Speaker
Description
Hanna et al. (2010) show the 3-200 keV spectrum of the total Sun observed by RHESSI during the
quiet phase of the Sun from 2005 to 2009. A possible source of this radiation could be synchrotron
emission by Cosmic Ray Electrons (CRes). I will present results from a preliminary exploration of
this model. Several near Earth instruments have observed CRe spectra at 1 AU during quiet and active
phase of the Sun. The spectrum of the CRes at the Sun are not observed but can be evaluated by a
detailed study of the transport of CRes from 1 AU to the solar photosphere. The transport is
affected by three physical process; energy loss due to synchrotron and inverse Compton (IC), and the
magnetic field convergence and scattering by the MHD turbulence in the solar wind. There are many
observations and subsequent models for the structure of the magnetic field in the inner heliosphere
which allow to address the first two processes fairly accurately. However, the third requires a
knowledge of the energy density and spectrum of turbulence from 1 AU to the Sun. Up to recently
these characteristics of the turbulence were measured around 1 AU, but Parker Solar Probe (PSP) has
extended this knowledge to 0.17 AU. Extrapolating these observations to the Sun I will present
result on transport of CRes using a novel and simple version of Fokker Planck equation. This will
give us the spectral evolution of the CRes from 1 AU to the photosphere. The spectra at the
photosphere can then be used to calculate the synchrotron spectrum and determine how well it
reproduces the RHESSI observations.
| vahep@stanford.edu |
