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American Association for the Advancement of Science, Science, 5993(329), p. 817-821, 2010

DOI: 10.1126/science.1192537

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

Journal article published in 2010 by Ö. Çelik, A.~A A.; /Naval Research Lab Wash D. C. /Natl R.-E.-S. Coun D. C.;Ackermann M.; /KIPAC Menlo Park /SLAC;Ajello Park /SLAC;Atwood W. B.; /UC Santa Cruz;Baldini L.; /INFN Pisa;Ballet J.; /DAPNIA Saclay;Barbiellini G.; /INFN Trieste /Tries Abdo, Y. Thayer, L. Torres, G. Tramacere, A. Uchiyama, Y. Uchiyama, Y. Usher, M. Ackermann ORCID, Vandenbroucke T. L., M. Ajello, Ł. Stawarz, E. Wang, W.~B B. Atwood, P. Wang and other authors.
This paper is available in a repository.
This paper is available in a repository.

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Data provided by SHERPA/RoMEO

Abstract

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 emission (0.1 to 10 billion electron volts) 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 pi(0) 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. Z9 0