Gamma-ray sources like V407 Cygni in symbiotic stars
Gamma-ray sources like V407 Cygni in symbiotic stars
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DOI：
10.1111/j.1745-3933.2011.01021.x
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发表时间：
2011-01
影响因子：
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通讯作者：
G. Lu;Chunhua Zhu;Zhaojun Wang;W. Huo;Yuangui Yang
中科院分区：
文献类型：
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作者：
G. Lu;Chunhua Zhu;Zhaojun Wang;W. Huo;Yuangui Yang
利用一个简单的加速模型和pi(0)模型的p-p碰撞产生伽马射线的假设，我们研究了共生星中像V407天鹅座这样的伽马射线源。它们在银河系中的出现率上限为0.5~5年(-1)，表明它们可能是高能伽马射线的重要来源。加速质子的最大能量主要分布在10(11)eV左右，勉强达到10(15)eV。D型SSS中的新星具有一颗白矮星和较长的轨道周期，是伽马射线源的良好候选者。由于轨道周期短，导致加速持续时间短，共生星RS Oph中的新星不能像V407天鹅座那样产生伽马射线发射。
Using a simple accelerating model and an assumption that gamma-rays originate from p-p collisions for a pi(0) model, we investigate gamma-ray sources like V407 Cygni in symbiotic stars. The upper limit of their occurrence rate in the Galaxy is between 0.5 and 5 yr(-1), indicating that they may be important sources of high-energy gamma-rays. The maximum energies of the accelerated protons mainly distribute around 10(11) eV, and barely reach 10(15) eV. The novae occurring in D-type SSs with ONe white dwarfs and long orbital periods are good candidates for gamma-ray sources. Due to a short orbital period which results in a short acceleration duration, the nova occurring in symbiotic star RS Oph cannot produce gamma-ray emission like that in V407 Cygni.