  The standard flare model, despite its success, is limited in comprehensively
explaining the various processes involving nonthermal particles. One such
missing ingredient is a detailed understanding of the various processes
involved during the transport of accelerated electrons from their site of
acceleration to different parts of the flare region. Here we use simultaneous
radio and X-ray observations from the Expanded Owens Valley Solar Array (EOVSA)
and Spectrometer/Telescope for Imaging X-rays (STIX) onboard the Solar Orbiter
(SolO), respectively, from two distinct viewing perspectives to study the
electron transport processes. Through detailed spectral modeling of the coronal
source using radio data and footpoint sources using X-ray spectra, we compare
the nonthermal electron distribution at the coronal and footpoint sources. We
find that the flux of nonthermal electrons precipitated at the footpoint is an
order of magnitude greater than that trapped in the looptop, consistent with
earlier works which primarily used X-ray for their studies. In addition, we
find that the electron spectral indices obtained from X-ray footpoints is
significantly softer than the spectral hardness of the nonthermal electron
distribution in the corona. We interpret these differences based on transport
effects and the difference in sensitivity of microwave and X-ray observations
to different regimes of electron energies. Such an understanding is crucial for
leveraging different diagnostic methods of nonthermal electrons simultaneously
to achieve a more comprehensive understanding of the electron acceleration and
transport processes of solar flares.
