1997/10/02 by Paul S. Ray, P. S. Ray, R. S. Foster +4 · 43 citations
Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Cosmic Phenomena #Compact star #Ephemeris #Flux (metallurgy) #Gamma-ray bursts and supernovae #Neutron star #Orbital period #Physics #Radio spectrum #Satellite #Spectral index #Spectral line #Stars #astro-ph
paper · pdf · doi:10.1086/304923
published in The Astrophysical Journal 491(1), 381-387 (IOP Publishing) · 23 pages, LaTex, 7 figures, to appear in ApJ, v491, Dec 10th issue, for associated info and preprints see http://www.srl.caltech.edu/personnel/paulr/lsi.html
arxiv created 1997/10/02 · openalex publication_date 1997/12/10 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/06
LSI +61°303 is an exotic binary system consisting of a ~10 M ☉ B star and a compact object that is probably a neutron star. The system is associated with the interesting radio source GT 0236+610, which exhibits bright radio outbursts with a period of 26.5 days. We report the results of continuous daily radio interferometric observations of GT 0236+610 at 2.25 and 8.3 GHz from 1994 January to 1996 February. The observations cover 25 complete (and three partial) cycles with multiple observations each day. We detect substantial cycle-to-cycle variability of the radio emission characterized by a rapid onset of the radio flares followed by a more gradual decrease of the emission. We detect a systematic change of the radio spectral index α (defined as S ν ∝ ν α ), which typically becomes larger than zero at the onset of the radio outbursts. This behavior is suggestive of expansion of material initially optically thick to radio frequencies, indicating either that synchrotron or inverse Compton cooling are important or that the free-free optical depth to the source is rapidly changing. After two years of observations, we see only weak evidence for the proposed 4 year periodic modulation in the peak flux of the outbursts. We observe a secular trend in the outburst phases according the best published ephemeris. This trend indicates either orbital period evolution, or a drift in outburst orbital phase in response to some other change in the system.