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Author name code: bruzek
ADS astronomy entries on 2022-09-14
author:"Bruzek, Anton"
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Title: Der Mond - Ein Atlas des Mondes, veröffentlicht in
Zusammenarbeitmit der Royal Astronomical Society.
Authors: Moore, P.; Bruzek, A.
1982demo.book.....M Altcode:
No abstract at ADS
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Title: Landolt-Börnstein. Numerical data and functional
relationships in science and technology. New series. Group VI:
Astronomy, astrophysics and space research. Volume_2. Astronomy and
astrophysics. Extension and supplement to Volume_1. Subvolume a:
methods - constants - solar system.
Authors: Hellwege, K. -H.; Schaifers, K.; Voigt, H. H.; Wolf, R.;
Durrant, C. J.; Behr, A.; West, R. M.; Solf, J.; Weigelt, G.; Schmahl,
G.; Staubert, R.; Trümper, J.; Lemke, D.; Hachenberg, O.; Enslin, H.;
Fricke, W.; Bruzek, A.; Gondolatsch, F.; Ip, W. -H.; Axford, W. I.;
Schubart, J.; Jessberger, E. K.; Rahe, J.; Fechtig, H.; Leinert, C.;
Grün, E.; Pilipp, W.; Scholer, M.; Palme, H.; Suess, H. E.; Zeh,
H. D.; Kirsten, T.
1981lndf.book.....H Altcode:
No abstract at ADS
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Title: On a Peculiar Type of Filament Activation
Authors: Bruzek, A.
1980IAUS...91..203B Altcode:
No abstract at ADS
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Title: Post-flare Hα plage formation
Authors: Bruzek, A.
1979SoPh...61...35B Altcode:
Observations on the permanent transformation during a flare of a fibril
region into a stable plage region are presented and interpreted as
flare-associated re-orientation of the chromospheric magnetic field.
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Title: Small scale motions in the chromosphere and in the corona.
Authors: Bruzek, A.
1979ssms.conf...79B Altcode:
No abstract at ADS
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Title: Flares and Associated Phenomena
Authors: Dodson-Prince, H. W.; Bruzek, A.
1977ASSL...69...81D Altcode: 1977igss.conf...81D
Solar Flare Thermal Flare Flare Area Flare Importance or Flare Class
Comprehensive Flare Index (CFI) Flash Phase Flare Kernels Plage Flare
Two-Ribbon Flare Filament-Associated Flares Homologous Flares Limb
Flares Flare-Associated Phenomena Moreton Wave White-Light Flare X-Ray
Flare Hard X-Ray Flare EUV Bursts Flare Gamma Ray Emission Particle
Flare or Energetic Flare Flare Mechanisms
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Title: Illustrated glossary for solar and solar terrestrial physics
Authors: Bruzek, A.; Durrant, C. J.
1977ASSL...69.....B Altcode: 1977igss.conf.....B; 1977assl...69.....B
This book collects all terms of relevance to solar and solar-terrestrial
physics that appear in current English-language literature. Each
term or group of related terms is given a concise phenomenological
and quantitative description, including the relationship to other
phenomena and an interpretation in terms of physical processes. The
major topics of the glossary encompass the solar interior, the solar
cycle, solar rotation, large-scale circulation, nonspot magnetic
fields, the quiet photosphere and chromosphere, the transition
region, the solar corona, active regions, spots and faculae, flares
and associated phenomena, prominences, solar radio emission, the
solar wind and interplanetary medium, solar-terrestrial physics,
and general theoretical terms. Specific terms defined include solar
neutrinos, convective theory, the solar activity cycle, dynamos,
the general solar magnetic field, the quiet sun, granulation and
supergranulation, coronal holes, sunspot groups, solar activity
indexes, the Evershed and Wilson effects, X-ray flares, EUV bursts,
particle flares, prominence phenomenology, radio noise storms, solar
radio bursts, macro/microturbulence, solar-wind models, geomagnetic
indexes, geomagnetic storms, radiation belts, and aurorae.
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Title: Spots and Faculae
Authors: Bruzek, A.
