The Be/X-ray binary A0535+26 during its recent 2009/2010 outbursts

Thumbnail Image

Files

INTEGRAL 2010_063.pdf (526.29 KB)

Links to Files

https://pos.sissa.it/115/063/

Permanent Link

https://doi.org/10.22323/1.115.0063
 http://hdl.handle.net/11603/29829

Collections

UMBC Center for Space Sciences and Technology (CSST) / Center for Research and Exploration in Space Sciences & Technology II (CRSST II)
UMBC Faculty Collection
UMBC Physics Department
UMBC Student Collection

Author/Creator

Author/Creator ORCID

https://orcid.org/0000-0002-4656-6881

Date

2011-11-16

Type of Work

conference papers and proceedings
Text

Department

Program

Citation of Original Publication

Caballero, Isabel, et al. “The Be/X-Ray Binary A0535+26 during Its Recent 2009/2010 Outbursts.” In Proceedings of 8th INTEGRAL Workshop “The Restless Gamma-Ray Universe” — PoS(INTEGRAL 2010), 115:063. SISSA Medialab, 2011. https://doi.org/10.22323/1.115.0063.

Rights

This item is likely protected under Title 17 of the U.S. Copyright Law. Unless on a Creative Commons license, for uses protected by Copyright Law, contact the copyright holder or the author.
Attribution-NonCommercial-ShareAlike 1.0 Generic (CC BY-NC-SA 1.0)

Subjects

Abstract

The Be/X-ray binary A0535+26 showed a giant outburst in December 2009 that reached ∼5.14 Crab in the 15-50 keV range. Unfortunately, due to Sun constraints it could not be observed by most X-ray satellites. The outburst was preceded by four weaker outbursts associated with the periastron passage of the neutron star. The fourth of them, in August 2009, presented a peculiar double-peaked light curve, with a first peak lasting about 9 days that reached a (15- 50 keV) flux of 440 mCrab. The flux then decreased to less than 220 mCrab, and increased again reaching 440 mCrab around the periastron. The outburst was monitored with INTEGRAL, RXTE, and Suzaku TOO observations. One orbital period (∼111 days) after the 2009 giant outburst, a new and unexpectedly bright outburst took place (∼ 1.4Crab in the 15-50 keV range). It was monitored with TOO observations with INTEGRAL, RXTE, Suzaku, and Swift. First results of the spectral and timing analysis of these observations are presented, with a specific focus on the cyclotron lines present in the system and its variation with the mass accretion rate.