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Author name code: steinitz
ADS astronomy entries on 2022-09-14
author:"Steinitz, Raphael"
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Title: CP and related phenomena in the context of Stellar Evolution
Authors: Braithwaite, J.; Akgün, T.; Alecian, E.; Kholtygin, A. F.;
Landstreet, J. D.; Mathis, S.; Michaud, G.; Portnoy, J.; Alecian,
G.; Bychkov, V. D.; Bychkova, L. V.; Drake, N.; Fabrika, S. N.;
Reisenegger, A.; Steinitz, R.; Vick, M.
2010HiA....15..161B Altcode: 2010arXiv1002.4091B
We review the interaction in intermediate and high mass stars between
their evolution and magnetic and chemical properties. We describe
the theory of Ap-star ‘fossil’ fields, before touching on the
expected secular diffusive processes which give rise to evolution of
the field. We then present recent results from a spectropolarimetric
survey of Herbig Ae/Be stars, showing that magnetic fields of the kind
seen on the main-sequence already exist during the pre-main sequence
phase, in agreement with fossil field theory, and that the origin of the
slow rotation of Ap/Bp stars also lies early in the pre-main sequence
evolution; we also present results confirming a lack of stars with
fields below a few hundred gauss. We then seek which macroscopic motions
compete with atomic diffusion in determining the surface abundances of
AmFm stars. While turbulent transport and mass loss, in competition with
atomic diffusion, are both able to explain observed surface abundances,
the interior abundance distribution is different enough to potentially
lead to a test using asterosismology. Finally we review progress on
the turbulence-driving and mixing processes in stellar radiative zones.
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Title: Application of Strong Spin Correlation in Visual Binaries
Authors: Farbiash, N.; Steinitz, R.
2007IAUS..240..383F Altcode:
We find correlation between the projected rotational velocities
(spins) in binary systems. Tidal interaction could be the reason for
such a correlation in close binaries. There is, however, strong spin
correlation in visual binaries as well; moreover, it is independent
of the separation of the components. Our results therefore indicate
the possibility that spin correlation in binaries is the result of
evolutionary history, rather than that of tidal interaction. Studies
of spin correlation in binaries could thus be an important tool in
understanding the evolution of such systems.
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Title: Stellar Atmospheres and the Diamagnetic Effect
Authors: Farbiash, N.; Steinitz, R.
2007ASPC..368..197F Altcode:
The structure of stellar atmospheres is modified when they include
embedded diverging magnetic fields. Diamagnetic Effects (DME) combined
with gravity result in speed filters. These, in turn, modify the
hydrostatic and thermal structure. Using numerical simulations of
charged particle motion, we examine the relevant effects. The run
of temperature and pressure is the result of the modified effective
gravity for the faster particles of the thermal distribution.
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Title: Statistics of multiple systems
Authors: Steinitz, Raphael
2007msf..confE..24S Altcode:
No abstract at ADS
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Title: Binary Systems Evolution History: Spin Correlation in Visual
Binaries Independent of Member Separation
Authors: Steinitz, R.; Farbiash, N.
2006ASPC..349..399S Altcode:
We found directional correlation of spins in binaries. The degree
of correlation is independent of the components' separation. It is
remarkable that spin correlation in visual binaries is strong. Here
we examine the possible implications related to the evolution of such
a system.
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Title: Structural Modification of Stellar Atmospheres by the
Diamagnetic Effect
Authors: Farbiash, N.; Steinitz, R.
2006ASPC..349..237F Altcode:
The structure of stellar atmospheres is modified when they include
embedded diverging magnetic fields. This is due to the Diamagnetic
Effect and the resulting speed filters. Here we examine some of the
relevant effects of these speed filters, using numerical simulations of
the motion of charged particles. They demonstrate how the hydrostatic
and thermal structure of the atmosphere is modified by the DME. Values
of pressure and temperature changes are caused by diminishing the
“effective" gravity by the faster particles of the normal distribution.
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Title: The origin of the Moon: a gravitational instability?
Authors: Griv, E.; Gedalin, M.; Steinitz, R.
