Author name code: steinitz ADS astronomy entries on 2022-09-14 author:"Steinitz, Raphael" ------------------------------------------------------------------------ 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. Bibcode: 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. Title: Application of Strong Spin Correlation in Visual Binaries Authors: Farbiash, N.; Steinitz, R. Bibcode: 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. Title: Stellar Atmospheres and the Diamagnetic Effect Authors: Farbiash, N.; Steinitz, R. Bibcode: 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. Title: Statistics of multiple systems Authors: Steinitz, Raphael Bibcode: 2007msf..confE..24S Altcode: No abstract at ADS Title: Binary Systems Evolution History: Spin Correlation in Visual Binaries Independent of Member Separation Authors: Steinitz, R.; Farbiash, N. Bibcode: 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. Title: Structural Modification of Stellar Atmospheres by the Diamagnetic Effect Authors: Farbiash, N.; Steinitz, R. Bibcode: 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. Title: The origin of the Moon: a gravitational instability? Authors: Griv, E.; Gedalin, M.; Steinitz, R. Bibcode: 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 Title: How is the Diamagnetic Effect (DME) Relevant to Stellar Surface Phenomena? Authors: Farbiash, Netzach; Steinitz, Raphael Bibcode: 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. Title: Evolutionary memeory in binary systems? Authors: Farbiash, N.; Steinitz, R. Bibcode: 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. Title: Spin Correlation In Binary Systems Authors: Farbiash, N.; Steinitz, R. Bibcode: 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. Title: Correlation of Projected Spins in Binary Systems Authors: Farbiash, N.; Steinitz, R. Bibcode: 2003ndcb.conf..106F Altcode: No abstract at ADS Title: Test Case for the Diamagnetic Effect: Helium Peculiarities in B Stars Authors: Steinitz, R. Bibcode: 2003ASPC..305..252S Altcode: 2003mfob.conf..252S No abstract at ADS Title: Ensemble and Time Averages: the Missing Diamagnetic Effect Authors: Steinitz, R. Bibcode: 2002stma.conf..233S Altcode: No abstract at ADS Title: Abundance Modification by the Diamagnetic Effect Authors: Steinitz, Raphael; Kunoff, Estelle Bibcode: 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. Title: Helium Peculiarities of B Stars Authors: Steinitz, Raphael; Goldstein, Ulzan Bibcode: 1997Ap&SS.252..423S Altcode: No abstract at ADS Title: Test Case for the Diamagnetic Effect: Helium Peculiarities on B Stars Authors: Steinitz, Raphael; Goldstein, Ulzan Bibcode: 1996JKASS..29..237S Altcode: No abstract at ADS Title: Helium peculiarities as a possible manifestation of the diamagnetic effect Authors: Goldstein, U.; Steinitz, R. Bibcode: 1996ASPC..109..685G Altcode: 1996csss....9..685G No abstract at ADS Title: Coronal Mass Ejections and the Critical Ionization Velocity Phenomenon Authors: Golbraikh, E.; Filippov, M.; Steinitz, R. Bibcode: 1995JApAS..16..388G Altcode: No abstract at ADS Title: Masked Coronal Mass Ejections - an Attempt to De-Mask Them Authors: Filippov, M.; Golbraikh, E.; Steinitz, R. Bibcode: 1995JApAS..16..388F Altcode: No abstract at ADS Title: Diamagnetic Acceleration of the Solar Wind Authors: Sekeles, B.; Steinitz, R. Bibcode: 1995JApAS..16..390S Altcode: No abstract at ADS Title: Misconceptions Concerning the Vanishing Average of the Diamagnetic Effect Authors: Steinitz, R. Bibcode: 1995JApAS..16R.389S Altcode: No abstract at ADS Title: Diamagnetic Abundance Differentiation Authors: Steinitz, R.; Kunoff, E. Bibcode: 1995JApAS..16Q.389S Altcode: No abstract at ADS Title: A new model for peculiar Helium stars Authors: Steinitz, R.; Goldstein, U. Bibcode: 1995IAUS..176P.151S Altcode: No abstract at ADS Title: Coronal Mass Ejections and the Critical Velocity Ionization Phenomenon Authors: Golbraikh, F.; Filippov, M.; Steinitz, R. Bibcode: 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. Title: Abundance Modification by the Diamagnetic Effect Authors: Steinitz, R.; Kunoff, E. Bibcode: 1994scs..confQ.498S Altcode: 1994IAUCo.144Q.498S No abstract at ADS Title: Masked Coronal Mass Ejections: an Attempt to Demask Them Authors: Filippov, M.; Golbraikh, F.; Steinitz, R. Bibcode: 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. Title: Diamagnetic Temperature Control in the Solar Wind Authors: Steinitz, R.; Sekeles, B. Bibcode: 1994scs..confR.472S Altcode: 