Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...254..167k&link_type=abstract
Astronomy and Astrophysics, Vol.254, NO. FEB(I), P. 167, 1992
Astronomy and Astrophysics
Astrophysics
11
Scientific paper
A model is presented to explain the radio flare observed from SN 1987A two days after explosion. The radiation mechanism is assumed to be synchrotron radiation from a population of relativistic electrons which are accelerated by multiple reflection from the supernova shock front. Multiple reflection occurs because the progenitor's stellar wind contains a magnetic field wound into the form of a spiral by stellar rotation; because the spiral becomes ever more tightly wound as the shock progresses outwards, reflected electrons are unable to escape ahead of the shock front. Eventually, when the spiral becomes so tightly wound that the shock is `superluminal' the accelerated electrons are overtaken and pass into the turbulent downstream medium. For parameters appropriate for SN 1987A, this occurs after 2 - 3 days. The radiation observed at about this time is emitted by the accelerated electrons after they have been overtaken by the shock and isotropised by the downstream turbulence. The decay of the flare is a result of adiabatic losses in the expanding downstream plasma. The predicted spectrum is a power law I is proportional to ν^-1^ the synchrotron self-absorption frequency, consistent with observation. We identify the flattening of the observed spectrum with the self-absorption turnover and find a magnetic field strength of about 400 mG. The observed peak flux of ~150 mJy is produced solely by electrons swept up by the shock from the hot plasma surrounding the progenitor. Although other injection mechanisms may operate, they are not essential to the model.
Kirk John G.
Wassmann Marko
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