2006cosp...36..154G Altcode: 2006cosp.meet..154G
The origin of the Moon has long been of interest and although the
Giant Impact theory is currently the preferred explanation unequivocal
supporting evidence has been lacking The megaimpact model is based on
the concept of a collision with the Earth of a body whose mass exceeded
one to two Martian masses Such an idea was suggested by Cameron and
coauthors and then developed mainly numerically in a number of papers In
our opinion however the megaimpact hypothesis belongs to a rare class
of catastrophic hypotheses that are based on low-probability random
events Here we consider an opposite model a regular evolution process
The formation of the Earth--Moon system is re-examined by considering
the stability of the common preplanetary disk of gas and dust with
a mass of about 100M oplus and a radius of about 100R oplus In the
framework of this model the preplanetary disk forms self-gravitating
massive sim 10-30 M oplus gaseous proto-Earth and proto-Moon through
a gravitational instability of the gas accompanied by settling and
coagulation of dust grains to form solid cores The larger part of
the initial mass of the Earth--Moon system as well as the initial
mass of protoplanets of the Earth s group were probably blown away
due to intensive thermal emission of the early Sun It is shown that a
collective process forming the basis of the gravitational instability
hypothesis solves with surprising simplicity the two main problems of
the dynamical characteristics of the Moon which are associated with
its significant mass and large orbital
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Title: How is the Diamagnetic Effect (DME) Relevant to Stellar
Surface Phenomena?
Authors: Farbiash, Netzach; Steinitz, Raphael
2005AIPC..784..596F Altcode: 2005astro.ph..1143F
The structure of stellar atmospheres can be modified if they include
embedded diverging magnetic fields. This is due to the presence of
speed filters. Here we examine some of the relevant effects through the
numerical simulation of the motion of charged particles. We introduce
the concept of "floating" particles and point out the relevance of
the diamagnetic effet (DME) to the evolution of Maxwellian velocity
distributions into Non-Maxwellian.
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Title: Evolutionary memeory in binary systems?
Authors: Farbiash, N.; Steinitz, R.
2004ASPC..318..226F Altcode: 2004ssrc.conf..226F; 2004astro.ph.12185F
Correlation between the spins (rotational velocities) in binaries has
previously been established. We now continue and show that the degree
of spin correlation is independent of the components' separation. Such
a result might be related for example to Zhang's non-linear model for
the formation of binary stars from a nebula.
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Title: Spin Correlation In Binary Systems
Authors: Farbiash, N.; Steinitz, R.
2004RMxAC..21...15F Altcode: 2004IAUCo.191...15F; 2004astro.ph.12182F
We examine the correlation of projected rotational velocities in binary
systems. It is an extension of previous work (Steinitz and Pyper,
1970; Levato, 1974). An enlarged data basis and new tests enable us
to conclude that there is indeed correlation between the projected
rotational velocities of components of binaries. In fact we suggest
that spins are already correlated.
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Title: Correlation of Projected Spins in Binary Systems
Authors: Farbiash, N.; Steinitz, R.
2003ndcb.conf..106F Altcode:
No abstract at ADS
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Title: Test Case for the Diamagnetic Effect: Helium Peculiarities
in B Stars
Authors: Steinitz, R.
2003ASPC..305..252S Altcode: 2003mfob.conf..252S
No abstract at ADS
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Title: Ensemble and Time Averages: the Missing Diamagnetic Effect
Authors: Steinitz, R.
2002stma.conf..233S Altcode:
No abstract at ADS
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Title: Abundance Modification by the Diamagnetic Effect
Authors: Steinitz, Raphael; Kunoff, Estelle
1999ApJ...510L..77S Altcode:
Abundances of elements with first ionization potential (FIP) less
than 10 eV in the corona and solar wind are augmented relative to the
solar photosphere. This enhancement has been found to be independent
of both mass and charge. We emphasize two facts that are relevant to
this problem: (1) Only elements with FIP<10 eV are already ionized
in the chromosphere, while in the corona, all elements are ionized. (2)
It is known that diverging magnetic field structures anchored in the
photosphere pass to the chromosphere (e.g., sunspots). Considering
these facts, we construct a model in which the combination of the
diamagnetic effect and gravity will pump charged particles, but not
neutrals, from the chromosphere into the corona, thus producing the
observed enhancement of low- versus high-FIP elements. This charged
particle pump is operational irrespective of the existence of other
mechanisms that have been proposed previously. Qualitative agreement
is obtained with observed abundance ratios in the Sun and several stars.
