K
No abstract at ADS
Title: Global oscillations of the sun according to observations of
(relative) fluctuations of photospheric brightness in the near
infrared
Authors: Koutchmy, S.; Kononovich, E. V.; Ryzhikova, N. N.; Kotov,
V. A.; Tsap, T. T.
Bibcode: 1985IzKry..73...26K
Altcode:
The instrument designed for monitoring of relative center-to-limb
brightness fluctuations of the photosphere in near IR spectral range (λ
= 1.65 μm) is described. Analysis of 67 days of observations carried
out in 1981 - 1982 shows clearly the presence of 160-min variations of
the differential, center-to-limb intensity with an average amplitude
of about 3×10-5 in units of the {average solar} brightness
near 1.65 μm or 0.2K in terms of the temperature of the photosphere.
Title: Ten years observations of long-period oscillations of the Sun
Authors: Kotov, V. A.; Severny, A. B.; Tsap, T. T.
Bibcode: 1984ESASP.220..189K
Altcode: 1984ESPM....4..189K
The measurements of Doppler shift of a Fraunhofer spectral line were
performed over 10 yr. The power spectrum of the data shows a major peak
at 160m period which is interpreted as multiple resonance of gravity
modes of the Sun. This 160m oscillation reveals remarkable phase
stability during the entire decade. It is noted that true pattern
of the power spectrum can be seriously spoiled by Earth sources of
noise. The importance of analysis of oscillations seen in a telluric
line is emphasized.
Title: 160-minute and other long-period oscillations of the sun
Analysis and interpretation of 9-year observations
Authors: Kotov, V. A.; Severnyi, A. B.; Tsap, T. T.
Bibcode: 1984MmSAI..55..117K
Altcode:
Besides the persistent 160-min oscillation Crimean observations show
the presence of 10 or more other long-period oscillations interpreted
as gravity g-modes.
Title: On Commensurability of the Axial Periods of Cometary Nuclei
Rotation with the 160-MINUTE Period
Authors: Kotov, V. A.; Tarashchuk, V. P.
Bibcode: 1984ATsir1318....1K
Altcode:
No abstract at ADS
Title: The 160-min pulsation period in the SMM solar hard X-ray
burst data
Authors: Kasinskij, V. V.; Kotov, V. A.
Bibcode: 1984PAZh...10..235K
Altcode:
Data on 2100 25-350-keV solar X-ray bursts obtained by the
hard-X-ray-burst spectrometer of the SMM satellite (Wagner, 1982)
over its entire period of operation in 1980-1981 and 400 1-min
SMM observations of the 3.2-A line of Ca XIX on June 24-28, 1980,
are analyzed statistically in terms of possible effects of the
160.010-min solar pulsations reported by Severnyi et al. (1976) and
Kotov et al. (1983). The power spectrum of the Ca XIX measurements
is calculated and plotted, and the superposed-epochs technique is
applied to the burst observations. Both sets of data are shown to
found to exhibit intensity modulations with the 160-min period; the
significance of the burst periodicity is determined as about 0.001.
Title: The 160-MINUTE Pulsation Period in the Solar Maximum Mission
Solar Hard X-Ray Burst Data
Authors: Kasinski, V. V.; Kotov, V. A.
Bibcode: 1984SvAL...10...98K
Altcode:
No abstract at ADS
Title: Periodic variations in the solar magnetic field?
Authors: Kotov, V. A.; Levitskii, L. S.
Bibcode: 1984BCrAO..69...84K
Altcode: 1986BCrAO..69...84K
No abstract at ADS
Title: Periodic variations of the solar magnetic field
Authors: Kotov, V. A.; Levitskii, L. S.
Bibcode: 1984IzKry..69...90K
Altcode:
Dominant recurrent periods - or rotation periods - of the mean
solar magnetic field have been studied using the polarity of the
interplanetary magnetic field (IMF, 1926 - 1981) as inferred from polar
geomagnetic observations and direct measurements of the magnetic field
of the sun seen as a star (1968 - 1981). The power spectra of these data
reveal a set of discrete lines associated with 27 - 29 days (synodic)
periods of the solar rotation. The most prominent peaks, in particular
those at 26.95, 27.20, 27.38 and 28.21 days periods, exhibit remarkable
phase-coherency over 56 years. It is suggested that these discrete lines
(periods) belong to certain latitudinal zones on the sun where the
magnetic field rotates coherently and almost independently (in regard
to the phase) of the 11-years cycle and of the polar field reversals
occurring near epochs of the solar activity maxima. In addition, the
present analysis of 56 years of the IMF polarity shows the existence
of a strong annual variation which appears to be, in the main part,
a by-product of the well-known Rosenberg-Coleman's effect in the IMF
predominant polarity.
Title: Power spectrum of long-period solar oscillations and 160-min
pulsations during 1974-82
Authors: Severnyi, A. B.; Kotov, V. A.; Tsap, T. T.
