2002/07/31 by R. S. Collins, Ross S. Collins, Christian Kaiser +3
Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Electron #Flux (metallurgy) #Gamma-ray bursts and supernovae #Infrared #Jet (fluid) #Mechanics #Physics #Pulsars and Gravitational Waves Research #astro-ph
paper · pdf · doi:10.1046/j.1365-8711.2003.06100.x
published as Mon.Not.Roy.Astron.Soc. 338 (2003) 331-339 · Accepted for publication in MNRAS, 10 pages, 10 figures, for related animations see http://www.astro.soton.ac.uk/~rsc/ckc02.html. v2: minor changes to match accepted version
arxiv created 2002/09/09 · openalex publication_date 2003/01/11 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
The variability in the infrared to millimetre emission from microquasar GRS 1915+105 is believed to be dominated by the system's relativistic jet. In this paper we develop a time-dependent version of the jet emission model of Blandford & Königl and apply it to the oscillations in the infrared and millimetre emission from GRS 1915+105 observed recently by Fender & Pooley. The resulting model provides a reasonable description of the observed flux oscillations from GRS 1915+105. From a fit of the observed time lag between the flux peaks in the infrared and millimetre emission together with the flux normalization, we were able to determine the model parameters for the GRS 1915+105 jet. We find that to achieve the observed flux levels with the model requires an unphysically large electron density within the jet. We therefore conclude that the Blandford & Königl model cannot explain these observations, either because it does not provide the correct description of the emission from microquasar jets, or because the observed emission variations do not originate in the jet.