scholarly journals HIGH-ENERGY EMISSION OF GRB 130427A: EVIDENCE FOR INVERSE COMPTON RADIATION

2013 ◽  
Vol 776 (2) ◽  
pp. 95 ◽  
Author(s):  
Yi-Zhong Fan ◽  
P. H. T. Tam ◽  
Fu-Wen Zhang ◽  
Yun-Feng Liang ◽  
Hao-Ning He ◽  
...  
Keyword(s):  
High Energy ◽  
Energy Emission ◽  
Inverse Compton ◽  
High Energy Emission

PULSED HIGH-ENERGY EMISSION AND PHASE-RESOLVED SPECTRA BY INVERSE COMPTON SCATTERING IN A PULSAR STRIPED WIND

2008 ◽  
Vol 17 (10) ◽  
pp. 1969-1976
Author(s):  
JÉRÔME PÉTRI ◽  
JOHN G. KIRK
Keyword(s):  
Gamma Ray ◽  
Direct Consequence ◽  
High Energy ◽  
Light Curves ◽  
Inverse Compton Scattering ◽  
Energy Emission ◽  
Inverse Compton ◽  
Pulse Structure ◽  
And Behavior ◽  
High Energy Emission

To date, seven gamma-ray pulsars are known, showing pulsed emission up to tens of GeV and associated light-curves with a double-pulse structure. We study this pulsed high-energy emission in the framework of the striped wind model. By numerical integration of the time-dependent emissivity in the current sheets, we compute the phase-dependent spectral variability of the inverse Compton radiation. Several light curves and spectra are presented. The pulses are a direct consequence of relativistic beaming. Our model is able to explain some of the high-energy (10 MeV–10 GeV) spectral features and behavior of several gamma-ray pulsars, such as Geminga and Vela.

scholarly journals MODELS FOR GAMMA-RAY PRODUCTION IN LOW-MASS MICROQUASARS

2008 ◽  
Vol 17 (10) ◽  
pp. 1903-1908 ◽  
Author(s):  
G. S. VILA ◽  
G. E. ROMERO
Keyword(s):  
Gamma Ray ◽  
High Energy ◽  
High Mass ◽  
Energy Emission ◽  
High Energy Tail ◽  
Inverse Compton ◽  
External Sources ◽  
Low Mass ◽  
High Energy Emission ◽  
Relativistic Particles

Unlike high-mass gamma-ray binaries, low-mass microquasars lack external sources of radiation and matter that could produce high-energy emission through interactions with relativistic particles. In this work, we consider the synchrotron emission of protons and leptons that populate the jet of a low-mass microquasar. In our model photohadronic and inverse Compton (IC) interactions with synchrotron photons produced by both protons and leptons result in a high-energy tail of the spectrum. We also estimate the contribution from secondary pairs injected through photopair production. The high-energy emission is dominated by radiation of hadronic origin, so we can call these objects "proton microquasars".

The prompt GRB high energy emission from internal shocks: synchrotron vs inverse Compton component

2009 ◽  
Author(s):  
Zeljka Bosnjak ◽  
Frédéric Daigne ◽  
Guillaume Dubus ◽  
Charles Meegan ◽  
Chryssa Kouveliotou ◽  
...  
Keyword(s):  
High Energy ◽  
Energy Emission ◽  
Inverse Compton ◽  
High Energy Emission

scholarly journals High Energy Emission of Symbiotic Recurrent Novae: RS Oph and V407 Cyg

2012 ◽  
Vol 21 (1-2) ◽  
Author(s):  
M. Hernanz ◽  
V. Tatischeff
Keyword(s):  
Particle Acceleration ◽  
White Dwarf ◽  
Pion Production ◽  
Supernova Remnant ◽  
High Energy ◽  
Energy Emission ◽  
Inverse Compton ◽  
Red Giant ◽  
Symbiotic Binaries ◽  
High Energy Emission

AbstractRecurrent novae occurring in symbiotic binaries are candidate sources of high energy photons, reaching GeV energies. Such emission is a consequence of particle acceleration leading to pion production. the shock between matter ejected by the white dwarf, undergoing a nova explosion, and the wind from the red giant companion are responsible for such a process, which mimics a supernova remnant but with much smaller energetic output and much shorter time scales. Inverse Compton can also be responsible for high energy emission. Recent examples are V407 Cyg, detected by Fermi, and RS Oph, which unfortunately exploded in 2006, before Fermi was launched.

High‐Energy Emission from the TeV Blazar Markarian 501 during Multiwavelength Observations in 1996

1999 ◽  
Vol 514 (1) ◽  
pp. 138-147 ◽  
Author(s):  
J. Kataoka ◽  
J. R. Mattox ◽  
J. Quinn ◽  
H. Kubo ◽  
F. Makino ◽  
...  
Keyword(s):  
High Energy ◽  
Energy Emission ◽  
High Energy Emission ◽  
Multiwavelength Observations
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