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Title: Helium Peculiarities of B Stars
Authors: Steinitz, Raphael; Goldstein, Ulzan
1997Ap&SS.252..423S Altcode:
No abstract at ADS
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Title: Test Case for the Diamagnetic Effect: Helium Peculiarities
on B Stars
Authors: Steinitz, Raphael; Goldstein, Ulzan
1996JKASS..29..237S Altcode:
No abstract at ADS
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Title: Helium peculiarities as a possible manifestation of the
diamagnetic effect
Authors: Goldstein, U.; Steinitz, R.
1996ASPC..109..685G Altcode: 1996csss....9..685G
No abstract at ADS
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Title: Coronal Mass Ejections and the Critical Ionization Velocity
Phenomenon
Authors: Golbraikh, E.; Filippov, M.; Steinitz, R.
1995JApAS..16..388G Altcode:
No abstract at ADS
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Title: Masked Coronal Mass Ejections - an Attempt to De-Mask Them
Authors: Filippov, M.; Golbraikh, E.; Steinitz, R.
1995JApAS..16..388F Altcode:
No abstract at ADS
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Title: Diamagnetic Acceleration of the Solar Wind
Authors: Sekeles, B.; Steinitz, R.
1995JApAS..16..390S Altcode:
No abstract at ADS
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Title: Misconceptions Concerning the Vanishing Average of the
Diamagnetic Effect
Authors: Steinitz, R.
1995JApAS..16R.389S Altcode:
No abstract at ADS
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Title: Diamagnetic Abundance Differentiation
Authors: Steinitz, R.; Kunoff, E.
1995JApAS..16Q.389S Altcode:
No abstract at ADS
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Title: A new model for peculiar Helium stars
Authors: Steinitz, R.; Goldstein, U.
1995IAUS..176P.151S Altcode:
No abstract at ADS
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Title: Coronal Mass Ejections and the Critical Velocity Ionization
Phenomenon
Authors: Golbraikh, F.; Filippov, M.; Steinitz, R.
1994scs..conf..159G Altcode: 1994IAUCo.144..159G
The authors propose a new viewpoint concerning the mechanism for
coronal mass ejection (CME) formation in the solar corona.
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Title: Abundance Modification by the Diamagnetic Effect
Authors: Steinitz, R.; Kunoff, E.
1994scs..confQ.498S Altcode: 1994IAUCo.144Q.498S
No abstract at ADS
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Title: Masked Coronal Mass Ejections: an Attempt to Demask Them
Authors: Filippov, M.; Golbraikh, F.; Steinitz, R.
1994scs..conf..101F Altcode: 1994IAUCo.144..101F
The authors unify the elaborated classification system applied to
Coronal Mass Ejections (CME). They conclude that it is not necessary to
keep ten different morphological classes of CME's, when they represent
only one and the same phenomenon, seen in different aspects.
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Title: Diamagnetic Temperature Control in the Solar Wind
Authors: Steinitz, R.; Sekeles, B.
1994scs..confR.472S Altcode: 1994IAUCo.144R.472S
No abstract at ADS
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Title: The diamagnetic effect: misconception about its vanishing
average.
Authors: Steinitz, R.
1994scs..confQ.472S Altcode:
No abstract at ADS
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Title: Diamagnetic Acceleration of the Solar Wind
Authors: Sekeles, B.; Steinitz, R.
1994scs..confR.498S Altcode: 1994IAUCo.144R.498S
No abstract at ADS
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Title: Stellar Spots - Heating and Cooling Diamagnetically
Authors: Steinitz, R.; Goldstein, U.
1993ASPC...44..279S Altcode: 1993IAUCo.138..279S; 1993pvnp.conf..279S
No abstract at ADS
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Title: Diamagnetic Abundance Differentiation in the Solar System(cp)
Authors: Steinitz, R.; Kunoff, E.
1992IAUS..150..425S Altcode:
No abstract at ADS
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Title: Thermodynamic equilibrium of astrophysical plasmas in magnetic
fields. Is it possible?
Authors: Steinitz, R.; Lonke, A.