1977ASSL...69...71B Altcode: 1977igss.conf...71B
Photospheric Faculae Facular Point Polar Faculae Magnetic Knots Moving
Magnetic Features (MMF) Pore Sunspot Umbra Umbral Dots Umbral Flashes
Umbral Oscillations Light Bridges Penumbra Penumbral Waves Evershed
Effect Wilson Effect
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Title: Active Regions
Authors: Martres, M. J.; Bruzek, A.
1977ASSL...69...53M Altcode: 1977igss.conf...53M
(Solar) Activity Active Region Complexes of Activity Emerging Flux
Regions Ephemeral Region Sunspot Group Proper Motion (of Sunspots)
Evolving Magnetic Features (EMF) Parasites or Inclusions Magnetic
Inversion Line Filament Channel or Plage Couloir Chromospheric Plage
Fibrils Moustache (Ellerman Bomb) Magnetic Classification of Active
Regions Mt. Wilson Spot Classification Solar Activity Indices Solar
Activity Data
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Title: Pre-Flare Energy Storage (title only)
Authors: Bruzek, A.
1976SoPh...47..215B Altcode:
No abstract at ADS
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Title: Book reviews
Authors: de Jager, C.; van Rensbergen, Walter; Kuperus, M.; Falthammar,
Carl-Gunne; Mewe, R.; Reunen, G. C. M.; Bruzek, A.; Swanenburg,
B. N.; Kleczek, J.; Millman, Peter M.; Vesseur, H. J. A.; Pacini,
F.; Monfils, A.
1976SSRv...18..541D Altcode:
No abstract at ADS
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Title: Solar activity (Activité solaire).
Authors: Newkirk, G.; Dunn, R. B.; Mehltretter, P.; MacQueen, R.;
Bonnet, R. M.; White, O. R.; Fokker, A. D.; Zwaan, C.; Bruzek, A.;
Durrant, C.; Grossmann-Doerth, U.; Mehltretter, J. P.; Svestka, Z.;
de Feiter, L. D.; Tandberg-Hanssen, E.; Howard, R.; Stix, M.; Pneuman,
G. W.; Hundhausen, A. J.; Sawyer, C.; Simon, P.
1976IAUTA..16b..13N Altcode:
No abstract at ADS
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Title: Solar Active Regions and Periodicities in Solar Activity
Authors: Bruzek, A.
1976IAUTA..16...27B Altcode: 1976IAUT...16...27B
No abstract at ADS
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Title: K.-O. Kiepenheuer, 1910 November 10 - 1975 May 23.
Authors: Bruzek, A.
1975SoPh...43....3B Altcode:
No abstract at ADS
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Title: In memoriam
Authors: Bruzek, A.
1975SoPh...43....2B Altcode:
No abstract at ADS
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Title: Changes of the Hα Fibril Pattern during Solar Flares
Authors: Bruzek, A.
1975SoPh...42..215B Altcode:
A pattern of parallel Hα fibrils inside a network cell changed into
a pattern of vertical or radial flbriles after a flare had covered the
region. This may be evidence for a change of the magnetic configuration
during flare occurrence.
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Title: K.-O. Kiepenheuer, 1910 November 10 - 1975 May 23.
Authors: Bruzek, A.
1975S&W....14..352B Altcode:
No abstract at ADS
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Title: The solar flare activity at the beginning of July 1974
Authors: Bruzek, A.
1975KlBer..18..179B Altcode:
A survey of the unexpectedly high flare activity of July, 1974, is
given. The flares occurred in a large spot group which developed and
decayed quickly during its passage across the solar disk. Its magnetic
configuration was rather complex with strong umbral magnetic fields and
a high-gradient delta-configuration. The maximum optical importance of
the flares was 2B while the associated X-ray bursts reached extremely
high intensities, in one case 1 erg/sq cm-sec in the 1 - 8 A band. Two
proton events with enhanced fluxes in the energy ranges below 30 MeV
and below 60 MeV, respectively, were observed. The development of the
presumable proton flare of July 3, 1974, is briefly discussed.
