Multipeaked X-ray bursts from 4U/MXB 1636-53 - evidence for burst-induced accretion disk coronae

Journal Article · Wed Apr 01 04:00:00 EST 1987 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/184858· OSTI ID:6067397

Melia, F

The specific features of multipeaked X-ray bursts from 4U/MXB 1636-53, which are relatively weak and show no correlated photospheric radius expansion or contraction near the burst maximum, are explained using a model in which the observed luminosity is the sum of the direct component from the central source attenuated through an accretion disk corona and a component due to diffuse scattering by the corona. According to this model, the central peak in the triple-peaked burst results from an enhanced scattering emissivity of the direct component. At large inclination angles, the direct component may be unobservable; a burst detected via the scattered component only would be relatively short, weak, and would have similar rise and decay times. The direct and scattered components can be distinguished by X-ray polarimetry. 30 references.

• Research Organization: Chicago Univ., IL
• OSTI ID: 6067397
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 315; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ACCRETION DISKS
ATMOSPHERES
BINARY STARS
COSMIC RAY SOURCES
COSMIC X-RAY SOURCES
ELECTROMAGNETIC RADIATION
IONIZING RADIATIONS
MATHEMATICAL MODELS
NEUTRON STARS
RADIATIONS
STAR ACCRETION
STAR EVOLUTION
STAR MODELS
STARS
STELLAR ACTIVITY
STELLAR ATMOSPHERES
STELLAR CORONAE
STELLAR FLARES
X RADIATION