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Author name code: frazier
ADS astronomy entries on 2022-09-14
author:"Frazier, Edward N."
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Title: EOS Chemistry spacecraft
Authors: Frazier, Edward N.; Rasmussen, Amy L.
1998SPIE.3498...53F Altcode:
The EOS Chemistry mission is the third of the 'flagship' missions
of NASA's Earth Sciences Enterprise, following EOS AM and EOS
PM. Design work on the Chemistry spacecraft has started under NASA
contract NAS5-32954. This spacecraft is the second of the EOS Common
Spacecraft, EOS PM being the first one. The design has recently been
successfully completed with spacecraft CDR this June, and it is now in
the fabrication phase for the PM mission. This design of the spacecraft
will be summarized. The Chemistry mission will carry four new scientific
instruments. These instruments place some new requirements on the
spacecraft to accommodate them, but these are satisfied with relatively
small 'kits' that are added to the Common Spacecraft design. This
design of the Chemistry configuration of the Common Spacecraft will
be presented. We have explored the cost effectiveness of small and
medium satellite architectures for hypothetical future Earth Science
missions. These cost comparisons include the life cycle cost of space,
launch and ground segments of each complete mission and are based
on actual costs of existing missions. We find that the lowest cost
approach under a wide variety of assumptions is to use a medium size
spacecraft carrying a suite of instruments.
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Title: A self-consistent model of the zodiacal light radiance.
Authors: Frazier, Edward N.; Boucher, Donald J.; Mueller, Gary F.
1987SPIE..819....2F Altcode:
A model of zodiacal light IR radiation is generalized to encompass the
effects of scattered sunlight. The model is compared with existing data
on scattered visible light in order to test compatibility between
IR and visible data, so that both can be explained by a single,
self-consistent model of the interplanetary dust. Both the IR emission
and the visible scattering calculations are based on the Mie equation,
with the optical constants of the interplanetary dust being the input
parameters. The space and size distributions of the dust particles are
explicitly parameterized. The results show that the IR and visible
data are compatible, and can be matched by adjusting the continuous
opacity within reasonable bounds.
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Title: Infrared Radiation of the Zodiacal Light
Authors: Frazier, E. N.
1985SPIE..513..216F Altcode:
No abstract at ADS
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Title: Simulation of the Magnetic Structure of the Inner Heliosphere
by Means of a Non-Spherical Source Surface
Authors: Levine, R. H.; Schulz, M.; Frazier, E. N.
1982SoPh...77..363L Altcode:
In this work we implement a new method for mapping the Sun's magnetic
field B from the photosphere through the corona and interplanetary
space. The method entails the derivation of B from a scalar potential
within a `current-free' annular volume bounded inside by the photosphere
and outside by a prescribed non-spherical `source surface' to which B
is made (as nearly as possible) perpendicular. As usual we obtain the
potential for the part of B that arises from currents inside the Sun
by fitting an expansion to the observed line-of-sight component of B
at the photosphere. The new aspect of our work is that we introduce
a second least-squares fit to obtain the part of B that arises from
currents outside the source surface. We do this by minimizing the
mean-square tangential component of B over the source surface. This
latter prescription allows a nearly arbitrary specification of the
source surface, and no particular symmetry properties need be invoked
for it. We have chosen as our prescription of the source surface
one that reasonably simulates the expected physical consequences
of coronal MHD effects. The magnetic field exterior to the source
surface is made perpendicular to the source surface and is mapped
throughout the heliosphere by means of a geometrical construction that
appropriately generalizes the Parker spiral. Detailed comparisons
have been made between this new model and observed coronal and
interplanetary structures. The equatorward inclination of coronal
helmet streamers is modeled much better with a non-spherical source
surface than with a spherical one. There is clear evidence, however,
that observational data underestimate the strength of photospheric polar
magnetic fields. Neutral lines on the source surface (i.e., contours on
which the normal component of B vanishes) generate heliospheric current
sheets outside the source surface. In the particular case studied, two
separate current sheets existed and were carried by the solar wind from
the source surface to the boundary of the heliosphere. The result was
a four-sector magnetic configuration near the ecliptic at 1 AU, and the
observations were in good agreement with this prediction of the model.