1989BAPS...34.1284S Altcode:
No abstract at ADS
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Title: Diamagnetic heating of stellar coronae
Authors: Steinitz, Raphael
1988VA.....31..435S Altcode:
This paper presents a model for a stellar coronal heating mechanism
based on magnetic structures. It is shown that the mechanism of
diamagnetic heating does not depend on energy transport to a corona in
the form of waves and their dissipation. Temperature gradients can be
sustained in the presence of diverging magnetic field structures. Thus,
the specific configuration on a given star can account for the
variable emission intensity as the star rotates, as well as for the
large dispersion in X-ray fluxes for a given bolometric magnitude.
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Title: Elemental abundance differentiation in the solar chromosphere
— corona
Authors: Steinitz, Raphael
1988VA.....31...27S Altcode:
No abstract at ADS
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Title: Diamagnetic Acceleration of Solar and Stellar Winds
Authors: Steinitz, R.; Lonke, A.
1987sowi.conf...88S Altcode:
No abstract at ADS
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Title: Solar Wind and Interstellar Medium Interaction Signature at
8.3 - 8.4 AU?
Authors: Steinitz, R.
1987sowi.conf..680S Altcode:
No abstract at ADS
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Title: Diamagnetic Heat Filters or Maxwell's Demon Resurrected
Authors: Lonke, A.; Steinitz, R.
1985tphr.conf..327L Altcode:
No abstract at ADS
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Title: Diamagnetic heat filters, or Maxwell's demon resurrected.
Authors: Lonke, A.; Steinitz, R.
1985MPARp.212..327L Altcode:
The authors explore an alternative to coronal heating. Their approach is
based on the existence of temperature dependent diamagnetic effects in
the presence of magnetic fields with diverging lines of induction. If
a uniform temperature exists in a plasma embedded in a magnetic field
with diverging field lines - heat conduction in the direction of
lower field intensity will result. Thus, a stationary closed magnetic
configuration can sustain a temperature gradient without any flow of
mass, charge or heat.
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Title: Removal of velocity bias in the interpretation of measurements
of the azimuthal component of the interplanetary magnetic field
Authors: Eyni, M.; Steinitz, R.
1983JGR....88.7236E Altcode:
Parker's model for the interplanetary magnetic field predicts
an r<SUP>-</SUP><SUP>1</SUP> dependence for the azimuthal
component. Departures from this relation were indicated in an analysis
of a subset of the Helios 1 data. As in a previous analysis of Pioneer
10 data, these departures can be traced to velocity bias. We examine
the decrease in solar wind speed which occurred as Helios 1 approached
the sun and thus simulated a steeper gradient of the azimuthal magnetic
field component. A simple linear fit between flow speed and distance
from the sun enables us to remove from the data most of the velocity
bias present. This procedure substantially improves the agreement
between Parker's model and the Helios data.
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Title: Momentum Flux Invariance and Solar Wind Sources
Authors: Steinitz, R.
1983SoPh...83..379S Altcode:
New solar wind data from Helios-2 are used to study, in a statistical
fashion, the relation between proton number density n, flow speed
u and heliocentric distance r. It is shown that the average of
nu<SUP>2</SUP>r<SUP>2</SUP> does not depend on flow speed nor on
distance, verifying the previously established invariance of momentum
flux density (mnu<SUP>2</SUP>) carried by the solar wind. Averages of
mnu<SUP>2</SUP> from different spacecraft do not show correlation with
the solar cycle. Rather, the close agreement (to within 1.8%) of values
from Helios-1 and Helios-2 suggests that the momentum flux density
carried by the solar wind may be also constant during the solar cycle.
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Title: Global properties of the solar wind. III - Density and
temperature fluctuations
Authors: Eyni, M.; Steinitz, R.
1982ApJ...256..259E Altcode:
The possibility is demonstrated of studying large-scale interactions in
the solar wind, using all the available data over a continuous range
of distance. The magnitude of the fluctuations of the proton density
and the temperature about their mean values and their correlation
diminish closer to the sun. The dependence of mean values on the
flow speed and the heliocentric distance is dealt with by using mean
value relations. Continuous distance coverage is obtained by using
data from the Helios 1 spacecraft. Indications are that the fast and
intermediate solar winds are more uniform than the slow wind. For the
latter, no clear correlation is found between temperature and density
fluctuations, over the whole range 0.3-1.0 AU.
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Title: Global properties of the solar wind. II - Empirical proton
temperature gradients and their dependence on flow velocity
Authors: Eyni, M.; Steinitz, R.