Bibcode: 1984Natur.307..247S
Altcode:
We report here the results of solar oscillation observations carried
out between 1974 and 1982 using the Crimean solar magnetograph. We
have eliminated all peaks of telluric origin from the mean power
spectrum; of the remaining 32 dominant (>=2σ) peaks, 19 are
of solar origin and 13 are partly blended with the atmospheric
peaks. We found that 10 solar peaks are in very good agreement with
the modes g10-g20 of degree 1 = 4 calculated by
Christensen-Dalsgaard et al.1 for the solar model C with
the envelope enriched in heavy elements by accretion. Deviations of the
observed long-period oscillations from a linearity can be appreciable,
leading to the appearance of combination frequencies. The dominant
160-min peak seems to be excited by a strong `double' resonance
of 2g8 mode of model C with a combination frequency,
and two other combination frequencies of modes 1g1 and
2f including the unstable mode l = 1. As model C is also in good
agreement with the neutrino experiment, we suggest that this could
be considered as the most appropriate model of the Sun. In contrast
to previous detailed studies of solar pulsation with the particular
160.01-min period2,3, the emphasis here is on the search for
other possible long-period solar oscillations of low degree. These
oscillations are thought to be bound to the regions beneath the
convection zone and penetrate to the Sun's core which makes them
a powerful tool for analysing the solar internal structure and the
evolution of the Sun.
Title: A review of the present state of gravity modes oscillations
of the sun
Authors: Severnyi, A. B.; Kotov, V. A.
Bibcode: 1984AdSpR...4h.129S
Altcode: 1984AdSpR...4..129S
Short review of ground-based observations of the Sun and of solar
gravity modes detection is presented with the emphasize on 160m
oscillation as predominant, long-time phase-coherent oscillation. The
limitations imposed by the influence of Earth's atmosphere and
geoseismic waves on observations of solar oscillations are pointed out
together with a necessity of the observations of solar oscillations
with the aid of space-probes.
Title: Measurements of the solar 160 min oscillation at the Metsaehovi
radio research station in 1980-1982 and comparison with the results
at the Crimean Astrophysical Observatory
Authors: Urpo, S.; Teraesranta, H.; Holsti, N.; Tiuri, M.; Kotov,
V.; Nesterov, N.
Bibcode: 1983STIN...8419268U
Altcode:
The results of solar 160 min oscillation measurements at 8 mm and 13.5
mm wavelengths are compared with optical and radio observations. Results
confirm the existence of this oscillation also at radio frequencies.
Title: Simultaneous registration of the 160-min pulsations of the
sun with two radio telescopes.
Authors: Nesterov, N. S.; Urpo, S.; Kotov, V. A.
Bibcode: 1983PAZh....9..312N
Altcode:
Observations of the center-limb differential solar brightness
obtained at 13.5 mm (using the 22-m radio telescope at the Crimean
Astrophysical Observatory) and at 8.15 mm (using the 13.7-m radio
telescope at Helsinki University) on June 22, 1981, are presented
and compared. An expression for determining the time evolution of
the brightness temperature is derived and applied, and a plot of the
processed data is shown. A 160-min variation is observed in both cases,
with agreement to within 0.05 period. A fourfold difference in amplitude
is attributed either to the wavelength difference or to an imperfect
match of the areas of the sun observed.
Title: The 160-MINUTE Solar Pulsation Recorded Simultaneously by
Two Radio Telescopes
Authors: Nesterov, N. S.; Urpo, S.; Kotov, V. A.
Bibcode: 1983SvAL....9..166N
Altcode:
No abstract at ADS
Title: Observation of global 160-min infrared (differential) intensity
variation of the Sun
Authors: Kotov, V. A.; Koutchmy, S.; Koutchmy, O.
Bibcode: 1983SoPh...82...21K
Altcode: 1983IAUCo..66...21K
The method developed and the instrument designed for detecting
variations of the solar limb darkening at the atmospheric transparency
window of the solar opacity minimum region of λ 1.65 μ are
described. This differential technique proved to be successful in
rejecting undesirable low frequency noises due to the atmosphere
and to the instrument. Analysis of observations made in 1977, 1978,
and 1981 indicates the persistance of global fluctuations of the IR
differential, center-to-limb intensity at the wellknown 160 min period
with an average amplitude of about ± 2 × 10-4 in units
of the `average Sun' intensity near 1.65 μm.
Title: Dominating periods of rotation of the general magnetic field
of the sun.
Authors: Kotov, V. A.; Levitskij, L. S.
Bibcode: 1983ppsf.conf...94K
Altcode:
No abstract at ADS
Title: 160-Minute oscillations in the 13.5 mm circularly polarized
radiation from the Sun
Authors: Efanov, V. A.; Kotov, V. A.; Moiseev, I. G.; Nesterov, N. S.;
Severnyi, A. B.
Bibcode: 1983BCrAO..67...98E
Altcode: 1985BCrAO..67...98E
No abstract at ADS
Title: The discreteness of the rotation periods of the solar and
interplanetary magnetic fields
Authors: Kotov, V. A.; Levitskii, L. S.
