Constraining cosmic-ray acceleration in the magnetospheric gaps of Sgr A*. (arXiv:2007.12189v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Katsoulakos_G/0/1/0/all/0/1">Grigorios Katsoulakos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rieger_F/0/1/0/all/0/1">Frank Rieger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reville_B/0/1/0/all/0/1">Brian Reville</a>
Sagittarius A* (Sgr A*) is a potential VHE gamma-ray and cosmic-ray source.
We examine limits to gap-type particle acceleration in the magnetosphere of Sgr
A*, showing that in the current phase of activity proton acceleration to PeV
energies is possible, with injection powers into the environment usually
limited to several 10^{36} erg/s. Compton upscattering of ambient soft photons
by gap-accelerated electrons could yield TeV emission compatible with the
detected VHE points source. We explore the dependency of the results on changes
in the accretion rate showing that higher stages in the past are unlikely to
increase the power output unless the inner accretion flows itself changed its
configuration.
Sagittarius A* (Sgr A*) is a potential VHE gamma-ray and cosmic-ray source.
We examine limits to gap-type particle acceleration in the magnetosphere of Sgr
A*, showing that in the current phase of activity proton acceleration to PeV
energies is possible, with injection powers into the environment usually
limited to several 10^{36} erg/s. Compton upscattering of ambient soft photons
by gap-accelerated electrons could yield TeV emission compatible with the
detected VHE points source. We explore the dependency of the results on changes
in the accretion rate showing that higher stages in the past are unlikely to
increase the power output unless the inner accretion flows itself changed its
configuration.
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