Abstract: The early history of the development of our understanding of neutron stars has been described by others, and we summarize it only briefly here. Following an early speculation by Baade & Zwicky ( 1934) soon after the discovery of the neutron in 1932, Oppenheimer & Volkoff(1939) presented a classic analysis of the theoretical viability of neutron stars, based on the general theory of relativity and the nuclear physics that was then known. A number of further theoretical studies were published during the next three decades, but it seemed that neutron stars might be virtually unobservable and thus remain little more than a theorist's curiosity piece. In a prophetic paper, Pacini (1967) noted that a rotating neutron star with a magnetic field whose axis was misaligned with the rotation axis should emit intense magnetic dipole radiation. Almost immediately thereafter (but quite independently), Hewish et al. (1968a,b) announced the discovery of radio pulsars. For a brief period, several theoretical models for the pulsar phenomenon were in contention. However, the discovery of the pulsar NP 0532 in the Crab Nebula (Staelin & Reifenstein i968, Comella et al. 1 969), followed by a notably straightforward set of observations and theoretical arguments, soon clinched the case for neutron stars (Gold 1969a).1 (For a review of these remarkable developments, see Gold 1969b.)

Abstract: Catalogue des listes de coordonnees, magnitudes, parametres orbitaux, parametres stellaires des composantes, et autres proprietes caracteristiques de 97 binaires cataclysmiques, 20 binaires RX a faible masse et 20 objets relies

Abstract: Mass-accreting white dwarfs in close binary systems are generally thought to be Type I supernova (SN I) progenitors. Low-mass (Mtot≲5 M⊙) binary X-ray sources (also known as Type II sources) equally appear to be the descendants of cataclysmic variables (CV) and thus to have been produced by the collapse of a mass-accreting white dwarf. We point out here that a single process, thermonuclear ignition inside a partially solid, carbon–oxygen white dwarf, may account for the full range of phenomena: from mildly or non-explosive collapses leaving a condensed remnant up to ‘slow’ to ‘fast’ SN I outbursts with total disruption of the parent star.

Abstract: Numerous observations of SS 433 were obtained with the Einstein X-ray Observatory over an 18 month period from 1979 March through 1980 October. MPC (as well as imaging) data from these observations show that the central object in SS 433 is variable in intensity and spectrum on a wide range of time scales. Flares appear to be correlated with the 13 day binary period, and may be more numerous at particular phases of the 164 day period. No evidence for variability on time scales less than 5 minutes is seen, suggesting the central X-ray source is extended and that the compact object itself is not directly visible. A model for SS 433 is suggested wherein the companion star has a spin misaligned with the orbital angular momentum. The volume of the Roche lobe reaches a minimum twice per binary orbit, giving rise to enhanced accretion which results in X-ray and radio flares. Additional constraints imposed by the X-ray and optical data suggest the compact object in SS 433 is an approximately 10-solar-mass black hole.

Abstract: X-ray emissions from HM Sge obtained in 1981 from the HEAO-2 satellite are analyzed and compared quantitatively with observations of HM Sge made in 1980 and of HM Sge, V 1016 Cyg, and RR Tel made in 1979. The change in the X-ray emission from HM Sge between 1979 and 1981 is found to be consistent with the X-ray luminosity and/or temperature of the emitting region declining with an e-folding timescale of the order of one to several decades. Comparison with X-ray data from V 1016 Cyg and RR Tel gives a composite X-ray light curve that is also consistent with such a decline. A comparison of the X-ray observation with spectroscopic information makes it possible to constrain the properties of the X-ray emitting region: the result is consistent with emission from an optically thin region between the two stars in the system where their winds collide head on. It is also shown that the observations are inconsistent with a stellar (blackbody) source, with emission from an accretion disk around a white dwarf or a neutron star, and with emission from a single star wind from either a white dwarf or a neutron star.

Abstract: The idea that solar oscillations might have been stimulated by gravitational radiation from a nearby binary system1,2 has recently been explored by Delache and co-workers3,4. They have announced that the γ-ray source CG195+4, known as Geminga, varies in intensity with a period of 159.96min (ref. 3), and therefore has a frequency just (1 yr)−1 greater than the 160.01-min solar oscillation5–7. From this coincidence they have inferred a gravitational connection between the two oscillations. We show here that if the generally accepted ideas of gravitational radiation are correct, the 160-min solar oscillation could not have been driven to its observed amplitude by any binary system of stellar mass. Only if there were a sustained resonance between the incident radiation and a solar mode of oscillation could there be any chance of an observable response. However, gravitational radiation causes the binary system to spin up, prohibiting it from remaining in resonance with a 160-min mode for long enough to have a perceptible effect It is just possible that 5-min oscillations in the Sun could be excited to an observable amplitude by a binary system having an orbital period of ∼10 min at 1,000 AU.

Abstract: High-resolution IUE spectra of Sk 160, the optical counterpart of the X-ray source SMC X-1, show substantial variations with orbital phase of the resonance P Cygni profiles. These variations are ascribed to the changing ionization state in the stellar wind caused by the X-rays emitted by the companion, as suggested by Hatchett and McCray and first established for the galactic X-ray binary Vela X-1. Furthermore, the profile observed during X-ray eclipse differs significantly from profiles of similar stars in the absence of X-ray ionization.

