Please use this identifier to cite or link to this item: http://hdl.handle.net/2445/113867
Title: Orbital and superorbital variability of LS I +61 303 at low radio frequencies with GMRT and LOFAR
Author: Marcote Martin, Benito
Ribó Gomis, Marc
Paredes i Poy, Josep Maria
Ishwara-Chandra, C. H.
Swinbank, J. D.
Broderick, J. W.
Markoff, S.
Fender, R. P.
Wijers, R. A. M. J.
Pooley, G.
Stewart, A. J.
Bell, M. E.
Breton, R. P.
Carbone, D.
Corbel, S.
Eislöffel, J.
Falcke, H.
Grießmeier, J.-M.
Kuniyoshi, M.
Pietka, M.
Rowlinson, A.
Serylak, M.
Van der Horst, A. J
Van Leeuwen, J.
Wise, M. W.
Zarka, P.
Keywords: Raigs gamma
Estels binaris
Astrofísica
Gamma rays
Double stars
Astrophysics
Issue Date: 21-Feb-2016
Publisher: Royal Astronomical Society
Abstract: LS I +61 303 is a gamma-ray binary that exhibits an outburst at GHz frequencies each orbital cycle of ≈26.5 d and a superorbital modulation with a period of ≈4.6 yr. We have performed a detailed study of the low-frequency radio emission of LS I +61 303 by analysing all the archival Giant Metrewave Radio Telescope data at 150, 235 and 610 MHz, and conducting regular LOw Frequency ARray observations within the Radio Sky Monitor (RSM) at 150 MHz. We have detected the source for the first time at 150 MHz, which is also the first detection of a gamma-ray binary at such a low frequency. We have obtained the light curves of the source at 150, 235 and 610 MHz, all of them showing orbital modulation. The light curves at 235 and 610 MHz also show the existence of superorbital variability. A comparison with contemporaneous 15-GHz data shows remarkable differences with these light curves. At 15 GHz we see clear outbursts, whereas at low frequencies we see variability with wide maxima. The light curve at 235 MHz seems to be anticorrelated with the one at 610 MHz, implying a shift of ∼0.5 orbital phases in the maxima. We model the shifts between the maxima at different frequencies as due to the expansion of a one-zone emitting region assuming either free-free absorption or synchrotron self-absorption with two different magnetic field dependences. We always obtain a subrelativistic expansion velocity, in some cases being close to the stellar wind one.
Note: Reproducció del document publicat a: https://doi.org/10.1093/mnras/stv2771
It is part of: Monthly Notices of the Royal Astronomical Society, 2016, vol. 456, num. 2, p. 1791-1802
Related resource: https://doi.org/10.1093/mnras/stv2771
URI: http://hdl.handle.net/2445/113867
ISSN: 0035-8711
Appears in Collections:Articles publicats en revistes (Física Quàntica i Astrofísica)

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