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Title: Simulation of the magnetic structure of the inner heliosphere
by means of non-spherical source surface
Authors: Levine, R. H.; Schulz, M.; Frazier, E. N.
1981STIN...8118977L Altcode:
A new method for mapping the Sun's magnetic field B from the photosphere
through the corona and interplanetary space is presented. The
method entails the derivation of B from a scalar potential within
a current-free annular volume bounded inside by photosphere and
outside by a prescribed nonspherical source surface to which B is
made (as nearly as possible) perpendicular. As usual we obtain the
potential for the part of B that arises from currents inside the Sun
by fitting an expansion to the observed line-of-sight component of
B at the photosphere. A second least-squares fit is introduced to
obtain the part of B that arises from currents outside the source
surface. Comparisons are made between this model and observed coronal
and interplanetary structures. There is evidence that observation data
underestimate the strength of photospheric polar magnetic fields.
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Title: The Non-Spherical Source Surface Magnetic Model: Comparison
with Coronal Data
Authors: Frazier, E. N.; Schulz, M.; Levine, R. H.
1980BAAS...12..544F Altcode:
No abstract at ADS
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Title: The Measurement of Global Scale Surface Dynamics
Authors: Frazier, E. N.
1980NASCP2098..147F Altcode: 1980sscs.nasa..147F
The SCADM mission implicitly contains a requirement for a fundamentally
new type of satellite instrument: a very sensitive (approximately 1
m s/1) imaging velocity detector. This is needed to measure global
oscillations and global circulation patterns, but the sensitivity
requirement is so severe that it has not yet been met even with ground
based instruments. In this presentation, the various possible sources
of noise and other errors in such a device are considered, and the
more detailed instrumental requirements are developed. This leads to
the conceptual design of a velocity graph that appears to achieve the
necessary sensitivity and imaging capability within a resonable weight
and volume.
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Title: Improved Models of Coronal Magnetic Structure: The
Non-Spherical Source Surface
Authors: Levine, R. H.; Schulz, M.; Frazier, E. N.
1979BAAS...11..697L Altcode:
No abstract at ADS
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Title: Magnetic, velocity and brightness structure of solar faculae.
Authors: Frazier, E. N.; Stenflo, J. O.
1978A&A....70..789F Altcode:
To investigate the magnetic, velocity, and brightness structure of solar
magnetic elements in active region plages, the line-ratio technique
of Stenflo (1973) was applied by making simultaneous magnetograph
recordings in the two Fe I lines at 525.0 and 524.7 nm. Not only the
B(525.0)/B(524.7) ratio but also the brightness-magnetic field and
velocity-magnetic field correlations were studied. The center-to-limb
variations of the parameters were also observed. The data were analyzed
in terms of a Milne-Eddington model atmosphere. The cross section of the
magnetic field was found to be narrower than the associated velocity
profile. The continuum contrast at disk center had an amplitude of
as much as 18%, which indicates that the heating starts at relatively
large optical depths, with temperature excess increasing rapidly with
height to account for the strong intensity enhancement in the line
core. With the M-E model, however, it was not possible to obtain
a fully consistent fit with all data at the same time. One needs a
multidimensional, time-dependent non-LTE model for the transfer of
polarized light in rapidly evolving small-scale magnetic geometries
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Title: Coronal magnetic-field model with non-spherical source surface.
Authors: Schulz, M.; Frazier, E. N.; Boucher, D. J., Jr.
