2016/03/30 by L. Saha, V. R. Chitnis, A. Shukla +2 · 10 citations
Physics and Astronomy · #Amplitude #Astrophysical Phenomena and Observations #Astrophysics and Cosmic Phenomena #Binary number #Binary star #Dark Matter and Cosmic Phenomena #Function (biology) #Jet (fluid) #Light curve #Matrix (chemical analysis) #Phase (matter) #X-ray binary #astro-ph.HE
paper · pdf · doi:10.3847/0004-637x/823/2/134
published in The Astrophysical Journal 823(2), 134 (IOP Publishing) · 10 pages, 7 figures, accepted for publication in ApJ
arxiv created 2016/03/30 · openalex publication_date 2016/05/31 · openalex created_date 2016/06/24 · arxiv updated 2018/03/08 · openalex updated_date 2026/08/06
ABSTRACT We study the characteristics of the TeV binary LS I+61°303 in radio, soft X-ray, hard X-ray, and gamma-ray (GeV and TeV) energies. The long-term variability characteristics are examined as a function of the phase of the binary period of 26.496 days as well as the phase of the superorbital period of 1626 days, dividing the observations into a matrix of 10 × 10 phases of these two periods. We find that the long-term variability can be described by a sine function of the superorbital period, with the phase and amplitude systematically varying with the binary period phase. We also find a definite wavelength-dependent change in this variability description. To understand the radiation mechanism, we define three states in the orbital/superorbital phase matrix and examine the wideband spectral energy distribution. The derived source parameters indicate that the emission geometry is dominated by a jet structure showing a systematic variation with the orbital/superorbital period. We suggest that LS I+61°303 is likely a microquasar with a steady jet.