Neutrino signals from galactic binaries

Christiansen, H. R.

doi:10.1590/s0103-97332007000400031

Cited by 1 publication

(3 citation statements)

References 41 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The spectral features should be detectable by an instrument like MAGIC and GLAST. Charged pion decay also leads to neutrino production as discussed in another work of the present meeting [1] (see also [27]). …”

Section: Discussionmentioning

confidence: 63%

“…For the energy dependent pion multiplicity we will follow the prescription adopted by Mannheim and Schlickeiser (1994) [21] ξ π (E p /GeV − 1.22) 1/4 , which should be valid up to 10 4 GeV, and adopt a softer root growing law for higher energies (see Christiansen et al (2006b) for details [27]). Under these assumptions, it can be shown that the maximum proton energy produced amounts to more than 50 PeV at periastron and lies below 15 PeV near apastron [1,27]. It can be derived from the simple argument that the Larmor radius of the particle should be smaller than the size of the acceleration region [22,23].…”

Section: Gamma Ray Luminosity and Opacitymentioning

confidence: 99%

“…As we discuss in another work of these proceedings (see Christiansen (2006a) [1]) the study of high-energy gammarays and neutrinos is expected to provide primary hints about the origin of cosmic rays.…”

mentioning

confidence: 93%

See 2 more Smart Citations

High-energy gamma-ray production in microquasars

2007

Self Cite

View full text Add to dashboard Cite

A hadronic model for gamma-ray production in microquasars is presented. Microquasars are galactic binary systems with jets, which have, presumably, hadronic components. We consider a microquasar formed by a neutron star that accretes matter from the equatorial wind of a Be primary star. The collision between the jet, emitted by the compact object, and the dense equatorial disk of the companion massive star is responsible for the gamma-ray production. Gamma-rays result from the decay of neutral pions produced in relativistic pp interactions arising from this collision all along the orbit. Assuming a simple, positional independent set of parameters, our calculations are consistent with a peak of gamma-ray flux at the periastron passage with a secondary maximum near apastron. Under this assumption, gamma-ray signals would be in contrast with the radio/X-ray outbursts which peak clearly after periastron. We finally calculate the opacity of the ambient photon field to the propagation of the gamma-rays. The spectral energy distribution appears strongly attenuated in a wide band (50 GeV -50 TeV) due to local absorption. These spectral features should be detectable by an instrument like MAGIC through exposures integrated along several periastron passages.

show abstract

Section: Discussionmentioning

confidence: 63%