1978SoPh...60...83S Altcode:
Previous global models of coronal magnetic fields have used a
geometrical construction based on a spherical source surface
because of requirements for computational speed. As a result
they have had difficulty accounting for (a) the tendency of full
magnetohydrodynamic (MHD) models to predict non-radial plasma flow out
to r ∼ 10r<SUB>⊙</SUB> and (b) the appreciable magnitude, ∼ 3γ,
of B<SUB>r</SUB>, (the radial component of B) consistently observed at r
∼ 1 AU. We present a new modelling technique based on a non-spherical
source surface, which is taken to be an isogauss of the underlying
potential field generated by currents in or below the photosphere. This
modification of the source surface significantly improves the agreement
between the geometrical construction and the MHD solution while
retaining most of the computational ease provided by a spherical source
surface. A detailed comparison between the present source-surface model
and the MHD solution is made for the internal dipole case. The resulting
B field agrees well in magnitude and direction with the coronal B field
derived from the full MHD equations. It shows evidence of the slightly
equatorward meridional plasma flow that is characteristic of the MHD
solution. Moreover, the B field obtained by using our non-spherical
source surface agrees well with that observed by spacecraft in the
vicinity of the Earth's orbit. Applied to a solar dipole field with a
moment of 1 G-r<SUB>⊙</SUB><SUP>3</SUP>, the present model predicts
that B<SUB>r</SUB> at r ∼ 1 AU lies in the range of ∼ 1-2γ and is
remarkably insensitive to heliomagnetic latitude. Our method should be
applicable also to more general (i.e., more realistic) configurations
of the solar magnetic field. Isogauss surfaces for two representative
solar rotations, as calculated from expansions of observed photospheric
magnetic-field data, are found to show large and significant deviations
from sphericity.
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Title: Coronal magnetic-field model with nonspherical source surface
Authors: Schulz, M.; Frazier, E. N.; Boucher, D. J., Jr.
1978aero.reptQ....S Altcode:
Previous global models of coronal magnetic fields have used a
geometrical construction based on a spherical source surface because
of requirements for computational speed. As a result they have had
difficulty accounting for the tendency of full magnetohydrodynamic
(MHD) models to predict non-radial plasma flow out to r about 10
solar radii and the appreciable magnitude, about 3 gamma, of Br (the
radial component of B) consistently observed at r about 1 AU. A new
modelling technique based on a nonspherical source surface is presented,
which is taken to be an isogauss of the underlying potential field
generated by currents in or below the photosphere. This modification
of the source surface significantly improves the agreement between the
geometrical construction and the MHD solution while retaining most of
the computational ease provided by a spherical source surface.
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Title: Line profile families of faculae and pores.
Authors: Frazier, E. N.
1978A&A....64..351F Altcode:
It is pointed out that for any given Fraunhofer line, there should
exist an entire range of facular line profiles. The consequences of
the hypothesis that the structure of faculae and pores is determined
to first order by the total magnetic flux is examined, and therefore,
there should be a one parameter family of line profiles, with the
magnetic flux being that parameter. Observations from a magnetograph
are used to construct this family of line profiles in a statistical
manner. Results are given for the two absorption lines, Fe I 525.022
nm and Fe I 524.706 nm. It is shown that the shape of these profiles
changes continuously from the smallest to the largest faculae,
even including pores. It is concluded that the T(tau) relation in
faculae and pores is a strong function of the total flux, and that a
generalized model of this phenomenon is needed. An additional effect
of this phenomenon is that past observations of facular line profiles
and continuum contrasts have probably been seriously contaminated by
observational selection.
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Title: Infrared radiation of the zodiacal light.
Authors: Frazier, E. N.
1977muit.conf..139F Altcode:
No abstract at ADS
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Title: Line profiles of faculae and pores.
Authors: Frazier, E. N.
1977IAUS...62..255F Altcode:
No abstract at ADS
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Title: The Photosphere - Magnetic and Dynamic State
Authors: Frazier, E. N.
1976RSPTA.281..295F Altcode: 1976RSLPT.281..295F
The photosphere is essentially a relatively thin boundary layer between
two fundamentally different plasma regimes. The solar interior is
characterized by high density, high opacity, high β and convective
instability, whereas the outer solar atmosphere has the opposite
properties. The convection in the interior provides the ultimate
driving force for all of the dynamic and magnetic structure of the
solar atmosphere, yet when we view the photosphere, we can observe
only the upper boundary of the convection zone. Instead, we observe
primarily its various after-effects: overshoot, wave propagation,
and confinement of the magnetic field. These observable phenomena
are described with a view toward diagnosing the essential physics
above and below the photosphere. The convective modes, granulation
and supergranulation, are reviewed briefly; the oscillatory modes are
discussed in somewhat more detail. Finally, the magnetic structure of
the photosphere is described.
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Title: A realistic approach to magnetic evolution.
Authors: Frazier, E. N.
