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2013 (English)In: ASTROPHYSICAL JOURNAL LETTERS, ISSN 2041-8205, Vol. 773, no 2, L35- p.Article in journal (Refereed) Published
Abstract [en]

Gamma-ray binaries are stellar systems for which the spectral energy distribution (discounting the thermal stellar emission) peaks at high energies. Detected from radio to TeV gamma rays, the gamma-ray binary LS I + 61 degrees 303 is highly variable across all frequencies. One aspect of this system's variability is the modulation of its emission with the timescale set by the similar to 26.4960 day orbital period. Here we show that, during the time of our observations, the gamma-ray emission of LS I + 61 degrees 303 also presents a sinusoidal variability consistent with the previously known superorbital period of 1667 days. This modulation is more prominently seen at orbital phases around apastron, whereas it does not introduce a visible change close to periastron. It is also found in the appearance and disappearance of variability at the orbital period in the power spectrum of the data. This behavior could be explained by a quasi-cyclical evolution of the equatorial outflow of the Be companion star, whose features influence the conditions for generating gamma rays. These findings open the possibility to use gamma-ray observations to study the outflows of massive stars in eccentric binary systems.

Place, publisher, year, edition, pages
2013. Vol. 773, no 2, L35- p.
Keyword [en]
gamma rays: general, gamma rays: stars, stars: emission-line, Be
National Category
Astronomy, Astrophysics and Cosmology
URN: urn:nbn:se:su:diva-93560DOI: 10.1088/2041-8205/773/2/L35ISI: 000322899600018OAI: diva2:647568


Available from: 2013-09-11 Created: 2013-09-10 Last updated: 2013-09-11Bibliographically approved

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Conrad, JanLarsson, Stefan
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Department of PhysicsThe Oskar Klein Centre for Cosmo Particle Physics (OKC)Department of Astronomy
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