this is for holding javascript data
Raffaella Margutti edited section_Radio_Observations_as_Probes__.tex
over 8 years ago
Commit id: 734b6f07b08859ae8bdf48a632ce082b2f166981
deletions | additions
diff --git a/section_Radio_Observations_as_Probes__.tex b/section_Radio_Observations_as_Probes__.tex
index 849a0cb..43ed1eb 100644
--- a/section_Radio_Observations_as_Probes__.tex
+++ b/section_Radio_Observations_as_Probes__.tex
...
\section{Radio Observations as Probes of Pre-SN Massloss}
The radio emission in SNe is powered by synchrotron emission due to shock-accelerated relativistic electrons gyrating in the post-shock magnetic field. The synchrotron self-absorption (SSA) or free-free absorption (FFA) at low frequencies results in a spectral turnover. The evolution of the spectral peak frequency and luminosity directly depend on the density of the environment and radius of the blast-wave. Thus, by monitoring the evolution of the radio emission resulting from the SN shock interaction with the medium, it is possible to map the density of the environment sampled by the shock. Since the SN shock is typically $\geq 30$ times faster than the progenitor stellar wind, the radio emission from a SN shock effectively acts as a time machine and allows us to sample the pre-SN life of the stellar progenitor in the centuries before the explosion. X-rays and radio emission from the SN shock interaction with the medium are currently the \emph{only} probes to sample this phase of evolution of evolved stars. We focus on the radio wavelength range as it offers the most homogeneous data set with observations covering the early- and late-time evolution of Ib/c SNe.
