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
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DOI：
10.1126/science.1192537
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发表时间：
2010-08-13
期刊：
影响因子：
56.9
通讯作者：
Yamanaka, M.
中科院分区：
文献类型：
--
作者：
Abdo, A. A.;Ackermann, M.;Yamanaka, M.
新星是白矮星表面上的热核爆炸，由伴星的质量吸积而成。目前的物理模型假设，新星壳层中受到冲击的膨胀气体可以产生x射线发射，但人们并没有普遍预期到更高能量的发射。在这里，我们报告了费米广域望远镜对最近探测到的共生星V407天鹅座光学新星的可变伽马射线发射(0.1到100亿电子伏特)的探测。我们认为，新星壳层的物质与红巨星原核致密的环境介质相互作用，粒子可以被有效地加速，从而从质子-质子相互作用中产生pi(0)衰变伽马射线。还考虑了红巨星辐射的逆康普顿散射发射，不排除这种情况。
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.