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Title: Book reviews
Authors: de Jager, C.; Bruzek, A.
1974SoPh...34..507D Altcode:
No abstract at ADS
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Title: Optical Evidence for Plasma Ejections and Waves in the
Solar Corona
Authors: Bruzek, A.
1974IAUS...57..323B Altcode:
No abstract at ADS
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Title: Über das Moustache-Phänomen
Authors: Bruzek, A.
1973MitAG..32..187B Altcode:
No abstract at ADS
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Title: Solar Activity
Authors: Bruzek, A.
1973lsp2.conf...39B Altcode:
No abstract at ADS
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Title: Lectures on Space Physics 1: Cosmic Rays and Space Biophysics
Authors: Bruzek, Anton; Pilkuhn, Hartmut
1973lsp1.conf.....B Altcode: 1973lsp1.book.....B
No abstract at ADS
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Title: Lectures on Space Physics 2: Sun and Interplanetary Medium,
Relativistic Astrophysics
Authors: Bruzek, Anton; Pilkuhn, Hartmut
1973lsp2.conf.....B Altcode: 1973lsp2.book.....B
No abstract at ADS
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Title: Some Observational Results on Moustaches
Authors: Bruzek, Anton
1972SoPh...26...94B Altcode:
The results of new observations of moustaches in Hα filtergrams and
in Hα spectra are presented and their relations to photospheric and
chromospheric phenomena are studied. The main findings and conclusions
are: (1) previous results on basic data (size, brightness, lifetime,
etc.) are essentially confirmed; (2) limb observations located the
moustaches at the base of the structured Hα chromosphere, just
above the level of the emission of Hα±1 Å. At the disk moustaches
are, in general, covered by absorbing and slightly Doppler-shifted
chromospheric elements which determine the Hα core in the moustache
spectrum. However, absorption-free moustaches with an Hα emission core
revealing a pure (true) moustache spectrum have also been found; (3)
moustaches have been found to coincide with continuous facular granules;
it is suggested that they are an extension of facular granules into
the chromosphere rather than a low-level flare-like phenomenon.
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Title: On the Relation between Filaments (Prominences) and Hα Loops
Authors: Bruzek, Anton
1972SoPh...24..118B Altcode:
The relation between occurrence of Hα loops and filaments is discussed
on the occasion of the observation of a new type of transient loops
during a flare associated filament activation. Considering all known
types of loop systems crossing neutral lines it is concluded that
concurrent existence of stable filaments and Hα loops is incompatible.
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Title: Physics of Solar Prominences. Report on an International
Colloquium Held at the German Solar Observatory, Anacapri, September
29 to October 1, 1971
Authors: Bruzek, Anton; Kuperus, Max
1972SoPh...24....3B Altcode:
This colloquium on solar prominences - the first ever held -
has shown that a major part of activity in prominence research in
recent years concentrated on both observation and computation of the
magnetic conditions which were found to play a crucial role for the
development and the maintainance of prominences. Remarkable progress
was made in fine-scale measurements of photospheric magnetic fields
around filaments and in internal field measurements in prominences. In
addition, important information on the structure of the magnetic fields
in the chromosphere adjacent to the filaments may be derived from high
resolution photographs of the Hα fine structure around filaments
which have become available recently; unfortunately, an unambiguous
determination of the vector field in the chromosphere is not yet
possible. <P />It is quite clear, now, that stable filaments extend
along `neutral' lines which divide regions of opposite longitudinal
magnetic fields. Different types of neutral lines are possible,
depending on the history and relationship of the opposite field
regions. There is convincing evidence that the magnetic field in the
neighbouring chromosphere may run nearly parallel to the filament
axis and that there are two field components in stable prominences:
an axial field dominant in the lower parts and a transverse field
dominant in the higher parts. <P />Methods for the computation of
possible prominence field configurations from measured longitudinal
photospheric fields were developed in recent years. In a number of
cases (e.g. for loop prominences) the observed configuration could
be perfectly represented by a force-free or even a potential field;
poor agreement was found between computed and measured field strengths
in quiescent prominences. In order to reconcile both of them it is
