SIMBAD references

2003A&A...409..581P - Astronomy and Astrophysics, volume 409, 581-588 (2003/10-2)

The imprint of Gould's Belt on the local cosmic-ray electron spectrum.

POHL M., PERROT C., GRENIER I. and DIGEL S.

Abstract (from CDS):

Recent analyses have shown that if the sources of cosmic-rays are discrete, as are supernova remnants, then the spectra of cosmic-ray electrons vary greatly with location and time and the locally measured electron spectrum may be not representative of the electron spectra elsewhere in the Galaxy. We have continued the earlier studies by investigating the impact of the star forming region Gould's Belt on the local electron spectrum at GeV to TeV energies. Our results indicate that if the electron sources in Gould's Belt are continous, the local electron spectrum would be slightly hardened with a spectral index increase of Δs≃0.07 due to the higher SN rate in the Belt. If the electron sources are discrete, which is the more probable case, the local electron spectrum above ∼30GeV is variable with similar amplitude as without Gould's Belt. By the method of Monte Carlo, we have also studied the correlation of the local electron flux with that in nearby molecular cloud complexes. The high energy electron flux above 30GeV near the Orion, Monoceros, Cassiopeia, Cepheus, and Perseus clouds does not vary in coordination with the local flux, but a correlation between the electron flux in the Taurus and Ophiuchus clouds and that in solar vicinity is indicated by our study, implying that the spatial correlation length is of the order of 200pc at electron energies of 100GeV and higher. This would permit hard γ-ray spectra from inverse Compton scattering to be produced in the more distant clouds, in agreement with the GeV excess observed towards Orion and Monoceros, without affecting the emissivity spectra of the very nearby clouds as in Taurus and Ophiuchus.

Abstract Copyright:

Journal keyword(s): ISM: cosmic rays - Galaxy: general - gamma rays: theory

Simbad objects: 10

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2020.02.19-03:35:55

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