Bibcode: 1983IzKry..68...56K
Altcode:
The rotation of solar magnetic fields during 1954-1980 has been
investigated using data sets for the polarity of the interplanetary
magnetic field (IMF) and measurements of the mean magnetic field
of the sun for 1968-1980. Each data set used in the analysis was
treated as a single time series. The power spectra of the fields
show a set of discrete peaks near the solar rotation period of 27-28
days. The most significant peaks were well reproduced in both the IMF
and SMMF spectra. It is shown that neither sampling effects nor the
interference of the 27-28-day variations in the long-term evolution
of the IMF and SMMF can account for the concentration of power in the
discrete lines. The solar magnetic fields at high latitudes (40-50 deg)
appear to contribute significantly to the SMMF as measured by a solar
magnetograph, and to the IMF observed at earth orbit.
Title: A study of the global oscillations of the sun. II - Results
of observations in 1974-1980, their analysis and conclusions
Authors: Kotov, V. A.; Severnyi, A. B.; Tsap, T. T.
Bibcode: 1983IzKry..66....3K
Altcode:
A superposed-epoch analysis of the differential radial velocity of
the sun covering a 7-year period (1974-1980), supported by a power
spectrum analysis, shows the presence of oscillations with a period of
160.01 m and an amplitude of about 0.5 m/s. Four other statistically
significant oscillations (with periods of 134.5, 148.4, 171.1, and
175.1 m) are shown to exist up to 1977. These, however, are thought
to be transient phenomena, whereas the 160.01-m oscillations persist
over the entire 7-year period, with the mean amplitude varying from
year to year. In addition to sporadic fluctuations, the amplitude of
the 160.01-m oscillations exhibits periodic variability with a sun
rotation period of about 27.2 d. The factors supporting the solar
origin of the 160.01-m oscillations are discussed.
Title: Long-term coherent periodicities in the mean magnetic field
of the sun
Authors: Kotov, V. A.; Levitskii, L. S.
Bibcode: 1983IAUS..102...23K
Altcode:
The present investigation is concerned with periodic variations of the
magnetic field of the sun as a star, taking into account mean field
measurements in the Crimea, Mt. Wilson, and Stanford observatories. A
total of 5783 daily values was available for the time interval from 1968
to 1981. The data provide a unique possibility to study the sun as a
variable magnetic star. In connection with the objective to combine the
three data sets into a single time series, the original measurements of
each observatory were corrected for the systematic calibration error,
giving attention to the application of correction factors determined on
the basis of an intercomparison of the three individual power spectra.
Title: A study of solar global oscillations. II. Results of
observations in 1974-1980, their analysis, and some conclusions
Authors: Kotov, V. A.; Severnyi, A. B.; Tsap, T. T.
Bibcode: 1983BCrAO..66....1K
Altcode: 1985BCrAO..66....1K
No abstract at ADS
Title: Discrete solar rotation frequencies deduced from the solar
and interplanetary magnetic fields
Authors: Kotov, V. A.; Levitskii, L. S.
Bibcode: 1983BCrAO..68...50K
Altcode: 1985BCrAO..68...50K
No abstract at ADS
Title: Variations of the interplanetary and solar magnetic fields
Authors: Kotov, V. A.; Levitskii, L. S.
Bibcode: 1983IzKry..66..110K
Altcode: 1983IzKry..66Q.110K
The authors determine time variations of the interplanetary magnetic
field (IMF) observed near the earth and of the mean magnetic field of
the sun seen as a star (SMMF) for 1968-1979. All the values of IMF and
SMMF were 28-day averaged to eliminate the dependence on solar rotation;
also the yearly means were calculated. It is shown that in contrast
to the yearly average magnitude of the IMF which is almost constant
throughout the solar cycle, that of the SMMF changes markedly from year
to year (by 3-4 times). The analysis reinforces the previous conclusion
(1981) on the presence of a significant annual variation in the SMMF
with amplitude of about 0.1 Gs. It is suggested that some asymmetry
of the global magnetic field of the sun in inertial (with respect to
stars) space can be responsible for this annual effect as observed
from the earth. The annual wave in the IMF magnitude is only marginally
significant, ⪉3%, demonstrating once more quite different behaviour of
the IMF and SMMF on a month-year time scale. The discrepancy is thought
mainly to be the result of different averaging of two physical fields.
Title: The 160-min variation of circularly polarized solar radio
emission at a wavelength of 13.5 MM
Authors: Efanov, V. A.; Kotov, V. A.; Moiseev, I. G.; Nesterov, N. S.;
Severnyi, A. B.
Bibcode: 1983IzKry..67..111E
Altcode:
Variations of the circularly polarized radio emission of the sun
with period of 160 min and amplitude of about 2×10-5 are
detected at 13.5 mm wavelength. They exhibit phase-coherence (with
about 34m delay-time) with the global 160-min oscillations
of the sun seen in the velocity of the photosphere and might be related
to synchronous changes of the solar general magnetic field.
Title: Manifestation of the 160-MIN Solar Oscillations in Velocity
and Brightness - Optical and Radio Observations
Authors: Kotov, V. A.; Severnyi, A. B.; Tsap, T. T.; Moiseev, I. G.;
Efanov, V. A.; Nesterov, N. S.