1981ApJ...243..279E Altcode:
Published spacecraft data on proton temperatures in the
solar wind are fitted to an expression (T/T<SUB>0</SUB>) =
(u/u<SUB>0</SUB>)<SUP>β</SUP>(r/r<SUB>0</SUB>)<SUP>-α</SUP>, using
a two-dimensional regression. This expression exhibits the dependence
of proton temperature T both on flow velocity u and heliocentric
distance r. The expression can be readily used to compare results
from different spacecraft. <P />The cooling index α is found to
depend on flow velocity such that steeper temperature gradients are
obtained for smaller flow velocities. For very low velocities, α >
4/3. This might indicate "superadiabatic" cooling, but can actually
be reconciled with adiabatic rates provided thermal anisotropy is
included in cooling theories. <P />Additional masking effects due
to stream-stream interactions and averaging over large flow-velocity
variance are pointed out.
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Title: Competing Effects Determining the Proton Temperature Gradient
in the Solar Wind
Authors: Steinitz, R.; Eyni, M.
1981sowi.conf..164S Altcode:
No abstract at ADS
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Title: Global properties of the solar wind. I. The invariance of
the momentum flux density.
Authors: Steinitz, R.; Eyni, M.
1980ApJ...241..417S Altcode:
A statistical analysis of published Helios 1 and Mariner 2 data is
used to establish a relation between proton number density n and
flow velocity u. It was found that n is inversely proportional to the
square of u and it is interpreted that this result is an invariance of
the momentum flux density carried by the protons in the solar wind in
different streams. At 1 AU the mean value of the momentum flux density
from Helios 1 is 2.2 x 10 to the -8th dyn/sq cm; similar values are
obtained from Mariner 2 and Vela 3 indicating an overall consistency of
the results from all three spacecraft. The spread in the distribution
of the momentum flux density diminishes closer to the sun, suggesting
that its invariance is a boundary condition at the sun. The faster and
more tenuous the flow, the more energy flux density is carried by it,
supporting the hypothesis that fast streams originate in coronal holes.
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Title: Are Solar Wind Measurements of Different Spacecraft Consistent
Authors: Steinitz, R.; Eyni, M.
1980IAUS...91..151S Altcode:
No abstract at ADS
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Title: An empirical relation between density, flow velocity and
heliocentric distance in the solar wind
Authors: Eyni, M.; Steinitz, R.
1980IAUS...91..147E Altcode:
No abstract at ADS
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Title: Velocity biasing in sampling of the solar wind
Authors: Steinitz, R.; Eyni, M.
1979JGR....84..105S Altcode:
Velocity biasing can lead to erroneous interpretation of temperature
and density evolution of the solar wind. It is argued that possibly
there is no difference in the physics of the slow and fast components
(Helios 1). Finally, it is suggested to use T/u<SUP>2</SUP>, in order
to reduce the strong dependence of temperature on velocity.
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Title: Cooling of slow solar wind protons from the helios 1 experiment
Authors: Eyni, M.; Steinitz, R.
1978JGR....83.4387E Altcode:
Careful sample selection is employed to demonstrate the cooling of
slow solar wind protons compatible with adiabatic expansion. A reduced
temperature is introduced into the analysis.
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Title: The cooling of solar wind protons from mariner 2 data
Authors: Eyni, M.; Steinitz, R.
1978JGR....83..215E Altcode:
We examine the possibility that cooling of solar wind protons has
escaped detection in the Mariner 2 data. After dividing the data into
two velocity ranges and introducing an intermediate quantity τ to
decrease the strong dependence of temperature on velocity, we find
that the low-velocity data exhibit cooling.
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Title: The embedded feature model for the interpretation of
chromospheric contrast profiles.
Authors: Steinitz, R.; Gebbie, K. B.; Bar, V.
1977ApJ...213..269S Altcode:
Contrast profiles obtained from chromospheric filtergrams and spectra of
bright and dark mottles have to date been interpreted almost exclusively
in terms of Becker's cloud model. Here we demonstrate the failure of
this model to account in a physically consistent way for the observed
contrasts. As an alternative, we introduce an embedded-feature model,
restricting our discussion in this paper to stationary features. Our
model is then characterized by three independent parameters: the
density of absorbing atoms, the geometrical depth, and the profile of
the absorption coefficient. An analytic approximation to the contrast
resulting from such a model reproduces well the observed behavior of
all types of contrast profiles.
