Light curve and neutrino spectrum emitted during the collapse of a nonrotating, supermassive star

Baushev, A. N.; Бисноватый-Коган, Г. С.

doi:10.1134/1.1687017

Cited by 11 publications

(24 citation statements)

References 9 publications

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“…An alternative interpretation of the observed lines was suggested in [17]. It assumes an anisotropic distribution of electron velocities in a collisionless shock wave with large Lorentz factors (the ratios of the total electron energy to m e c 2 = 511 keV), γ r ∼ 40.…”

Section: Magnetic Fieldsmentioning

confidence: 99%

“…Equations (16) and (17) are a particular case of this expansion. Petri [76] developed a technique of expansion of electromagnetic fields around a rotating magnetized star over vector spherical harmonics, which allows one to find a solution of the Maxwell equations in the GR for an arbitrary multipole component of the magnetic field.…”

Section: General Relativity Effectsmentioning

confidence: 99%

“…The problem is complicated, because the surface distributions of the magnetic field and the temperature are not known in advance. As a fiducial model one conventionally employs the relativistic dipole model (16), (17), while the temperature distribution, consistent with the magnetic-field distribution, is found from calculations of heat transport in neutronstar envelopes (e.g., [84]). Results of such calculations, performed in [381], are shown in Fig.…”

Section: Spectra Of Magnetic Photospheresmentioning

confidence: 99%

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Atmospheres and radiating surfaces of neutron stars

Potekhin¹

2014

Phys.-Usp.

114

129

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The early 21st century witnesses a dramatic rise in the study of thermal radiation of neutron stars. Modern space telescopes have provided a wealth of valuable information which, when properly interpreted, can elucidate the physics of superdense matter in the interior of these stars. This interpretation is necessarily based on the theory of formation of neutron star thermal spectra, which, in turn, is based on plasma physics and on the understanding of radiative processes in stellar photospheres. In this paper, the current status of the theory is reviewed with particular emphasis on neutron stars with strong magnetic fields. In addition to the conventional deep (semi-infinite) atmospheres, radiative condensed surfaces of neutron stars and "thin" (finite) atmospheres are considered.

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Section: Magnetic Fieldsmentioning

confidence: 99%

Section: General Relativity Effectsmentioning

confidence: 99%

Section: Spectra Of Magnetic Photospheresmentioning

confidence: 99%

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Atmospheres and radiating surfaces of neutron stars

Potekhin¹

2014

Phys.-Usp.

114

129

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“…It was shown by [38] that energy losses by a pulsar relativistic wind are important also when the magnetic and rotational axes coincide, and one may use (2.1) with A = R 6 ns 6c 3 , and B ns corresponding to the magnetic pole, at any inclination angle. Magnetic fields of radio pulsars estimated using (2.1) with observational values of P andṖ lay in a wide region between 10 8 and 10 13 G [55].…”

Section: Radio Pulsarsmentioning

confidence: 99%

“…According to [37,7], in the magnetic field near the pulsar the cross component of a momentum of electrons is emitting rapidly, while the parallel velocity remains constant. Hence the momentum In order to obtain the whole experimental spectrum of the Her X-1 the following model of the hot spot (Fig.5) was considered in [3]. A collision-less shock wave is generated in the accretion flow near the surface on the magnetic pole of a neutron star.…”

Section: Relativistic Dipole Interpretation Of the Spectral Feature Imentioning

confidence: 99%

Evolutions of Neutron Stars and their Magnetic Fields

Бисноватый-Коган¹

2018

Proceedings of XII Multifrequency Behaviour of High Energy Cosmic Sources Workshop — PoS(MULTIF2017)

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Estimations of magnetic fields of neutron stars, observed as radio and X-ray pulsars, are discussed. It is shown, that theoretical and observational values for different types of radio pulsars are in good correspondence. Radio pulsars in close binaries and millisecond pulsars, which have passed the stage of disk accretion (recycled radio pulsars), have magnetic fields 2-4 orders of magnitude smaller than ordinary single pulsars. Most probably, the magnetic field of the neutron star was screened by the infalling material. Several screening models are considered. Formation of single recycled pulsars loosing its companion is discussed. Magnetic fields of some X-ray pulsars are estimated from the cyclotron line energy. In the case of Her X-1 this estimation exceeds considerably the value of its magnetic field obtained from long term observational data related to the beam structure evolution. Another interpretation of the cyclotron feature, based on the relativistic dipole radiation mechanism, could remove this discrepancy. Observational data about soft gamma repeaters and their interpretation as magnetars are critically analyzed.

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The influence of radiative effects on the accretion onto stellar magnetospheres

Kryukov

Pogorelov

Anzer

et al. 2003

A&A

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Abstract. The influence of radiative effects on the accretion onto stellar magnetospheres is investigated by performing global 2-and 2.5-dimensional simulations on the basis of high-resolution numerical schemes with the application of irregular grids adapted to the shape of the magnetopause. The latter is represented by an impermeable, contracted dipole magnetic field surface with polar holes. Accreting matter is assumed to be optically thin. The physical mechanisms which are taken into account include cooling due to free-free and free-bound transitions, the Compton heating via X-ray scattering on electrons, and the inverse Compton cooling in the regions where the temperature of the matter becomes sufficiently large to be able to transfer part of its internal energy to photons. Depending on the determining parameters, both steady-state solutions with a system of discontinuities and unsteady flows with expanding shock waves can be obtained. It is shown that efficient cooling of the matter can substantially facilitate the penetration of the matter through the polar holes. The detailed consideration of the realistic radiative effects proved to be of great importance in our understanding of the accretion phenomenon, since they can substantially affect it both qualitatively and quantitatively.

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Light curve and neutrino spectrum emitted during the collapse of a nonrotating, supermassive star

Cited by 11 publications

References 9 publications

Atmospheres and radiating surfaces of neutron stars

Atmospheres and radiating surfaces of neutron stars

Evolutions of Neutron Stars and their Magnetic Fields

The influence of radiative effects on the accretion onto stellar magnetospheres

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