The pre-outburst flare of the A 0535+26 August/September 2005 outburst

被引：39

作者：

Caballero, I. ^{[1
]}

Santangelo, A. ^{[1
]}

Kretschmar, P. ^{[2
]}

Staubert, R. ^{[1
]}

Postnov, K. ^{[1
,3
]}

Klochkov, D. ^{[1
]}

Camero-Arranz, A. ^{[4
]}

Finger, M. H. ^{[5
]}

Kreykenbohm, I. ^{[1
,6
]}

Pottschmidt, K. ^{[7
,8
]}

Rothschild, R. E. ^{[9
]}

Suchy, S. ^{[9
]}

Wilms, J. ^{[10
]}

Wilson, C. A. ^{[5
]}

机构：

[1] Inst Astron & Astrophys, D-72076 Tubingen, Germany

[2] ESAC, ISOC, Madrid, Spain

[3] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia

[4] Univ Valencia, Inst Ciencias Mat, GACE, Valencia 46071, Spain

[5] Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA

[6] ISDC, CH-1290 Versoix, Switzerland

[7] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA

[8] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA

[9] Univ Calif San Diego, CASS, La Jolla, CA 92093 USA

[10] Univ Erlangen Nurnberg, Astron Inst, D-96049 Bamberg, Germany

来源：

ASTRONOMY & ASTROPHYSICS | 2008年 / 480卷 / 02期

关键词：

X-rays : binaries; stars : magnetic fields; stars : individual : A 0535+26;

D O I：

10.1051/0004-6361:20079310

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We study the spectral and temporal behavior of the High Mass X-ray Binary A 0535+26 during a "pre-outburst flare" which took place similar to 5d before the peak of a normal (type I) outburst in August/September 2005. We compare the studied behavior with that observed during the outburst. Methods. We analyse RXTE observations that monitored A 0535+26 during the outburst. We complete spectral and timing analyses of the data. We study the evolution of the pulse period, present energy-dependent pulse profiles both at the initial pre-outburst flare and close to outburst maximum, and measure how the cyclotron resonance-scattering feature (hereafter CRSF) evolves. Results. We present three main results: a constant period P = 103.3960(5) s is measured until periastron passage, followed by a spin-up with a decreasing period derivative of. P = (-1.69 +/- 0.04) x 10(-8) s s(-1) at MJD 53 618, and P remains constant again at the end of the main outburst. The spin-up provides evidence for the existence of an accretion disk during the normal outburst. We measure a CRSF energy of E-cyc similar to 50 keV during the pre-outburst flare, and E-cyc similar to 46 keV during the main outburst. The pulse shape, which varies significantly during both pre-outburst flare and main outburst, evolves strongly with photon energy.

引用

页码：L17 / U1

页数：5

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