AX J1910.7+0917: the slowest X-ray pulsar

作者：Sidoli L^*; Israel G L; Esposito P; Castillo G A Rodriguez; Postnov K

来源：Monthly Notices of the Royal Astronomical Society, 2017, 469(3): 3056-3061.

DOI：10.1093/mnras/stx1105

• stars: neutron
• pulsars: general
• X-rays: binaries
• X-rays: individual: AX J1910.7+0917, CXOU J191043.7+091629, 2XMM J191043.4+091629

Pulsations from the high-mass X-ray binary AX J1910.7+0917 were discovered during Chandra observations performed in 2011. We report here more details on this discovery and discuss the source nature. The period of the X-ray signal is P = 36200 +/- 110 s, with a pulsed fraction, PF, of 63 +/- 4 per cent. Given the association with a massive B-type companion star, we ascribe this long periodicity to the rotation of the neutron star (NS), making AX J1910.7+0917 the slowest known X-ray pulsar. We also report on the spectroscopy of XMM-Newton observations that serendipitously covered the source field, resulting in a highly absorbed (column density almost reaching 10(23) cm(-2)), power-law X-ray spectrum. The X-ray flux is variable on a time-scale of years, spanning a dynamic range greater than or similar to 60. The very long NS spin period can be explained within a quasi-spherical settling accretion model that applies to low luminosity, wind-fed, X-ray pulsars.

• 出版日期2017-8