A model for LSI 61 303
Open Access
- 1 January 1981
- journal article
- Published by Oxford University Press (OUP) in Monthly Notices of the Royal Astronomical Society
- Vol. 194 (1) , 1P-5P
- https://doi.org/10.1093/mnras/194.1.1p
Abstract
The radio star LSI 61° 303 is an unusual object possibly associated with the γ-ray source CG 135. The recently observed radio periodicity of 26 day strongly suggests that the system is a binary. Here we propose that the invisible companion is a relatively young pulsar (of age 104–105 yr) losing energy via a relativistic wind. At the boundary between the pulsar wind and the stellar wind of the primary, the dominant energy-loss for relativistic electrons is Compton-scattering off the optical photons of the primary, which should account for the X-ray to γ-ray emission, while synchrotron radiation from the same electrons would explain the radio emission. If the source radiates 1037 ergs−1 in the MeV band, as suggested by the observations by Perotti et al., a very high efficiency of production of 1-GeV electrons by the pulsar is required, which agrees with the expectations of some pulsar models. A substantial orbital eccentricity is expected.Keywords
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