Two black widow pulsars in the optical and X-rays

被引：1

作者：

Bobakov, A. V. ^{[1
]}

Kirichenko, A. Yu. ^{[1
,2
]}

Zharikov, S. V. ^{[2
]}

Karpova, A. V. ^{[1
]}

Zyuzin, D. A. ^{[1
]}

Shibanov, Yu. A. ^{[1
]}

Mennickent, R. E. ^{[3
]}

Garcia-Alvarez, D. ^{[4
,5
]}

机构：

[1] Ioffe Inst, 26 Politekhn Skaya, St Petersburg 194021, Russia

[2] Univ Nacl Autonoma Mexico, Inst Astron, Apdo Postal 106, Ensenada 22800, Baja California, Mexico

[3] Univ Concepcion, Dept Astron, Casilla 160-C, Concepcion, Chile

[4] Inst Astrofis Canarias, Via Lactea S-N, E-38200 San Cristobal la Laguna, Tenerife, Spain

[5] GRANTECAN, Cuesta San Jose S-N, E-38712 Brena Baja, La Palma, Spain

来源：

ASTRONOMY & ASTROPHYSICS | 2024年 / 690卷

基金：

美国国家科学基金会; 俄罗斯科学基金会; 美国国家航空航天局;

关键词：

binaries: close; stars: neutron; pulsars: individual: PSR J2017-1614; pulsars: individual: PSR J1513-2550; NEUTRON-STAR; MILLISECOND PULSARS; GAIA; DEMOGRAPHICS; ABSORPTION; DISCOVERY; COMPANION; RADIUS; MODEL; NICER;

D O I：

10.1051/0004-6361/202450205

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Two millisecond pulsars, PSR J1513-2550 and PSR J2017-1614, with spin periods of about 2.1 and 2.3 ms were recently discovered in the radio and gamma-rays and classified as black widow pulsars in tight binary stellar systems with orbital periods of about 4.3 and 2.3 h. Aims. Our goals are to reveal the fundamental parameters of both systems and their binary components using multi-wavelength observations. Methods. We carried out the first time-series multi-band optical photometry of the objects with the 2.1-m telescope of the Observatorio Astronomico Nacional San Pedro Martir, the 6.5-m Magellan-1 telescope, and the 10.4-m Gran Telescopio Canarias. To derive the parameters of both systems, we fitted the obtained light curves with a model assuming heating of the companion by the pulsar. We also analysed archival X-ray data obtained with the XMM-Newton observatory. Results. For the first time, we firmly identified J1513-2550 in the optical and both pulsars in X-rays. The optical light curves of both systems have a single peak per orbital period with a peak-to-peak amplitude of greater than or similar to 2 magnitudes. The J2017-1614 light curves are symmetric, while J1513-2550 demonstrates strong asymmetry whose nature remains unclear. Conclusions. We constrained the orbital inclinations, pulsar masses, companion temperatures and masses, and the distances to both systems. We also conclude that J2017-1614 may contain a massive neutron star of 2.4 +/- 0.6 M-circle dot. The X-ray spectra of both sources can be fitted by power laws with parameters typical of black widow systems.

引用

页数：9

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