REGIMES OF HIGH-ENERGY SHOCK EMISSION FROM THE BE STAR PULSAR SYSTEM PSR-1259-63

被引：62

作者：

TAVANI, M

ARONS, J

KASPI, VM

机构：

[1] PRINCETON UNIV,DEPT PHYS,PRINCETON,NJ 08544

[2] UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720

[3] UNIV CALIF BERKELEY,DEPT PHYS,BERKELEY,CA 94720

来源：

ASTROPHYSICAL JOURNAL | 1994年 / 433卷 / 01期

关键词：

GAMMA-RAYS; THEORY; PULSARS; INDIVIDUAL; (PSR-B1259-63); STARS; EMISSION-LINE; BE; X-RAYS;

D O I：

10.1086/187542

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

PSR B1259-63 is a 47 ms radio pulsar in a wide, eccentric orbit with a Be star. We study the shock interaction between the pulsar and the companion's mass outflow and investigate the time evolution of radiative shock regimes. We find that for small values of the Be star's mass-loss rate, inverse-Compton scattering is likely to dominate the shock emission. Alternately, for a large mass-loss rate, synchrotron emission will dominate. Multifrequency X-ray and gamma-ray observations near periastron can distinguish between these cases and yield unique constraints on the pulsar and Be star winds. The PSR B1259-63 system provides a unique laboratory to study the time-dependent interaction of a pulsar wind with the circumbinary material from its companion star.

引用

页码：L37 / L40

页数：4

共 13 条

[1] HIGH-ENERGY EMISSION FROM THE ECLIPSING MILLISECOND PULSAR PSR 1957+20 [J].