Accretion of a clumped wind from a red supergiant donor on to a magnetar is suggested by the analysis of the XMM-Newton and NuSTAR observations of the X-ray binary 3A 1954+319

被引：12

作者：

Bozzo, E. ^{[1
]}

Ferrigno, C. ^{[1
]}

Oskinova, L. ^{[2
,3
]}

Ducci, L. ^{[1
,4
]}

机构：

[1] Univ Geneva, Dept Astron, Chemin Ec 16, CH-1290 Versoix, Switzerland

[2] Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany

[3] Kazan Fed Univ, Kremlevskaya Str 18, Kazan, Russia

[4] Univ Tubingen, Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, Sand 1, D-72076 Tubingen, Germany

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2022年 / 510卷 / 03期

关键词：

accretion; accretion discs; stars: massive; stars: neutron; X-rays: binaries; X-rays: individual: 3A 1954+319; X-rays: stars; COUNTERPART; 4U-1700+24; DISCOVERY; STARS; ULX;

D O I：

10.1093/mnras/stab3688

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

3A 1954+319 has been classified for a long time as a symbiotic X-ray binary, hosting a slowly rotating neutron star and an aged M red giant. Recently, this classification has been revised thanks to the discovery that the donor star is an M supergiant. This makes 3A 1954+319 a rare type of high-mass X-ray binary consisting of a neutron star and a red supergiant donor. In this paper, we analyse two archival and still unpublished XMM-Newton and NuSTAR observations of the source. We perform a detailed hardness ratio-resolved spectral analysis to search for spectral variability that could help investigating the structures of the inhomogeneous M supergiant wind from which the neutron star is accreting. We discuss our results in the context of wind-fed supergiant X-ray binaries and show that the newest findings on 3A 1954+319 reinforce the hypothesis that the neutron star in this system is endowed with a magnetar-like magnetic field strength (greater than or similar to 10(14) G).

引用

页码：4645 / 4653

页数：9

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