necessary to assume electric currents. Unambiguous solutions will not
be found until measurements of the vector field in the photosphere
and in the prominences are available. <P />The two-dimensional
Kippenhahn-Schlüter model is still considered a useful tool for the
study of prominence support and stability. However, a more refined
model taking into account both field components and considering also
thermal stability conditions is available now. It was proposed that
quiescent prominences may form in magnetically neutral sheets in
the corona where fields of opposite directions meet. <P />As for
the problem of the origin of the dense prominence material there
are still two opposite processes under discussion. The injection of
material from below, which was mainly applied to loop prominences, has
recently been considered also a possible mechanism for the formation of
quiescent prominences. On the other hand, the main objections against
the condensation mechanism could be removed: it was shown that (1)
sufficient material is available in the surrounding corona, and that
(2) coronal matter can be condensed to prominence densities and cooled
to prominence temperatures in a sufficiently short time. <P />The energy
balance in prominences is largely dependent on their fine structure. It
seems that a much better radiative loss function for optically thin
matter is now available. The problem of the heat conduction can only
be treated properly if the field configuration is known. Very little is
known on the heating of the corona and the prominence in a complicated
field configuration. For the optically thick prominences the energy
balance becomes a complicated radiative transfer problem. <P />Still
little is known on the first days of prominence development and on
the mechanism of first formation which, both, are crucial for the
unterstanding of the prominence phenomenon. As a first important step,
it was shown in high resolution Hα photographs that the chromospheric
fine structure becomes aligned along the direction of the `neutral'
line already before first filament appearance. More Hα studies and
magnetic field measurements are badly needed. <P />Recent studies
have shown that even in stable prominences strong small-scale internal
rotational or helical motions exist; they are not yet understood. On the
other hand, no generally agreed interpretation of large-scale motions of
prominences seems to exist. A first attempt to explain the ascendance
of prominences, the `Disparitions Brusques', as the result of a kink
instability was made recently. <P />New opportunities in prominence
research are offered by the study of invisible radiations: X-rays and
meterwaves provide important information, not available otherwise,
on physical conditions in the coronal surroundings of prominences;
EUV observations will provide data on the thin transition layer between
the cool prominence and the hot coronal plasma.
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Title: Properties of solar active regions.
Authors: Bruzek, A.
1972sstp.conf...49B Altcode:
No abstract at ADS
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Title: Properties of Solar Active Regions
Authors: Bruzek, A.
1972ASSL...29...49B Altcode: 1972sun..conf...49B
No abstract at ADS
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Title: Flare Associated Coronal Expansion Phenomena
Authors: Bruzek, Anton; Demastus, Howard L.
1970SoPh...12..447B Altcode:
Two classes of coronal expansion phenomena have been studied
in Sacramento Peak coronal movies: Slow, slightly decelerated
expansion phenomena (v=∼10− =∼ 2 km/sec) and fast, accelerated,
quasi-exploding arches (v =∼ 10 - > 100 km/sec). The various
phenomena were found to be associated with flares in different ways:
The slow expansions were long lived post-flare phenomena initiated by
the flare; the accelerated expanding arches were either (a) arches
expanding prior to and apparently exploding at flare onset, or (b)
arches apparently emerging from the flare (probably in its initial
phase) and rapidly expanding and exploding, or (c) the expansion and
disruption of (originally stable) coronal arches during occurrence of
a distant flare. These expansions may be considered as evidence for
corresponding flare associated changes in the coronal magnetic field.
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Title: Motions in Arch Filament Systems
Authors: Bruzek, A.
1969SoPh....8...29B Altcode:
A new analysis of Hα filtergrams and Hα spectra of arch filament
systems (AFS) shows that material flows downwards in both branches
of the arch filaments (v ≈ 50 km/sec) while the top of the arches
ascends (v ≲ 10 km/sec). It is suggested that AFS are produced by
the magnetic field which expands, between growing spots, into higher
levels carrying material with it that subsequently slides down along
the magnetic field following gravity.
