High-energy neutrino emission from x-ray binaries

被引：36

作者：

Christiansen, HR

Orellana, M

Romero, GE

机构：

[1] Univ Estadual Ceara, Dept Phys, BR-60740000 Fortaleza, Ceara, Brazil

[2] IAR, RA-1894 Villa Elisa, Bsas, Argentina

来源：

PHYSICAL REVIEW D | 2006年 / 73卷 / 06期

关键词：

D O I：

10.1103/PhysRevD.73.063012

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We show that high-energy neutrinos can be efficiently produced in X-ray binaries with relativistic jets and high-mass primary stars. We consider a system where the star presents a dense equatorial wind and the jet has a small content of relativistic protons. In this scenario, neutrinos and correlated gamma-rays result from pp interactions and the subsequent pion decays. As a particular example we consider the microquasar LS I +61 303. Above 1 TeV, we obtain a mean-orbital nu(mu)-luminosity of similar to 5 10(34) erg/s which can be related to an event rate of 4-5 muon-type neutrinos per kilometer-squared per year after considering the signal attenuation due to maximal neutrino oscillations. The maximal neutrino energies here considered will range between 20 and 85 TeV along the orbit. The local infrared photon field is responsible for opacity effects on the associated gamma radiation at high energies, but below 50 GeV the source could be detected by MAGIC telescope. GLAST observations at E-gamma > 100 MeV should also reveal a strong source.

引用

页数：10

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