Bibcode: 1983SoPh...82....9K
Altcode: 1983IAUCo..66....9K
All evidence of the solar origin of 160-min period oscillations is
collected, and the present state of observations of this oscillation in
optical and radio-ranges is considered. The main results are summarized:
(a) the 160-min oscillation was observed in 1981 as well as before,
(b) an attempt to find a nonradial component with l = 2 has failed,
(c) the intensity and circular polarization of radioemission show with
statistical significance the presence of this 160-min periodicity.
Title: Time variations of the interplanetary and solar magnetic fields
Authors: Kotov, V. A.; Levitskii, L. S.
Bibcode: 1983BCrAO..66..100K
Altcode: 1985BCrAO..66..100K
No abstract at ADS
Title: Potential Models of the Unipolar Sunspot Magnetic Field
Authors: Denisenko, V. V.; Kotov, V. A.; Romanov, V. A.; Sokolov, V. S.
Bibcode: 1982SoPh...81..217D
Altcode:
The potential models of the unipolar sunspot magnetic field are
calculated on the basis of magnetographic measurements of the magnetic
field made in the three spectral lines of different intensities, Hα,
CaI λ6103 and FeI λ4808. The computed distributions of the magnetic
field vector are compared with actual distributions observed at these
three levels. It is shown that the electric current density in the
spot reaches values up to 105 CGSE in the volume contained
between formation depths of two pairs of lines, FeI λ4808-CaI λ6103
and FeI λ4808 - Hα. Therefore, the magnetic field of the spot
deviates strongly from a potential configuration. To the contrary, at
higher levels, in the semi-infinite volume restricted at the bottom
by the hydrogen Hα-line, the field appears to be quite close to a
potential one.
Title: An investigation of the global oscillations of the sun:
1. Methods and instruments
Authors: Kotov, V. A.; Severnyi, A. B.; Tsap, T. T.
Bibcode: 1982BCrAO..65....1K
Altcode: 1982BuCri..65....1K; 1984BCrAO..65....1K
No abstract at ADS
Title: Study of solar global oscillations. I - Method and instrument
Authors: Kotov, V. A.; Severnyi, A. B.; Tsap, T. T.
Bibcode: 1982IzKry..65....3K
Altcode:
The present investigation is concerned with a method for the
measurement of the Doppler shift of the position of the spectral
line Fe I lambda 5124 A, averaged over the central zone of the solar
disk, with respect to the mean position of the same line for the limb
region. The statistical accuracy of the measurement of the velocity
is approximately + or - 0.2 m/sec. The historical background regarding
the considered measurements is discussed along with the Crimean Solar
Tower Telescope and the magnetograph employed in the measurements,
the study of the sun in a parallel beam, and the method used to measure
the solar global oscillations. Attention is given to questions regarding
the accuracy of the method, errors related to the instrument, aspects of
guidance and stability, possible errors due to the electronics system,
and an evaluation of the effects of the errors on the accuracy of the
results obtained with the aid of the considered method.
Title: Present State of the Study of 160-MINUTES Solar Oscillation
Authors: Severnyi, A. B.; Kotov, V. A.; Tsap, T. T.
Bibcode: 1981SoPh...74...65S
Altcode:
Global oscillation of the Sun with a period of 160 rain were first
discovered in 1974 and since observed in Crimea during the last 6 years;
they were confirmed, in 1976-1979, by Doppler measurements at Stanford
(Scherrer et al., 1980) and quite recently by observations of Fossat
and Grec at the south geographic pole. The average amplitude of the
oscillation is about 0.5 m s-1. The phase shows remarkable
stability at the period 160.010 min and good agreement between different
sites on the Earth; therefore, this oscillation should now be recognized
as definitely of solar origin. It is probably accompanied by synchronous
fluctuations in the IR brightness and radio-emission of the Sun, and
exhibits a dependence of the amplitude on the phase of solar rotation
(with a peak of power at 27.2 days).
Title: Annual variation of the mean magnetic field of the sun
Authors: Kotov, V. A.; Levitskii, L. S.; Stepanyan, N. N.
Bibcode: 1981BCrAO..63....1K
Altcode: 1981BuCri..63....1K
No abstract at ADS
Title: Annual variation of the solar mean magnetic field.
Authors: Kotov, V. A.; Levitskii, L. S.; Stepanian, N. N.
Bibcode: 1981IzKry..63....3K
Altcode:
The paper examines observations of the solar mean magnetic field
(SMMF) made during 1968-1978 at the Crimean, Mt. Wilson, and Stanford
observatories. An analysis of the data clearly shows an annual variation
of the SMMF with an amplitude of about 0.1 G, and it is argued that
this periodicity can be attributed neither to instrumental nor to
seasonal causes. It is noted that the heliolatitude effect cannot
be used to explain this periodicity, and that there are unexplained
phase differences between annual variations of the SMMF and the sun's
polar field. The nature of the annual variation of the SMMF is left
unresolved.
Title: Global Oscillations of the Sun
Authors: Severny, A. B.; Kotov, V. A.; Tsap, T. T.
Bibcode: 1981IGAFS..56...11S
Altcode:
No abstract at ADS
Title: Detection of 160 min solar intensity variations: sampling
effects.
