2007A&A...473..351C

We suggest that the energy source of the observed diffuse gamma-ray emission from the direction of the Galactic center is the Galactic black hole Sgr A*, which becomes active when a star is captured at a rate of ∼10^–5yr^–1. Subsequently the star is tidally disrupted and its matter is accreted into the black hole. During the active phase relativistic protons with a characteristic energy ∼6x10⁵²erg per capture are ejected. Over 90% of these relativistic protons disappear due to proton-proton collisions on a timescale τ_pp ∼10⁴ years in the small central bulge region with radius ∼50pc within Sgr A*, where the density is ≥10³cm^–3. The gamma-ray intensity, which results from the decay of neutral pions produced by proton-proton collisions, decreases according to e^–t/τpp_^, where t is the time after last stellar capture. Less than 5% of relativistic protons escaped from the central bulge region can survive and maintain their energy for >10⁷ years due to much lower gas density outside, where the gas density can drop to ∼1cm^–3. They can diffuse to a ∼500pc region before disappearing due to proton-proton collisions. The observed diffuse GeV gamma-rays resulting from the decay of neutral pions produced via collision between these escaped protons and the gas in this region is expected to be insensitive to time in the multi-injection model with the characteristic injection rate of 10^–5yr^–1. Our model calculated GeV and 511keV gamma-ray intensities are consistent with the observed results of EGRET and INTEGRAL, however, our calculated inflight annihilation rate cannot produce sufficient intensity to explain the COMPTEL data.