Multiwavelength coverage of the 2024 periastron passage of PSR B1259-63/LS 2883

被引：0
|
作者：
Chernyakova, M. [1 ,2 ,3 ]
Malyshev, D. [4 ]
van Soelen, B. [5 ]
Finn Gallagher, A. [1 ,2 ]
Matchett, N. [5 ]
Russell, T. D. [6 ]
van den Eijnden, J. [7 ]
Lower, M. E. [8 ]
Johnston, S. [8 ]
Tsygankov, S. [9 ]
Salganik, A. [9 ]
Shebalkova, Iu [1 ,2 ]
机构：
[1] Dublin City Univ, Sch Phys Sci, Dublin D09 W6Y4, Ireland
[2] Dublin City Univ, Ctr Astrophys & Relat, Dublin D09 W6Y4, Ireland
[3] Dublin Inst Adv Studies, 31 Fitzwilliam Pl, Dublin D02 XF86, Ireland
[4] Univ Tubingen, Inst Astron & Astrophys Tubingen, Sand 1, D-72076 Tubingen, Germany
[5] Univ Free State, Dept Phys, POB 339, ZA-9300 Bloemfontein, South Africa
[6] INAF IASF Palermo, Via Ugo Malfa 153, I-90146 Palermo, Italy
[7] Univ Warwick, Dept Phys, Coventry CV4 7AL, England
[8] CSIRO Space & Astron, Australia Telescope Natl Facil, POB 76, Epping, NSW 1710, Australia
[9] Univ Turku, Dept Phys & Astron, FI-20014 Turku, Finland
来源：
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2024年 / 536卷 / 01期
关键词：
radiation mechanisms: non-thermal; stars:; emission-line; Be; gamma-rays: general; X-rays: binaries; pulsars: individual: PSRB1259-63; X-rays: individual: PSRB1259-63; GAMMA-RAY EMISSION; PARAMETER-ESTIMATION; SYSTEM; DISCOVERY; ASTRONOMY; FLARE;
D O I：
10.1093/mnras/stae2621
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
PSR B1259-63is a gamma-ray binary system with a 48 ms radio pulsar orbiting around an O9.5Ve star, LS 2883, in a highly eccentric similar to 3.4 yr long orbit. Close to the periastron the system is detected from radio up to the TeV energies due to the interaction of the stellar wind from LS 2883 and the pulsar's relativistic outflow. Observations of the last four periastron passages, taken in 2010-2021, demonstrate periastron-to-periastron variability at all wavelengths, probably linked to the state of the Be star's decretion disc. In this paper, we present the results of our optical, radio and X-ray observational campaigns on PSR B1259-63 performed in 2024 accompanied with the analysis of the publicly available GeV Fermi/LAT data. We show that this periastron passage was characterized by the early flaring of X-rays before the periastron passage and GeV emission after the periastron passage, which can be explained by a larger size of the decretion disc as supported by the optical observations. The structure of the GeV flare is also in agreement with the disruption of the large dense disc. The possible X-ray/radio correlation was observed only during the post-periastron rise of X-ray and radio emission.
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收藏
页码：247 / 253
页数：7
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