Gamma-Ray Emission Concurrent with the Nova in the Symbiotic Binary V407 Cygni

Details Gamma-Ray Emission Concurrent with the Nova in the Symbiotic Binary V407 Cygni Gamma-Ray Emission Concurrent with the Nova in the Symbiotic Binary V407 Cygni

2010-08-23

arxiv.org/abs/1008.3912v1

Science 329: 817-821, 2010

Astronomy and Astrophysics

Astrophysics

High Energy Astrophysical Phenomena

38 pages, includes Supplementary Online Material; corresponding authors: C.C. Cheung, A.B. Hill, P. Jean, S. Razzaque, K.S. Wo

Scientific paper

10.1126/science.1192537

Novae are thermonuclear explosions on a white dwarf surface fueled by mass accreted from a companion star. Current physical models posit that shocked expanding gas from the nova shell can produce X-ray emission but emission at higher energies has not been widely expected. Here, we report the Fermi Large Area Telescope detection of variable gamma-ray (0.1-10 GeV) emission from the recently-detected optical nova of the symbiotic star V407 Cygni. We propose that the material of the nova shell interacts with the dense ambient medium of the red giant primary, and that particles can be accelerated effectively to produce pi0 decay gamma-rays from proton-proton interactions. Emission involving inverse Compton scattering of the red giant radiation is also considered and is not ruled out.

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