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Title: Cooling of the solar wind protons. Mariner 2 data.
Authors: Eyni, M.; Steinitz, R.
1977BuIPS..23..110E Altcode:
No abstract at ADS
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Title: A New Method for Determining Doppler Widths
Authors: Steinitz, R.; Bar, V.; Wyckoff, S.
1975ApJ...201..729S Altcode:
An explicit analytical relation between the absorption-line profile
and the emergent intensity is developed for a stellar atmosphere
in which the absorption profile and the source and sink terms of the
source function are depth-independent. Using this relation, a method is
described for determining the Doppler width of the solar chromospheric
Ha absorption profile, for which it is known that the source and sink
terms are indirectly controlled by radiation fields external to the
line-forming zone. Good agreement is found between the Doppler width
derived for solar Ha and previous results. Finally, the method for
determining the Doppler width is generalized for application to stellar
spectra. Subject headings: chromosphere, solar - line formation
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Title: On the Variations in the Spectra of AP Stars
Authors: Steinitz, R.; Gebbie, K. B.
1975BAAS....7..512S Altcode:
No abstract at ADS
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Title: Emission Conditions for Solar He II
Authors: Epstein, G. L.; Steinitz, R.
1975BAAS....7..522E Altcode:
No abstract at ADS
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Title: The Formation of the HeI λ584 and HeII λ304 Resonance Lines
in the Solar Transition Region
Authors: Gebbie, K. B.; Steinitz, R.
1975BAAS....7..523G Altcode:
No abstract at ADS
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Title: Solar He II - A Reappraisal.
Authors: Epstein, G. L.; Steinitz, R.
1975BAAS....7..450E Altcode:
No abstract at ADS
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Title: A General Approach to the Interpretation of Chromospheric
Mottles
Authors: Gebbie, K. B.; Steinitz, R.
1975BAAS....7..353G Altcode:
No abstract at ADS
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Title: The non-LTE transport equation for polarized radiation in
the presence of magnetic fields. I. Formulation.
Authors: House, L. L.; Steinitz, R.
1975ApJ...195..235H Altcode:
A formulation of the radiative transfer of polarized light under
conditions departing from local thermodynamic equilibrium and accounting
for the presence of a magnetic field is presented. The formulation is
self-consistent in that the equations of statistical equilibrium for
magnetic sublevels are also included. The quantum-mechanical derivation
of the absorption matrix, the key to the presentation, is derived in
detail utilizing the density matrix approach. The polarization of the
radiation field is described in terms of the usual Stokes parameters,
but the discussion of the Stokes parameters in this paper illustrates
their quantum mechanical origin and interpretation. The equation of
radiative transfer for the Stokes vector is cast in a form reminiscent
of the nonlocal thermodynamic equilibrium (NLTE) scalar equation
of transfer, except that the equation is now a vector equation in
the Stokes parameters and the source function is a vector function
containing the population of magnetic sublevels.
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Title: Determination of the Doppler Width of Solar Hα in the
Chromosphere.
Authors: Wyckoff, S.; Steinitz, R.
1974BAAS....6R.428W Altcode:
No abstract at ADS
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Title: On Spatial Variations in the Intensity of Chromospheric HA
Authors: Gebbie, K. B.; Steinitz, R.
1974ApJ...188..399G Altcode:
We investigate the formation of patterns in Ha spectroheliograms and
filtergrams. Introducing a source-sink-control diagram, we conclude
that the Ha line source function in the quiet solar chromosphere is
indirectly controlled by the photospheric radiation fields in the Balmer
and Paschen continua. We demonstrate that in producing the observed
patterns, horizontal spatial variations in the shape of the absorption
profile are extremely effective compared to changes in the source and
sink terms. Applying this mechanism, we compute asymptotic values for
the contrasts and visibilities in chromospheric Ha. Subject headings:
chromosphere, solar - line formation - spectroheliograms
---------------------------------------------------------
Title: On the formation of chromospheric Halpha .
Authors: Steinitz, R.; Gebbie, K. B.; Bar, V.
