TeV Gamma-Ray Emission from Vela X: Leptonic or Hadronic?

Details TeV Gamma-Ray Emission from Vela X: Leptonic or Hadronic? TeV Gamma-Ray Emission from Vela X: Leptonic or Hadronic?

Jul 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009apj...699l.153z&link_type=abstract

The Astrophysical Journal Letters, Volume 699, Issue 2, pp. L153-L156 (2009).

Astronomy and Astrophysics

Astronomy

1

Gamma Rays: Theory, Ism: Individual: Vela Nebula, Radiation Mechanisms: Non-Thermal

Scientific paper

We study nonthermal photon emission properties from Vela X in both a leptonic and a hadronic-leptonic model. In the leptonic model, it is difficult to reproduce the observed photon spectrum from X-ray to TeV bands using reasonable model parameters; the model results can compare with either the observed data at the TeV band (the total energy of electrons required to match the observations is W e ≈ 6.1 × 1045 erg) or those at the X-ray band (W e ≈ 1.3 × 1045 erg). In the hadronic-leptonic model, however, the observed photon spectrum can be reproduced in the hadronic-leptonic model and TeV photons are mainly from π0 decay in proton-proton interaction. The energy required for iron nuclei released in the pulsar wind is W Fe ≈ 2.1 × 1048 erg and the energy of iron nuclei transferred to positrons is W_e^+≈ 8.4× 10^{45} erg in this case.

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