Abstract: On a observe 8 pulsars RX: Her X-1, Cen X-3, 4U 1626-67, OAO 1657-415, A 0535+26, Vela X-1, 4U 1538-52 et GX 301-2. On donne les periodes de pulsation, mesurees entre Mars 1979 et Octobre 1983, ainsi que celles de 4U 1700-37 et 4U 1907+09

Abstract: Resultats des observations par le satellite IUE de la contrepartie optique de la source RX transitoire periodique et recurente du GNM A0538-66

Abstract: Recent observations1,2 of the X-ray binary source Cygnus X-3 have revealed a flux of ultra-high energy γ rays. Other observations and subsequent models suggest that Cyg X-3 may be a dominant source of galactic high-energy cosmic rays. Here I investigate whether it is possible to escape this conclusion with a model in which most of the energy of accelerated particles at the source is emitted as curvature radiation (that is, radiation emitted by particles travelling on curved paths in a magnetic field so strong that synchrotron radiation is suppressed). I conclude that such a model is not consistent with the observations.

Abstract: X-ray, optical and ultraviolet observations of massive binary systems have yielded basic information on the masses and radii of the massive early-type companions and the masses and moments of inertia of the neutron stars. We briefly review the evidence for the existence of accretion disks in massive X-ray binaries.

Abstract: The authors present an orbit for the double-lined spectroscopic binary HD 63099 based on 77 spectra. The mass ratio is typical of other known WC5 binary systems; likewise the inferred mass of the Wolf-Rayet component is relatively small.

Abstract: Close binaries can evolve through various ways of interaction into compact objects (white dwarfs, neutron stars, black holes) Massive binary systems (mass of the primary M 1 larger than 14 to 15 M 0) are expected to leave, after the first stage of mass transfer a compact component orbiting a massive star These systems evolve during subsequent stages into massive X-ray binaries Systems with initial large periode evolve into Be X-ray binaries

Abstract: We present a high resolution (λ/Δλ = 80) Soft X-ray spectrum (44-95 A) of the magnetic white dwarf binary AM Her obtained with the Objective Grating Spectrometer on board the Einstein observatory. Black body fits to the continuum strongly limits the range of allowable parameters and indicate a "color" temperature in the soft X-ray range between 40 and 55 eV (90% confidence limits). After egress from the eclipse the spectrum hardens and indicates a black body temperature increase from 38 eV to 52 eV. This is interpreted as a limb darkening effect of a layer with negative outward temperature gradient. Assuming the radiative flux to be constant, both the soft X-ray spectrum and the UV spectrum are consistent with a plane parallel layer in radiative equilibrium with an effective temperature of 20 eV. The color temperature in the soft X-ray range is insensitive to the effective temperature in such layers. A variable heating source at large optical depth associated with a variable accretion rate, changes the soft X-ray intensity but does not change the soft X-ray nor the UV spectral shape.

Abstract: The nature of the high energy universe and the design of instruments to analyze stellar and galactic radiation are described in this history of the HEAO program and its scientific and technical accomplishments. Topics covered include: creative violence, stellar explosions, cosmic rays, superbubbles, stellar coronas, collapsed stars, neutron stars, degenerate dwarf stars, black holes, X-ray images of galaxies, galactic nuclei, spiral galaxies, galactic clusters, the mystery of the missing mass, and cosmic fire.

Abstract: The evolutionary processes of close binary stars have been examined. It is found that there is a strong deficit of binaries evolving in CaseA in the whole mass range. Probably the binary stars having binary separation corresponding to CaseA evolution cannot form.

Abstract: Interpretation de 822 observations de ce systeme sur les plaques de Sonneberg a l'aide d'une camera plein ciel

Abstract: We present a model to explain the origin of galactic bulge X-ray sources. We study the evolution of initially cold and massive carbon-oxygen white dwarfs in a close binary system. Under this assumption the core of the white dwarf is solid when the star is reactivated by mass transfer. This implies a low velocity burning front as compared with the fluid case and perhaps a chemical differentiation of the star. Both effects allow the electron captures to overcome the thermonuclear burning. So, the collapse to a neutron star is a very likely outcome.

Abstract: The orbital evolution of a massive binary system interacting with a background field of single stars whose phase density is homogeneous in configuration space is considered. The velocity distribution is assumed isotropic up to some limiting value, and a typical field star is regarded as having a velocity much higher than the orbital speed of the pair components. An expression is derived for the transfer of energy from the binary to the field stars. The time evolution of the orbit parameters a, e is established, and the evolution rate is estimated for Kardashev's (1983) model galactic nucleus containing a central black-hole binary. On the above assumptions the components should become twice as close together within only a few tens of millennia, although the picture may change fundamentally if the nucleus is rotating. 13 references.

Abstract: The spherically symmetric accretion of matter onto a neutron star with a weak magnetic field is shown to be accompanied by the generation of gamma rays due to the Comptonization of X=rays from the neutron star on the flow of incident plasma.

Abstract: The peculiar γ-ray burst phenomenon of 5 March, 1979, and the other subsequent bursts on 6 March, 4 April, and 24 April, 1979, are studied, using the physically more realistic exponentially increasing accretion rate on a highly magnetized neutron star from its companion, and the conclusions that pycnonuclear reaction flash for the first and thermonuclear flashes for the subsequent bursts as the most probable model for this series of bursts, are made

Abstract: On examine le spectre optique de HDE 226868 pour montrer l'existence d'une periode lumineuse et RX de 294 jours. On essaie d'expliquer le pourquoi de cette periode

Abstract: A model of Cyg X-3, as a binary cocooned star system with two sources of X-rays, one above the polar caps of the neutron star — the usual pulsar radiation — and the other around the equatorial plane of the magneto-bounding surface formed due to the interaction of the infalling plasma and the magnetic field of the neutron star, is made. The X-ray, γ-ray, and IR radiation light curves are considered from the shadow effect. An upper limit on the mass of the neutron star is estimated from the consideration of periodic derivative purely due to mass loss. A comparison is made with the results of Elsneret al. (1980) and Ghoshet al. (1981), which they derived from the consideration of period derivative purely from apsidal motion.