Authors: Koutchmy, S.; Koutchmy, O.; Kotov, V. A.
Bibcode: 1980A&A....90..372K
Altcode:
The theory that the 2 h 40 min period in the Crimean and Stanford
global solar velocity oscillation measurements may have resulted
partly by 1-day sampling is verified using the IR center-limb
intensity variations measurements. It was shown that (1) the power
spectrum of these data has a peak near the 2 h 40 min period, and (2)
the power spectra of the series with the observing windows 'filled'
with a constant do not manifest a significant peak at the 9th harmonic
of the day. It was concluded that the analysis of the really observed
data is not biased by the influence of data windows and 1-day sampling
regularity of observations.
Title: Detection of 160-min solar oscillations and atmospheric
extinction
Authors: Severnyi, A. B.; Kotov, V. A.; Tsap, T. T.
Bibcode: 1980A&A....88..317S
Altcode:
The influence of the earth's atmosphere on the search for global solar
oscillations with a period of 160m is studied. It is shown that neither
the amplitude nor the phase behavior of the oscillations persisting
during the last five years (1974-1978) can be explained in terms of
the terrestrial atmospheric influences or by the statistical method
of treatment. The observational evidence strongly suggests that the
160m periodicity is of solar origin.
Title: Further evidence of solar oscillations with a period of
160 minutes
Authors: Scherrer, P. H.; Wilcox, J. M.; Severnyi, A. B.; Kotov,
V. A.; Tsap, T. T.
Bibcode: 1980ApJ...237L..97S
Altcode:
Observations made at the Crimean Astrophysical Observatory and the
Stanford Solar Observatory during 1979 provide evidence of the existence
of oscillations of the sun with a period near 160 minutes. The new
observations showed the same period with a phase of maximum expansion
as predicted from earlier data; for 1979 the time of maximum expansion
of the center of the solar disk was found to be 01:55 UT for the Crimean
observatories and 01:58 UT for Stanford with a phase uncertainty of plus
or minus 15 minutes. In addition, a new regression line can be found
which yields a period of 160.01 minutes or a drift in phase of 31.5
minutes per year in an analysis at exactly 160 minutes. The continued
agreement in phase (and amplitude) between the two observatories
for four years, as well as the fact that the period of oscillations
determined differs from exactly one-ninth of a day, supports the
interpretation that solar oscillations are indeed being observed.
Title: The Effect of the Equation of Time on the 160-MINUTE Solar
0SCILLATION
Authors: Kotov, V. A.; Koutchmy, S.; Severnyi, A. B.; Tsap, T. T.
Bibcode: 1980SvAL....6..233K
Altcode:
No abstract at ADS
Title: Certain characterisitics of the large-scale magnetic fields
of the Sun
Authors: Kotov, V. A.; Stepanyan, N. N.
Bibcode: 1980BCrAO..62...96K
Altcode: 1980BuCri..62...96K
No abstract at ADS
Title: Solar pulsations.
Authors: Severnyi, A. B.; Kotov, V. A.; Tsap, T. T.
Bibcode: 1980HiA.....5..453S
Altcode:
Observations of solar oscillations with a period of approximately 160
min are discussed. The oscillations were detected independently in 1974,
1976, 1978 and 1979, with a high phase coherence between observation
times. The amplitude of the oscillations is found to depend on the
phase of solar rotation, and a slow drift of the phase of maximum
is observed, leading to an estimate of a period of 160.010 min. The
period may be interpreted by a variety of pulsation modes while the
spherical harmonic l is not known, however the observed dependence of
oscillation amplitude on solar rotation phase can be accounted for by
the rotational splitting of the S1(m) mode at l = 2. The oscillations
have also been observed to disappear and reappear with nearly the same
phase, and may offer the possibility of a means of energy transport
other than radiative.
Title: Certain characteristics of large-scale magnetic fields on
the sun
Authors: Kotov, V. A.; Stepanian, N. N.
Bibcode: 1980IzKry..62..117K
Altcode:
The characteristics are obtained by comparing the sun's general
magnetic field, measured with a magnetograph, with the background field,
determined on the basis of H-alpha maps. The average intensity of the
magnetic field in the photosphere is found to be approximately 2.2
gauss. The intensity in the regions occupied by the S field is somewhat
greater than in the regions of the N field. During the years 1973-1976,
the primary period for the rotation of the large-scale fields was
approximately 27.04-27.15 d; in 1976-1978, two period were observed,
26.75 d and 29.30 d. This is seen as the result of a shift toward the
equator of the large-scale structures of the magnetic field of the
old 11-year cycle and the formation of the high-latitude structures
of a new cycle. It is also found that the background field in the N
hemisphere, on the average, is positive (approximately +0.14 gauss),
whereas in the S hemisphere it is negative (approximately -0.14
gauss). In the southern hemisphere, the magnetic structures are found
to rotate somewhat faster than in the northern hemisphere. It is noted
that this would be the case if the structures in the S hemisphere were
closer to the equator than in the N hemisphere.
Title: The magnetic field of the Sun as a star, 1969-1976
Authors: Kotov, V. A.; Demidov, M. L.