1976SoPh...47..205F Altcode:
An improved scheme for measuring and analyzing the magnetic field of
flares is presented in general outline form. The techniques employed
during the last solar cycle are reviewed very briefly. The point is made
that those techniques were inadequate due to fundamental limitations
in the data. A realistic scheme for acquiring the necessary data is
then proposed. The scheme is realistic in that it makes only those
assumptions which appear to be indeed valid, and it presupposes only
instrumental techniques which are presently available. It is suggested
that, with this improved data, the structure and evolution of the
pre-flare magnetic field can be calculated with sufficient accuracy
to form the basis of theoretical models.
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Title: On the statistical desription of inhomogeneities in the
quiet solar atmosphere. I. Linear regression analysis and absolute
calibration of multichannel observations of the Ca<SUP>+</SUP>
emission network.
Authors: Skumanich, A.; Smythe, C.; Frazier, E. N.
1975ApJ...200..747S Altcode:
Observations with a 2';4 square aperture (1968 epoch) of the Ca
+ K core brightness (1.1 A bandwidth), vertical magnetic field,
vertical velocity, and continuum brightness have been analyzed to yield
average network and nonnetwork values and dispersions as well as linear
regression relations. The statistics of all variables but the continuum
consist of a symmetric core superposed on an extended tail which is
associated with the chromospheric network. Network statistics were
derived by subtraction of a Gaussian fit to the core which was taken
to represent nonnetwork fluctuations. The velocity network was only
partially resolved so that its distribution, and that of the continuum,
was obtained by identifying network regions as those with field >
10 gauss. The average network has a field of 26 gauss, independent
of polarity, a Ca + brightness 1.27 that of the average nonnetwork or
undisturbed chromosphere, a downdraft velocity of 41 m a monochromatic
continuum enhancement of 0.34 percent, and covers 39 percent of the
quiet Sun. The network brightness increases relative to its average
with a slope of 2.1 percent gauss-1 for Ca + and 2.6 percent gauss
-1 for the continuum while the downdraft velocity increases by 1.6
m 1 gauss-1 for fields between 25 and 120 gauss. Nonlinear effects
appear for larger and smaller fields. The average outward flux density
of network over nonnetwork regions is 2.4 >c 10 ergs 1 forCa+ Kand
3.8 x l08ergscm-2s-1 for the continuum. Photometric calibration of the
Ca + K line observations was effected by a comparison of the observed
relative contrast statistics with a statistically equivalent absolute
brightness distribution obtained from a calibrated slit spectrum of
the Ca + K line. Subject headings:atmospheres, solar - Ca ii emission -
magnetic fields, solar - solar atmospheric motions
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Title: How to Observe Faculae
Authors: Frazier, E. N.
1975BAAS....7..472F Altcode:
No abstract at ADS
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Title: A Velocity Error in Babcock-Type Magnetographs
Authors: Frazier, E. N.
1974SoPh...38...69F Altcode:
An associated error exists in the velocities observed with Babcock-type
magnetographs. This error is used to derive information concerning the
fine structure of magnetic field regions. To calculate a velocity error
which agrees with observation a generalization of Stenflo's model of
a profile of a magnetic filament is used. The model calculation is
compared with the observational data to show that the reproduction
of the observed velocity error with reasonable values of the free
parameter in the three Stenflo filament profiles is possible.
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Title: The Small-Scale Structure of Solar Velocity Fields
Authors: Frazier, E. N.
1974BAAS....6..287F Altcode:
No abstract at ADS
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Title: Motions of Chromospheric Fine Structures
Authors: Frazier, E. N.
1974IAUS...56...97F Altcode:
No abstract at ADS
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Title: A New Dual Filter Telescope
Authors: Frazier, E. N.
1973BAAS....5U.272F Altcode:
No abstract at ADS
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Title: On the Small-Scale Structure of Solar Magnetic Fields
Authors: Frazier, E. N.; Stenflo, J. O.
1972SoPh...27..330F Altcode:
The small-scale structure of solar magnetic fields has been studied
using simultaneous recordings in the spectral lines Fe I 5250 Å and Fe
I 5233 Å, obtained with the Kitt Peak multi-channel magnetograph. We
find that more than 90% of the magnetic flux in active regions
(excluding the sunspots), observed with a 2.4 by 2.4″ aperture, is
channelled through narrow filaments. This percentage is even higher in
quiet areas. The field lines in a magnetic filament diverge rapidly
with height, and part of the flux returns back to the neighbouring
photosphere. Therefore the strong fields within a magnetic filament are
surrounded by weak fields of the order of a few gauss of the opposite
polarity. The field-strength distribution within a filament, including
the surrounding opposite-polarity fields, seems to be almost the same
for all filaments within a given active or quiet region.
