期刊
ASTROPHYSICAL JOURNAL LETTERS
卷 736, 期 1, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/2041-8205/736/1/L10
关键词
gamma rays: stars; pulsars: individual (PSR B1259-63); radiation mechanisms: non-thermal; X-rays: binaries
资金
- HK Government [HKU700908P]
- National Science Council of the Republic of China (Taiwan) [NSC99-2112-M-007-004-MY3, NSC100-2923-M-007-001-MY3]
- Chungnam National University
The binary system PSR B1259-63/LS 2883 consists of a 47.8 ms radio pulsar that orbits the companion Be star with a period of 3.4 years in a highly eccentric orbit. The system has been well sampled in radio, X-ray, and TeV gamma-ray bands, and shows orbital phase-dependent variability in all observed frequencies. Here we report on the discovery of >100 MeV gamma-rays from PSR B1259-63/LS 2883 through the 2010 periastron passage. Using data collected with the Large Area Telescope on board Fermi from 33 days before periastron to 75 days after periastron, PSR B1259-63/LS 2883 was detected at a significance of 13.6 standard deviations. The gamma-ray light curve was highly variable over this period, with a changing photon index that correlates with the gamma-ray flux. In particular, two major flares that occur after the periastron passage were observed. The onset of gamma-ray emission occurs close to, but not at the same orbital phases as, the two disk passages that occur similar to 1 month before and similar to 1 month after the periastron passage. The fact that the GeV orbital light curve is different from that of the X-ray and TeV light curves strongly suggests that GeV gamma-ray emission originates from a different component. We speculate that the observed GeV flares may be resulting from Doppler boosting effects.
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