Neutron Stars in Interacting Binary Systems

Joss, P. C.; Rappaport, S.

doi:10.1146/annurev.aa.22.090184.002541

Cited by 253 publications

(147 citation statements)

References 106 publications

(169 reference statements)

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“…Indeed, neutron stars with masses up to about two solar masses are known to exist. To take the most reliable data [24], the mass of the neutron star 4 U 0900-40, (1.85_+0.35) Mo, can be considered as an upper limit (strictly a lower bound for this limit). This figure can be explained by a sufficiently stiff equation of state only.…”

Section: Applications To Neutron Starsmentioning

confidence: 99%

Neutron matter properties in an extended Brueckner approach

Deneye

Lejeune

1987

Z. Physik A - Atomic Nuclei

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Neutron matter properties are calculated both at zero and finite temperature within an extended Brueckner approach using the Paris potential. The binding energy turns out to be very close to the one calculated variationally with the Urbana v14 potential. Particular emphasis is put on the symmetry energy, on the isospin dependence of the mean field and on the effective mass. As an illustration, the masses of neutron stars are calculated. 21.65. +f PACS: IntroductionA great deal of interest is currently devoted to the nuclear matter equation of state. The present situation is however rather confuse. To describe it very shortly, conventional analysis of giant monopole in nuclei [1,2], early analysis of heavy-ion collisions neglecting effective mass effects [3,4] and microscopic calculations based on potential models, be them performed in a variational [5] or in a (nonrelativistic [6] or relativistic [7]) perturbative scheme, seem to point to a so-called stiff nuclear matter equation of state, i.e. a sharp increase of the binding energy per particle between P0 and ,-~4po (P0 =normal nuclear matter equilibrium density). On the other hand, reanalysis of nuclear properties in the spirit of the Landau sum rules for Fermi liquids [8], and recent calculations on supernovae explosions [9] seem, on the contrary, to suggest that the equation of state would be much softer. Finally, the masses of known neutron stars favour [10] a stiff nuclear matter equation of state. The last considerations involve asymmetric nuclear matter, for which the theoretical investigations are much less numerous in comparison with the symmetric case. In fact, for purely neutronic matter, there is practically only one very sophisticated microscopic * Work supported by the NATO Grant 025.81 calculation [5], based on the variational method. Here, we want to study the same system by a detailed Brueckner type approach, both at zero and at low temperature, extending so our previous investigations of symmetric nuclear matter [6]. Actually, our purpose is fourfold. First, we want to calculate the binding energy of neutron matter, in order to check whether the agreement between variational and perturbative approaches, observed for N =Z [6], also holds for Z = 0. Second, we want to calculate microscopically the symmetry energy. Third, we investigate the single-particle properties of neutron matter both at T= 0 and T+ 0, especially the neutron effective mass, which can play an important role in supernovae explosions. Fourth, we propose ourselves to use our results to calculate the neutron star mass spectrum. This is for illustrative purpose mainly, since this calculation requires the detailed knowledge of the equation of state at large densities, for which the perturbative approach is inadequate or, at least, on less safe grounds than the variational approach.The paper is organized as follows. Section 2 shortly describes the theoretical frame. Section 3 contains the numerical results for the binding energy, the average nucleon field, the effective mass and...

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Section: Applications To Neutron Starsmentioning

confidence: 99%

Neutron matter properties in an extended Brueckner approach

Deneye

Lejeune

1987

Z. Physik A - Atomic Nuclei

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“…The neutron star binary systems [ 3 ] can also be divided i n t o two main classes. The Population I systems have massive companion s t a r s .…”

Section: I Phenomenology Of Compact Binary X-ray Sourcesmentioning

confidence: 99%

“…The gas must be cool ("lO 1 * K) for 3 < E m i n and hot (~1Q8 K) for E > S^. where p i s the gas density in g cm" 3 . T y p i c a l l y , R « 1 f o r the photosphere of compact X-ray sources, even at the surface of a neutron s t a r .…”

Section: V Interaction Of X Rays and Nattermentioning

confidence: 99%

“…F i r s t , i t seems l i k e l y that the w i l d i n t e n s i t y f l u c t u a t i o n s of black hole sources such as Cyg X -l are a manifestation of non-linear i n s t a b i l i t i e s in the inner disk f l o w . Second, the quasi-periodic outbursts of the cataclysmic variables and of the "rapid burster" may be due to the non-linear development of a thermal-viscous i n s t a b i l i t y i n the disk [ 7 -1 0 , 3 …”

Section: Accretion Disksmentioning

confidence: 99%

“…According t o the standard model [ 3 ] , the bursts are a manifestation of thermonuclear flashes of hydrogen and helium gas that has accreted onto the surface of a weakly magnetized neutron s t a r . Thus, i t is reasonable t o attempt to describe the bursts with a s p h e r i c a l l y symmetric hydrodynamic model.…”

Section: I X-ray Burst Sourcesmentioning

confidence: 99%

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Compact Binary X-Ray Sources

McCray

1986

International Astronomical Union Colloquium

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Compact binary X-ray sources include white dwarfs, neutron stars, and black holes that are accreting matter from a companion star. The X-ray emission from these systems is produced by the accreting matter as i t flows through an accretion disk and strikes the surface of the compact object. The emitting regions have opacities dominated by electron scattering, and radiation pressure is likely to play an important role in the hydrodynamics. Strong magnetic fields greatly modify the hydrodynamics and radiation transfer in the pulsating neutron star sources. Accretion disks have complex structure, including an electron scattering corona, a cool outer region, and possibly a thick torus in their inner region. The structure and stab i l i t y properties of accretion disks are only partially understood. Major problems exist with the interpretation of the spectra and luminosities of the X-ray burst sources. The pulsed X-ray emission from the pulsating binary X-ray sources probably comes from "mounds" of accreting gas at the magnetic poles of neutron stars, in which the accreting matter is decelerated by radiation pressure. The physics of these systems is reviewed, with an emphasis on problems for which hydrodynamical simulations may be especially useful.

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Kernmaterie bei extremer Dichte: Von der Supernova zum Quark‐Gluon‐Plasma

Stock¹,

Gutbrod²

1988

Phys. Bl.

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Neutron Stars in Interacting Binary Systems

Cited by 253 publications

References 106 publications

Neutron matter properties in an extended Brueckner approach

Neutron matter properties in an extended Brueckner approach

Compact Binary X-Ray Sources

Kernmaterie bei extremer Dichte: Von der Supernova zum Quark‐Gluon‐Plasma

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