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Title: Comments on the Paper 'Fine Structure of Solar Magnetic Fields'
by H. Zirin
Authors: Frazier, Edward N.
1972SoPh...26..142F Altcode:
No abstract at ADS
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Title: The Magnetic Structure of Arch Filament Systems
Authors: Frazier, Edward N.
1972SoPh...26..130F Altcode:
Photographic-type magnetograms are used in conjunction with Hα
filtergrams to study the structure and evolution of magnetic fields
associated with arch filament systems. The magnetograms show that the
opposite ends of the arch filaments are indeed rooted in photospheric
magnetic fields of opposite polarity. Furthermore, these magnetic
field systems are in every case new magnetic flux appearing at the
solar surface. Time lapse studies show the detailed process by which
the flux tubes emerge through the surface. First, supergranules bring
individual strands of magnetic flux to the surface and sweep the two
feet of the flux tube to opposite sides of the supergranule. Then,
the flux tube rises through the chromosphere, creating a visible arch
filament. It is also shown that the observed rotation of the axis of
an arch filament system in the plane of the solar surface is caused
by the emergence of successive flux loops, each possessing different
axial tilts.
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Title: On the Quantitative Description of the Fluctuating Solar
Atmosphere. I. Regression Analysis and Calibration of Multi-channel
Observations
Authors: Skumanich, A.; Smythe, C.; Frazier, E. N.
1972BAAS....4W.391S Altcode:
No abstract at ADS
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Title: The Relations between Chromospheric Features and Photospheric
Magnetic Fields
Authors: Frazier, Edward N.
1972SoPh...24...98F Altcode:
High resolution photographic magnetograms are compared with
Hα filtergrams (both on- and off - band) for a wide variety of
solar features. It is verified that Hα filaments overlie neutral
lines or bands and that Hα plages always occur at magnetic field
clumps. However, the brightness of Hα plages bear no relation
to magnetic field strength or polarity, and the direction of
the magnetic field with respect to threads and filaments remains
obscure. Counter-examples can be found for virtually every `rule'
that has been formulated so far.
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Title: On the Filamentary Nature of Active-Region Magnetic Fields
Authors: Stenflo, J. O.; Frazier, E. N.
1972lfpm.conf..295S Altcode:
No abstract at ADS
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Title: Multi-Channel Magnetograph Observations. III: Faculae
Authors: Frazier, Edward N.
1971SoPh...21...42F Altcode:
Simultaneous observations of photospheric magnetic fields, CaII K
emission, the `photospheric network' and continuum faculae show that
these four quantities are correlated in a complicated manner. The
photospheric and calcium networks show increasing contrast with
increasing magnetic field strength up to field strengths of about
500 G. Higher values of the magnetic field are found only in pores
and sunspots. Continuum faculae also show increasing contrast with
increasing magnetic field strength (even at the disk center), but this
contrast reaches a maximum at field strengths of about 200 G. At higher
field strengths, continuum faculae become monotonically darker until
pore or spunspot conditions are reached.
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Title: Supergranulation at the Center of the Disk
Authors: Frazier, E. N.
1971IAUS...43..260F Altcode:
No abstract at ADS
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Title: Multi-Channel Magnetograph Observations. II. Supergranulation
Authors: Frazier, Edward N.
1970SoPh...14...89F Altcode:
The Kitt Peak multi-channel magnetograph was used to make raster
scans of the super-granulation. The region scanned was carefully
selected to be quiet and was located at the center of the disk. Each
point in the raster was observed twice (with a time interval of
150 sec) and averaged, thereby cancelling out effects of the 5 min
oscillations. Subsequent raster scans were made over a period of 4
h and averaged, further reducing short-lived, nonperiodic modes and
enhancing the long-lived super-granulation.
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Title: Supergranulation at the Center of the Solar Disk
Authors: Frazier, Edward N.