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Title: Flare associated optical phenomena
Authors: Bruzek, A.
1969sfsr.conf...61B Altcode:
No abstract at ADS
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Title: Koronale Expansionsphänomene
Authors: Bruzek, A.
1969MitAG..27..211B Altcode:
No abstract at ADS
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Title: Strukturen um Sonnenflecken.
Authors: Bruzek, A.
1969Umsch..69..212B Altcode:
No abstract at ADS
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Title: Solar flares
Authors: Bruzek, A.
1969pia..conf...71B Altcode:
No abstract at ADS
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Title: Flares in the active region during the proton flare period
of July 1966.
Authors: Bruzek, A.
1969AIQSY...3...82B Altcode:
No abstract at ADS
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Title: Dynamik von Hα Feinstrukturen in aktiven Gebieten der Sonne
Authors: Bruzek, A.
1968MitAG..25..189B Altcode:
No abstract at ADS
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Title: Bright Points (moustaches) and Arch Filaments in Young
Active Regions
Authors: Bruzek, A.
1968IAUS...35..293B Altcode:
No abstract at ADS
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Title: On small-scale mass motion associated with flares
Authors: Bruzek, A.
1968mmsf.conf...67B Altcode:
No abstract at ADS
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Title: On Arch-Filament Systems in Spotgroups
Authors: Bruzek, A.
1967SoPh....2..451B Altcode:
Systems of arch-shaped filaments (AFS) occurring in the interspot region
of young bipolar groups are studied. Their main characteristics are:
Average length: 30000km, average width 20000km, width of individual
filaments 1000-3000 km, height of arches 4-15000 km. A typical lifetime
of the filaments 30 min; appreciable changes of the system occur
within several hours; the lifetime of a system is about three days. -
The arch-filament systems bridge the `neutral' line and connect the
regions of the innermost spots of opposite polarity. Material moves
along the filaments (v ∼ 25-50 km/sec) following the direction of the
magnetic field, and sometimes arches are observed rising at a rate of
∼ 20 km/sec. They are very dark on the inner disk and appear either in
emission or in absorption close to the solar limb. - The occurrence of
`bright points' (moustaches) is found to be closely associated with AFS
in young spotgroups. - The possible nature of AFS and their relation
to other types of filamentary structures is discussed.
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Title: Physics of Solar Flares: The Energy and Mass Problem
Authors: Bruzek, A.
1967sp...conf..399B Altcode:
No abstract at ADS
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Title: Das Flare-Phänomen auf der Sonne
Authors: Bruzek, A.
1966MitAG..21....7B Altcode:
No abstract at ADS
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Title: On the Association Between Loop Prominences and Flares.
Authors: Bruzek, A.
1964ApJ...140..746B Altcode:
The evolution of loop prominence systems (LPS) and their relation to
flares were studied using Ha observations from the solar limb and the
solar disk. The limb observations show that a small LPS may start to
develop from a flare knot several minutes after flare onset. The LPS's
then grow discontinuously at a rate of the order of 10 km/sec by the
formation of higher and higher loops which attain maximum heights
of 40000 up to 150000 km (average valu , 83000 km); they have a
characteristic lifetime of 12 hours. All LPS's so far detected on the
disk (25 cases) were closely ?elated to major flares of the twostrand
expanding type which produced strong SSWF effects (100 per cent), Type
IV bursts (95 per cent), and PCA effects (85 per cent). Depending on
their position the LPS's appeared on the disk in various shapes and with
different delay times after flare onset; they were visible either in
emission or in absorption. The observations strongiy suggest that the
LPS's are part of a powerful flare event and are due to a propagation
of the flare process into the solar corona. A model of the evolution
bf the combined flare-loop system is derived from the observations.