Bibcode: 1980BCrAO..61....1K
Altcode:
No abstract at ADS
Title: Shaking Down the Sun's Long-Period Vibes
Authors: Kotov, V. A.; Severny, A. B.; Tsap, T. T.; Scherrer, P. H.;
Wilcox, J. M.; Fossat, E.; Grec, G.; Pomerantz, M.
Bibcode: 1980SciN..118..100K
Altcode:
No abstract at ADS
Title: The magnetic field of the sun as a star, 1969-1976
Authors: Kotov, V. A.; Demidov, M. L.
Bibcode: 1980IzKry..61....3K
Altcode:
A superposed epoch analysis of the mean solar magnetic field measured in
the Crimea during 1969-1976 was performed using approximately 215 sector
boundaries of the interplanetary magnetic field. The mean field displays
a sector structure, with a typical field strength within a sector of
0.4-0.3 G. The average magnitude of the mean field decreased from 0.5
G in 1969-1970 to 0.15 G in 1975-1976. The principal recurrence period
in the data is 27.04 d + or - 0.06 d. The resulting curve reflects
the asymmetry between magnetic fields of opposite sign (the duration
of S polarity is 3-4 days greater than that of the N polarity).
Title: Solar oscillations and the problem of the internal structure
of the sun
Authors: Severnyi, A. B.; Kotov, V. A.; Tsap, T. T.
Bibcode: 1979SvA....23..641S
Altcode: 1980SvA....23..641S
No abstract at ADS
Title: Solar oscillations and the problem of the internal structure
of the sun
Authors: Severny, A. B.; Kotov, V. A.; Tsap, T. T.
Bibcode: 1979AZh....56.1137S
Altcode:
Observations of solar oscillations made over a period of five years
are reviewed, and implications of the observations for the physics
of the solar interior are indicated. An analysis of over 1000 hours
of solar observations from 1974 to 1978 is presented which shows the
observed oscillations of the solar radius to be real, with a period of
160.010 + or - 0.004 min and a Doppler shift amplitude of 1 m/sec. The
slow drift of the phase of the velocity maximum has been observed,
together with the dependence of the amplitude on the phase of the
solar rotation period. Synchronous oscillations of the solar magnetic
field and radio emission have also been found to be synchronous to
the brightness oscillations, and the oscillations have been seen to
disappear occasionally, possibly due to the passage of a supergranule
across the solar disk. It is suggested that the oscillations represent
gravitational quadrupole oscillations, and could serve as a means for
nonradiative heat transfer from within the sun and thus alleviate the
problem of low neutrino flux.
Title: Solar radio pulsations of 160-min period observed at 1.9-3.5 CM
Authors: Eryushev, N. N.; Kotov, V. A.; Severnyij, A. B.; Tsvetkov,
L. I.
Bibcode: 1979PAZh....5..546E
Altcode:
Centimeter-wavelength measurements of solar radio emission with
the 22-m Crimean radio telescope during 1977-1978 have revealed
fluctuations in the relative (center/limb) radio brightness with a
160-min period and an amplitude of approximately 0.001. They correspond
to brightness-temperature variations of plus or minus approximately
10 K and are synchronized with the 160-min global pulsations of the
solar surface.
Title: Solar Radio Pulsations of 160-MIN Period Observed at 1.9-CM
and 3.5-CM
Authors: Eryushev, N. N.; Kotov, V. A.; Severnyi, A. B.; Tsvetkov,
L. I.
Bibcode: 1979SvAL....5..292E
Altcode:
No abstract at ADS
Title: Observations of solar oscillations with periods of 160 minutes
Authors: Scherrer, P. H.; Wilcox, J. M.; Kotov, V. A.; Severny, A. B.;
Tsap, T. T.
Bibcode: 1979Natur.277..635S
Altcode:
Severny et al. (1976) have reported oscillations of the sun with
a period near 160 min. A description is presented of observations
made at the Stanford Solar Observatory during the time from 1975 to
the present which seem to support the reports by Severny et al. At
Stanford the relative velocity between a central circular area of
radius 0.5 solar radius on the solar disk and most of the remaining
area of the solar disk is measured. A superposed epoch analysis of
the observations using a period of 160 min is discussed. An apparent
agreement in phase between the obtained observational data and those
reported by Severny et al. tends to support the interpretation that
solar oscillations are being observed.
Title: Observations of oscillations of the Sun.
Authors: Kotov, V. A.; Severnyi, A. B.; Tsap, T. T.
Bibcode: 1978MNRAS.183...61K
Altcode:
Evidence is presented which shows that a previously observed 160-min
oscillation in the solar surface and certain other periodic oscillations
that have persisted for three years are of intrinsic solar origin and
cannot be ascribed to any possible sources of error in observations or
measurements. A method is described which involves measurement of the
relative Doppler shift between a spectral line from the whole central
portion of the solar disk and the same line produced by the whole outer
rim of the disk. Results are discussed for applications of this method
to the magnetically insensitive line of Fe I at 5123.7 A. Various
analyses of the data obtained are performed, possible sources of
systematic error are eliminated, and it is demonstrated that significant
periods of solar oscillation exist, the most significant being 160
min. Attempts made to detect oscillations in mean solar magnetic fields
and brightness as well as in the brightness of Uranus are noted.