1970BAAS....2T.192F Altcode:
No abstract at ADS
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Title: Multi-Channel Magnetograph Observations. I: Comparison with
Spectroheliograms
Authors: Frazier, Edward N.; Scherrer, Philip H.
1969SoPh...10..297F Altcode:
A new technique for displaying magnetograph observations is
presented and applied to the 12-channel magnetograph at Kitt Peak
National Observatory. Using the data from a raster scan, a digital
`spectroheliogram' is constructed on the face of a cathode ray tube and
photographed. This enables one to recognize patterns in magnetograph
data as easily as with conventional photographs. Comparisons with
simultaneous spectroheliograms show no qualitative differences and
indicate that the magnetograph is quite capable of studying morphology
of individual solar features.
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Title: Computer Display of Magnetograph Observations
Authors: Frazier, Edward N.
1969BAAS....1..276F Altcode:
No abstract at ADS
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Title: An Observational Study of the Hydrodynamics of the Lower
Solar Photosphere
Authors: Frazier, Edward N.
1968ApJ...152..557F Altcode:
Velocity and temperature fluctuations in the solar photosphere were
studied using a series of high- resolution spectrograms of the same
area on the surface of the Sun at intervals of 20 sec for 55 mm The
observations were made with the McMath solar telescope at Kitt Peak
National Observatory. Doppler shifts and intensity fluctuations were
measured on every frame for three lines, Si ii X6371 .36, Fe X6364.38,
and Fe X6355.04, and their temporal properties were studied using
Fourier analysis techniques. The use of these three lines allowed the
author to study the Fourier properties as a function of altitude in
the range from the convection zone to the temperature minimum. The
power spectrum of the velocity fluctuations showed a large amount of
the low-frequency, or convective, component. This low-frequency power
was about 70 per cent coherent with the granulation, and in phase
with it. Furthermore, it was present at all levels of the photosphere,
implying a consider- able amount of convective overshoot all the way up
to the temperature minimum. Specifically, 61 per cent of the power at
the level of the Si ii line was convective, and 3.5 per cent of this
power penetrated to the temperature minimum. The increased Fourier
resolution, afforded by the relatively long observing time of 55 mill,
resolved the oscillatory (300-sec period) component into two components;
a very sharp component with a period of 265 sec, and a weaker, broader
component with a period of 345 sec. Both of these periods remain con-
stant with altitude. The relative amplitudes of the two components
vary with altitude in the sense that the 265-sec component becomes
relatively stronger with height. No vertical phase lags were observed
at any frequency; the oscillations must be standing waves. The velocity
auto-correlation functions showed that these oscillations are extremely
long-lived, probably steady state. The power spectra of the intensity
fluctuations showed primarily the convective component, again at all
levels. Small amounts of oscillatory power were seen, however, in all
intensity power spectra. Even the continuum intensity power spectrum
contained 10 per cent oscillatory power. The many pairs of coherence
and phase spectra yielded additional details of the hydrodynamics of
the various modes
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Title: A Spatio-Temporal Analysis of Velocity Fields in the Solar
Photosphere
Authors: Frazier, E. N.
1968ZA.....68..345F Altcode:
No abstract at ADS
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Title: A Spatio-Temporal Analysis of Fine-Scale Velocity Fields in
the Photosphere.
Authors: Frazier, Edward
1968AJS....73Q..61F Altcode:
A series of high (spatial) resolution spectrograms were taken of
the center of the solar disk at Kitt Peak National Observatory. The
spectrograms were taken every 20 seconds for 55 minutes. The Doppler
shifts of the absorption lines, as well as the intensity fluctuations,
both in the continuum and in the lines, were subjected to a simultaneous
spatial and temporal analysis. The results are displayed in the form of
contour lines in the k -~ plane, or diagnostic diagram. These results
clearly show convective overshoot at all levels of the photosphere. They
also show that the well-known 5-minute oscillations are primarily
standing resonant acoustic waves.
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Title: An Observational Study of the Hydrodynamics of the Lower
Solar Photosphere
Authors: Frazier, E. N.
1966PASP...78..424F Altcode:
No abstract at ADS
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Title: An Observational Study of the Hydrodynamics of the Lower
Solar Photosphere .
Authors: Frazier, Edward Nelson
1966PhDT.........2F Altcode:
No abstract at ADS
