POTENTIAL GAMMA-RAY EMISSIONS FROM LOW-MASS X-RAY BINARY JETS

ABSTRACT By proposing a pure leptonic radiation model, we study the potential gamma-ray emissions from the jets of low-mass X-ray binaries. In this model, the relativistic electrons that are accelerated in the jets are responsible for radiative outputs. Nevertheless, jet dynamics are dominated by ma...

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Bibliographic Details
Published in:The Astrophysical journal 2015-06, Vol.806 (2), p.1-8
Main Authors: Zhang, Jian-Fu, Gu, Wei-Min, Liu, Tong, Xue, Li, Lu, Ju-Fu
Format: Article
Language:English
Subjects:
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
Bands
BINARY STARS
COMPTON EFFECT
ELECTRONS
Emission analysis
ENERGY SPECTRA
GAMMA RADIATION
Gamma rays
gamma rays: general
GEV RANGE
JETS
KINETIC ENERGY
KINETIC EQUATIONS
MASS
Mathematical models
PROTONS
radiation mechanisms: non-thermal
RELATIVISTIC RANGE
stars: individual (GX 339-4)
SYNCHROTRON RADIATION
TELESCOPES
TEV RANGE
X RADIATION
X-ray stars
X-rays
X-rays: binaries
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Summary:ABSTRACT By proposing a pure leptonic radiation model, we study the potential gamma-ray emissions from the jets of low-mass X-ray binaries. In this model, the relativistic electrons that are accelerated in the jets are responsible for radiative outputs. Nevertheless, jet dynamics are dominated by magnetic and proton-matter kinetic energies. The model involves all kinds of related radiative processes and considers the evolution of relativistic electrons along the jet by numerically solving the kinetic equation. Numerical results show that the spectral energy distributions can extend up to TeV bands, in which synchrotron radiation and synchrotron self-Compton scattering are dominant components. As an example, we apply the model to the low-mass X-ray binary GX 339-4. The results not only can reproduce the currently available observations from GX 339-4, but also predict detectable radiation at GeV and TeV bands by the Fermi and CTA telescopes. Future observations with Fermi and CTA can be used to test our model, which could be employed to distinguish the origin of X-ray emissions.
ISSN:0004-637X
1538-4357
1538-4357
DOI:10.1088/0004-637X/806/2/168