Title: Further Progress in Observations of Solar Oscillations
Authors: Severny, A. B.; Kotov, V. A.; Tsap, T. T.
Bibcode: 1978pfsl.conf..123S
Altcode: 1978ESPM....2..123S
No abstract at ADS
Title: Measurements of the solar limb-darkening in the 1 - 4 µm
range.
Authors: Koutchmy, S.; Koutchmy, O.; Kotov, V.
Bibcode: 1977A&A....59..189K
Altcode:
Radial scans in selected spectral regions near the opacity minimum,
in both equatorial and polar directions, have been performed for the
purpose of obtaining improved values for the limb darkening of the very
undisturbed quiet solar atmosphere. Equipment and correction procedures
are described. The new data are compared with earlier values, and the
HSRA model is found to be inadequate for predicting values near the
opacity minimum. The data are more in accord with the new model M of
Vernazza et al. (1976) and also with the BCA model. No pole-equator
difference of limb darkening due to the presence of faint faculae
was found.
Title: The mean magnetic field of the sun: method of observation
and relation to the interplanetary magnetic field.
Authors: Scherrer, P. H.; Wilcox, J. M.; Kotov, V.; Severnyi, A. B.;
Howard, R.
Bibcode: 1977SoPh...52....3S
Altcode:
The mean solar magnetic field as measured in integrated light has
been observed since 1968. Since 1970 it has been observed both at
Hale Observatories and at the Crimean Astrophysical Observatory. The
observing procedures at both observatories and their implications for
mean field measurements are discussed. A comparison of the two sets
of daily observations shows that similar results are obtained at both
observatories. A comparison of the mean field with the interplanetary
magnetic polarity shows that the IMF sector structure has the same
pattern as the mean field polarity.
Title: Polarization of light appearing on mirrors of a tower solar
telescope.
Authors: Kotov, V. A.
Bibcode: 1977IzKry..56..150K
Altcode:
No abstract at ADS
Title: Contribution of the background magnetic field and fields of
active regions and spots to the general magnetic field of the sun.
Authors: Kotov, V. A.; Stepanian, N. N.; Shcherbakova, Z. A.
Bibcode: 1977IzKry..56...75K
Altcode:
No abstract at ADS
Title: Observations of solar pulsations
Authors: Severnyi, A. B.; Kotov, V. A.; Tsap, T. T.
Bibcode: 1976Natur.259...87S
Altcode:
We have modified our solar magnetograph to measure velocities at the
solar surface, rather than magnetic fields. Using this apparatus, we
have observed fluctuations of period 2 h 40 min, which are remarkably
stable. The interpretation of this phenomenon seems to cause much
theoretical difficulty.
Title: The rotation of matter in a sunspot.
Authors: Kotov, V. A.
Bibcode: 1976IzKry..54..184K
Altcode:
Radial velocities in a sunspot are derived from magnetographic
measurements of the Fe I lines at 4808 and 5250 A, the Ca I line at
6103 A, and the H-alpha line. It is found that the gas in the sunspot
rotates in a cyclonic sense at a mean velocity of about 0.25 km/s in
the photosphere and in an anticyclonic sense at a mean velocity of about
-1.3 km/s in the chromosphere, which agrees with the behavior expected
for a sunspot in the southern hemisphere. Measurements of three lines
with different intensities are reported which might indicate a slight
increase in tangential velocity with depth, and the vortex structure
of mass-flow lines and magnetic lines of force is discussed. It is
suggested that the observation of gas rotation in opposite directions
in the photosphere and chromosphere should be taken into account in
a proposed model for the transformation of rotational kinetic energy
into electromagnetic energy of the current system.
Title: Observations of Oscillations of the Entire Sun
Authors: Kotov, V. A.; Severny, A.; Tsap, T.
Bibcode: 1976IAUTB..16..244K
Altcode: 1976IAUT...16B.244K
No abstract at ADS
Title: Enhancement of magnetic fields, radio brightness at
mm-wavelengths and Halpha -activity at the polar regions of the sun.
Authors: Babin, A. N.; Gopasiuk, S. I.; Efanov, V. A.; Kotov, V. A.;
Moiseev, I. G.; Nesterov, N. S.; Tsap, T. T.
Bibcode: 1976IzKry..55....3B
Altcode:
No abstract at ADS
Title: Measurements of the magnetic field from different spectral
lines.
Authors: Gopasyuk, S. I.; Kotov, V. A.; Severnyj, A. B.; Tsap, T. T.
Bibcode: 1975IzKry..53..247G
Altcode:
No abstract at ADS
Title: The interpretation of the total magnetic vector measurements
in sun spots
Authors: Kotov, V. A.