1974BAAS....6..264S Altcode:
No abstract at ADS
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Title: Comparison of Hα and CA II H and K Spectroheliograms as a
Diagnostic Probe
Authors: Gebbie, K. B.; Steinitz, R.
1974IAUS...56...55G Altcode:
No abstract at ADS
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Title: The Stokes Formulation of Non-LTE Radiative Transfer in a
Magnetic Field
Authors: House, Lewis L.; Steinitz, Raphael
1973ApL....15..129H Altcode:
No abstract at ADS
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Title: On the Visibility of Hα Fibrils
Authors: Steinitz, R.; Gebbie, K. B.
1973BAAS....5T.280S Altcode:
No abstract at ADS
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Title: A Mechanism for the Production of Light and Dark Contrasts
in Radiatively Controlled Lines
Authors: Gebbie, K. B.; Steinitz, R.
1973SoPh...29....3G Altcode:
It is argued that visible contrasts can arise even in a line that is
controlled wholly by an external radiation field. Lateral differences
in the local shapes of the line absorption profile are shown to account
for such contrasts. Two cases are treated explicitly: (a) a profile
locally broadened by mass flow, and (b) a profile locally narrower
due to the suppression of turbulent velocities, as might result from
the presence of magnetic fields.
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Title: On the dependence of the two-levelsource function on its own
radiation field.
Authors: Steinitz, Raphael; Shine, Richard A.
1973MNRAS.162..197S Altcode:
The consequences of the universally made assumption that the
stimulated emission profile is identical to the absorption profile
are quantitatively investigated for a two-level atom with Doppler
redistribution. The nonlinear terms arising in the source function are
evaluated iteratively. We find that the magnitude of the effects are
governed by = <SUP>(hv/kT</SUP> - I)-' and are probably completely
negligible for visible and UV solar lines. For = 2 effects of 5 per
cent are encountered. Larger `s lead to numerical instabilities in
the method of solution used.
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Title: The Short Period Magnetic Variable HD 133029
Authors: Steinitz, Raphael; Pyper, Diane M.
1971Ap&SS..11..322S Altcode:
It is shown that the magnetic measurements of HD 133029 exhibit a
correlation of magnetic intensity with exposure length. Due to this
effect a re-examination of the star's period was undertaken, resulting
in a new period of 0.168 days. The significance of such a short period
is discussed. It is argued that this short variation cannot be due to
an oblique rotator.
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Title: The period of gamma Equ.
Authors: Steinitz, R.; Pyper, D. M.
1971A&A....11..489S Altcode:
An analysis of the magnetic variations of Equ yielded a period of
1785.7 days (4.9 years). Key words: magnetic variable - period
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Title: 3 Hya = HD 72968
Authors: Steinitz, R.; Pyper, D. M.
1970IBVS..413....1S Altcode:
No abstract at ADS
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Title: Rotational Correlation in Binary Stars
Authors: Steinitz, R.; Pyper, D. M.
1970stro.coll..165S Altcode: 1970IAUCo...4..165S
No abstract at ADS
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Title: Magnetic Multipole Expansion and Line Profiles
Authors: Leibowitz, E.; Steinitz, Raphael
1967mrs..conf...89L Altcode:
No abstract at ADS
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Title: Rotation of magnetic stars
Authors: Steinitz, R.
1967maco.conf..189S Altcode:
No abstract at ADS
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Title: The Magnetic Oblique Rotator
Authors: Steinitz, Raphael
1967mrs..conf...83S Altcode:
No abstract at ADS
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Title: The Period of the Magnetic Variable HD 8441
Authors: Steinitz, R.
1965IBVS..101....1S Altcode:
No abstract at ADS
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Title: Overstability in rotating stars
Authors: Steinitz, R.
1965IAUS...22..117S Altcode:
No abstract at ADS
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Title: The period of the magnetic variable HD 8441 (Note)
Authors: Steinitz, R.
1965BAN....18..125S Altcode:
No abstract at ADS
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Title: Magnetic stars and rotation
Authors: Steinitz, R.
1964BAN....17..504S Altcode:
No abstract at ADS
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Title: Studies on magnetic stars
Authors: Steinitz, R.
1964PhDT.......116S Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Studies on magnetic stars
Authors: Steinitz, Raphael
1964PhDT.......128S Altcode:
No abstract at ADS