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Title: Optical Characteristics of Cosmic Ray and Proton Flares
Authors: Bruzek, Anton
1964JGR....69.2386B Altcode:
In recent years several attempts have been made to find characteristic
properties of the optical manifestations of flare events that produce
the energetic protons which generate cosmic-ray increases at ground
level (GLE) and polar-cap absorption effects (PCA). In a study1 of 9
flares which were followed by a PCA effect Dodson and Hedeman [1962]
recognized that in each of these cases part of the Ha flare covered
the umbra of a large spot. Ellison et al. [1961] noticed that all
cosmic-ray flares which had been well observed on the solar disk
(7 cases) consisted of two roughly parallel bright strands which
covered partly or completely the largest umbras of the associated spot
group. Avignon et al. [1963] found a similar arrangement of the flare
filaments in 13 out 15 PCA flares.
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Title: Case Histories of Flares: The Large Flares of July 11, 12,
18, and 20, 1961
Authors: Bruzek, A.
1964NASSP..50..301B Altcode: 1964psf..conf..301B
No abstract at ADS
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Title: The Influence of Flares on the Associated Permanent Coronal
Condensation
Authors: Bruzek, A.
1963IAUS...16..137B Altcode:
No abstract at ADS
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Title: Über Fleckenprotuberanzen vor der Sonnenscheibe. Mit 4
Textabbildungen
Authors: Bruzek, A.
1962ZA.....54..225B Altcode:
No abstract at ADS
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Title: Über die Umlaufgeschwindigkeit der polaren Filamente. Mit
2 Textabbildungen
Authors: Bruzek, A.
1961ZA.....51...75B Altcode:
No abstract at ADS
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Title: Beobachtungen über die Beziehungen zwischen Eruptionen und
Fleckenfeldern. Mit 4 Textabbildungen
Authors: Bruzek, A.
1960ZA.....50..110B Altcode:
No abstract at ADS
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Title: Über die Spiculen auf der Sonnenscheibe. Mit 2 Textabbildungen
Authors: Bruzek, A.
1959ZA.....47..191B Altcode:
No abstract at ADS
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Title: Die Filamente und Eruptionen eines Aktivitätszentrums. Mit
6 Textabbildungen
Authors: Bruzek, A.
1958ZA.....44..183B Altcode:
No abstract at ADS
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Title: Über eruptionsartige Fackeln bei Filamentaufstiegen. Mit
5 Textabbildungen
Authors: Bruzek, A.; Becker, U.
1957ZA.....42...76B Altcode:
No abstract at ADS
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Title: Die Korona-Emissionsgebiete und ihre Beziehungen zu
Sonnenflecken und Fackeln. Mit 15 Textabbildungen.
Authors: Bruzek, A.
1955ZA.....35..213B Altcode:
No abstract at ADS
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Title: Die Mitte-Rand-Variation der H<SUB>α-</SUB>-Linienbreite,
der H<SUB>α-</SUB> Zentralintensität und der Flächen der
Eruptionen. Mit 4 Textabbildungen
Authors: Bruzek, A.
1955ZA.....38....1B Altcode:
No abstract at ADS
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Title: Beziehungen zwischen Protuberanzen und monochromatischer
Korona. Mit 5 Textabbildungen
Authors: Bruzek, A.
1955ZA.....35..265B Altcode:
No abstract at ADS
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Title: Die hypothetische Neigung der Sonnenfleckenachsen. Mit 4
Textabbildungen
Authors: Bruzek, A.
1953ZA.....33..267B Altcode:
No abstract at ADS
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Title: On a type of flare associated with ascendant dark filaments
Authors: Bruzek, A.
1952Obs....72..154B Altcode:
No abstract at ADS
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Title: Über die Ursache der ”Plötzlichen" Filamentauflösungen. Mit
4 Textabbildungen
Authors: Bruzek, A.
1952ZA.....31...99B Altcode:
No abstract at ADS
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Title: Die Ausbreitung von "Euptionsstörungen". Mit 2 Textabbildungen
Authors: Bruzek, A.
1952ZA.....31..111B Altcode:
No abstract at ADS
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Title: Beobachtungen über das Verhalten von Filamenten während
chromosphärischer Eruptionen. Mit 7 Textabbildungen
Authors: Bruzek, A.
1951ZA.....28..277B Altcode:
No abstract at ADS