Bibcode: 1974STIN...7527993K
Altcode:
A large change in the magnetic field with depth in the spot was
found on the basis of the total vector (H) measurements at two levels
corresponding to the depths of the line formations lambda 5250 A Fe
and lambda 6103 A Ca. The spiralling of the horizontal field and its
rotation with depth were observed where the vertical field increases
with height. The densities of the vertical and horizontal electric
currents in the spot are equal to approximately 5000 and approximately
100,000 CGSE respectively. The discrepancy between the height gradients
of the vertical field inside the spot was obtained from the measured
vertical field at two levels and from the use of the equation div H =
O. This discrepancy may be attributed to the difference between the very
high resolution at depth and the low resolution on the sun's surface.
Title: An investigation of the transversal magnetic field in sunspots.
Authors: Kotov, V. A.
Bibcode: 1974IzKry..51...39K
Altcode:
The effect of transverse magnetic field rotation with depth is examined
with the aid of sunspot magnetograms obtained in the 4808-A and 5250-A
Fe I lines, the 6103-A Ca I line, and the H-alpha line. The results
show a significant change (45 to 90 deg) in the orientation of the
transverse magnetic field in different sunspot regions. Stronger
rotation was observed in umbrae, but more detailed measurements are
needed to confirm this. The depth behavior of the transverse magnetic
field is analyzed, and it is found that rotation is more pronounced
in the deeply formed 4808-A line than in the others. The 5250-A line
is apparently formed in the uppermost sunspot layers. Observations of
rotation in northern and southern hemispheric sunspots are found not
to contradict the dependence of rotation direction on magnetic field
polarity, which follows from the Zeeman-effect theory with allowance
for anomalous dispersion.
Title: The Comparison of the Magnetographic Magnetic Field Measured
in Different Spectral Lines
Authors: Gopasyuk, S. I.; Kotov, V. A.; Severny, A. B.; Tsap, T. T.
Bibcode: 1973SoPh...31..307G
Altcode:
The discrepancies in the values of longitudinal magnetic field
obtained from magnetographic records in different spectral lines
are considered. On the basis of extensive data including 60 pairs of
magnetographic maps for 11 spectral lines, obtained simultaneously
for one of these lines and λ6103 with the aid of the Crimean double
channel magnetograph, the following conclusions have been reached. The
relative field strength (6103) depends partly on the distance from the
center of the disk (Figure 4) and mainly on the magnetic sensitivity
of the line gλ2 (Figure 3), pointing to the primary role
of saturation effect. The possible influence of line asymmetry on
these discrepancies is also suggested.
Title: On the influence of instrumental polarization on magnetic
field measurements.
Authors: Kotov, V. A.
Bibcode: 1973IzKry..48...78K
Altcode:
No abstract at ADS
Title: On the calibration of photoelectric measurements of a
magnetic field.
Authors: Kotov, V. A.
Bibcode: 1973IzKry..47...14K
Altcode:
No abstract at ADS
Title: Measurements of the Transverse Magnetic Field in the
Chromosphere above a Sunspot.
Authors: Kotov, V. A.
Bibcode: 1972SvA....15..687K
Altcode:
No abstract at ADS
Title: On the interpretation of total magnetic vector measurements
in sunspots.
Authors: Kotov, V. A.
Bibcode: 1972IzKry..46..115K
Altcode:
No abstract at ADS
Title: The systematic errors of the total vector H of magnetic field
measurements with the Crimean Astrophysical Observatory magnetograph.
Authors: Kotov, V. A.
Bibcode: 1972IzKry..44...77K
Altcode:
No abstract at ADS
Title: Measurements of the Transverse Magnetic Field in the
Chromosphere above a Sunspot.
Authors: Kotov, V. A.
Bibcode: 1971AZh....48..869K
Altcode:
No abstract at ADS
Title: Systematic Errors of the Crimean Vector Magnetograph (presented
by a. Severny)
Authors: Kotov, V. A.
Bibcode: 1971IAUS...43...71K
Altcode:
No abstract at ADS
Title: On the Structure of Magnetic Field and Electric Currents of
a Unipolar Sunspot (presented by a. Severny)
Authors: Kotov, V. A.
Bibcode: 1971IAUS...43..212K
Altcode:
No abstract at ADS
Title: A Comparison of Simultaneous Measurements of the Polar Magnetic
Fields Made at the Crimea and Mount Wilson
Authors: Kotov, V. A.; Stenflo, J. O.
Bibcode: 1970SoPh...15..265K
Altcode:
Measurements of the polar magnetic fields of the sun made in August
1968 with the Crimean and Mt Wilson magnetographs are compared. The
agreement between the results obtained at the two observatories is
rather satisfactory. The correlation coefficient between the Crimean
and Mt Wilson values of the observed average field strength at different
latitudes is 0.7 for the north and 0.5 for the south polar region. The
earlier conclusion based on the Mt Wilson material that a polarity
reversal of the field occurred at latitudes +70° and -55° in the north
and south hemispheres (Stenflo, 1970) is confirmed by the Crimean data.
Title: Magnetic field and electric currents of a unipolar sunspot.
Authors: Kotov, V. A.
Bibcode: 1970IzKry..41...67K
Altcode:
No abstract at ADS
Title: The magnetic field of a solar prominence.
Authors: Kotov, V. A.
Bibcode: 1969IzKry..39..276K
Altcode:
No abstract at ADS