1994IAUCo.144R.472S No abstract at ADS Title: The diamagnetic effect: misconception about its vanishing average. Authors: Steinitz, R. Bibcode: 1994scs..confQ.472S Altcode: No abstract at ADS Title: Diamagnetic Acceleration of the Solar Wind Authors: Sekeles, B.; Steinitz, R. Bibcode: 1994scs..confR.498S Altcode: 1994IAUCo.144R.498S No abstract at ADS Title: Stellar Spots - Heating and Cooling Diamagnetically Authors: Steinitz, R.; Goldstein, U. Bibcode: 1993ASPC...44..279S Altcode: 1993IAUCo.138..279S; 1993pvnp.conf..279S No abstract at ADS Title: Diamagnetic Abundance Differentiation in the Solar System(cp) Authors: Steinitz, R.; Kunoff, E. Bibcode: 1992IAUS..150..425S Altcode: No abstract at ADS Title: Thermodynamic equilibrium of astrophysical plasmas in magnetic fields. Is it possible? Authors: Steinitz, R.; Lonke, A. Bibcode: 1989BAPS...34.1284S Altcode: No abstract at ADS Title: Diamagnetic heating of stellar coronae Authors: Steinitz, Raphael Bibcode: 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. Title: Elemental abundance differentiation in the solar chromosphere — corona Authors: Steinitz, Raphael Bibcode: 1988VA.....31...27S Altcode: No abstract at ADS Title: Diamagnetic Acceleration of Solar and Stellar Winds Authors: Steinitz, R.; Lonke, A. Bibcode: 1987sowi.conf...88S Altcode: No abstract at ADS Title: Solar Wind and Interstellar Medium Interaction Signature at 8.3 - 8.4 AU? Authors: Steinitz, R. Bibcode: 1987sowi.conf..680S Altcode: No abstract at ADS Title: Diamagnetic Heat Filters or Maxwell's Demon Resurrected Authors: Lonke, A.; Steinitz, R. Bibcode: 1985tphr.conf..327L Altcode: No abstract at ADS Title: Diamagnetic heat filters, or Maxwell's demon resurrected. Authors: Lonke, A.; Steinitz, R. Bibcode: 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. Title: Removal of velocity bias in the interpretation of measurements of the azimuthal component of the interplanetary magnetic field Authors: Eyni, M.; Steinitz, R. Bibcode: 1983JGR....88.7236E Altcode: Parker's model for the interplanetary magnetic field predicts an r-1 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. Title: Momentum Flux Invariance and Solar Wind Sources Authors: Steinitz, R. Bibcode: 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 nu2r2 does not depend on flow speed nor on distance, verifying the previously established invariance of momentum flux density (mnu2) carried by the solar wind. Averages of mnu2 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. Title: Global properties of the solar wind. III - Density and temperature fluctuations Authors: Eyni, M.; Steinitz, R. Bibcode: 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. Title: Global properties of the solar wind. II - Empirical proton temperature gradients and their dependence on flow velocity Authors: Eyni, M.; Steinitz, R. Bibcode: 1981ApJ...243..279E Altcode: Published spacecraft data on proton temperatures in the solar wind are fitted to an expression (T/T0) = (u/u0)β(r/r0)-α, 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.

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.

Additional masking effects due to stream-stream interactions and averaging over large flow-velocity variance are pointed out. Title: Competing Effects Determining the Proton Temperature Gradient in the Solar Wind Authors: Steinitz, R.; Eyni, M. Bibcode: 1981sowi.conf..164S Altcode: No abstract at ADS Title: Global properties of the solar wind. I. The invariance of the momentum flux density. Authors: Steinitz, R.; Eyni, M. Bibcode: 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. Title: Are Solar Wind Measurements of Different Spacecraft Consistent Authors: Steinitz, R.; Eyni, M. Bibcode: 1980IAUS...91..151S Altcode: No abstract at ADS Title: An empirical relation between density, flow velocity and heliocentric distance in the solar wind Authors: Eyni, M.; Steinitz, R. Bibcode: 1980IAUS...91..147E Altcode: No abstract at ADS Title: Velocity biasing in sampling of the solar wind Authors: Steinitz, R.; Eyni, M. Bibcode: 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/u2, in order to reduce the strong dependence of temperature on velocity. Title: Cooling of slow solar wind protons from the helios 1 experiment Authors: Eyni, M.; Steinitz, R. Bibcode: 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. Title: The cooling of solar wind protons from mariner 2 data Authors: Eyni, M.; Steinitz, R. Bibcode: 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. Title: The embedded feature model for the interpretation of chromospheric contrast profiles. Authors: Steinitz, R.; Gebbie, K. B.; Bar, V. Bibcode: 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. Title: Cooling of the solar wind protons. Mariner 2 data. Authors: Eyni, M.; Steinitz, R. Bibcode: 1977BuIPS..23..110E Altcode: No abstract at ADS Title: A New Method for Determining Doppler Widths Authors: Steinitz, R.; Bar, V.; Wyckoff, S. Bibcode: 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 Title: On the Variations in the Spectra of AP Stars Authors: Steinitz, R.; Gebbie, K. B. Bibcode: 1975BAAS....7..512S Altcode: No abstract at ADS Title: Emission Conditions for Solar He II Authors: Epstein, G. L.; Steinitz, R. Bibcode: 1975BAAS....7..522E Altcode: No abstract at ADS Title: The Formation of the HeI λ584 and HeII λ304 Resonance Lines in the Solar Transition Region Authors: Gebbie, K. B.; Steinitz, R. Bibcode: 1975BAAS....7..523G Altcode: No abstract at ADS Title: Solar He II - A Reappraisal. Authors: Epstein, G. L.; Steinitz, R. Bibcode: 1975BAAS....7..450E Altcode: No abstract at ADS Title: A General Approach to the Interpretation of Chromospheric Mottles Authors: Gebbie, K. B.; Steinitz, R. Bibcode: 1975BAAS....7..353G Altcode: No abstract at ADS Title: The non-LTE transport equation for polarized radiation in the presence of magnetic fields. I. Formulation. Authors: House, L. L.; Steinitz, R. Bibcode: 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. Title: Determination of the Doppler Width of Solar Hα in the Chromosphere. Authors: Wyckoff, S.; Steinitz, R. Bibcode: 1974BAAS....6R.428W Altcode: No abstract at ADS Title: On Spatial Variations in the Intensity of Chromospheric HA Authors: Gebbie, K. B.; Steinitz, R. Bibcode: 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. Bibcode: 1974BAAS....6..264S Altcode: No abstract at ADS Title: Comparison of Hα and CA II H and K Spectroheliograms as a Diagnostic Probe Authors: Gebbie, K. B.; Steinitz, R. Bibcode: 1974IAUS...56...55G Altcode: No abstract at ADS Title: The Stokes Formulation of Non-LTE Radiative Transfer in a Magnetic Field Authors: House, Lewis L.; Steinitz, Raphael Bibcode: 1973ApL....15..129H Altcode: No abstract at ADS Title: On the Visibility of Hα Fibrils Authors: Steinitz, R.; Gebbie, K. B. Bibcode: 1973BAAS....5T.280S Altcode: No abstract at ADS Title: A Mechanism for the Production of Light and Dark Contrasts in Radiatively Controlled Lines Authors: Gebbie, K. B.; Steinitz, R. Bibcode: 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. Title: On the dependence of the two-levelsource function on its own radiation field. Authors: Steinitz, Raphael; Shine, Richard A. Bibcode: 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 = (hv/kT - 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. Title: The Short Period Magnetic Variable HD 133029 Authors: Steinitz, Raphael; Pyper, Diane M. Bibcode: 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. Title: The period of gamma Equ. Authors: Steinitz, R.; Pyper, D. M. Bibcode: 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 Title: 3 Hya = HD 72968 Authors: Steinitz, R.; Pyper, D. M. Bibcode: 1970IBVS..413....1S Altcode: No abstract at ADS Title: Rotational Correlation in Binary Stars Authors: Steinitz, R.; Pyper, D. M. Bibcode: 1970stro.coll..165S Altcode: 1970IAUCo...4..165S No abstract at ADS Title: Magnetic Multipole Expansion and Line Profiles Authors: Leibowitz, E.; Steinitz, Raphael Bibcode: 1967mrs..conf...89L Altcode: No abstract at ADS Title: Rotation of magnetic stars Authors: Steinitz, R. Bibcode: 1967maco.conf..189S Altcode: No abstract at ADS Title: The Magnetic Oblique Rotator Authors: Steinitz, Raphael Bibcode: 1967mrs..conf...83S Altcode: No abstract at ADS Title: The Period of the Magnetic Variable HD 8441 Authors: Steinitz, R. Bibcode: 1965IBVS..101....1S Altcode: No abstract at ADS Title: Overstability in rotating stars Authors: Steinitz, R. Bibcode: 1965IAUS...22..117S Altcode: No abstract at ADS Title: The period of the magnetic variable HD 8441 (Note) Authors: Steinitz, R. Bibcode: 1965BAN....18..125S Altcode: No abstract at ADS Title: Magnetic stars and rotation Authors: Steinitz, R. Bibcode: 1964BAN....17..504S Altcode: No abstract at ADS Title: Studies on magnetic stars Authors: Steinitz, R. Bibcode: 1964PhDT.......116S Altcode: No abstract at ADS Title: Studies on magnetic stars Authors: Steinitz, Raphael Bibcode: 1964PhDT.......128S Altcode: No abstract at ADS