Gamma-rays from the Crab Nebula and other plerions-testing MHD models

Details Gamma-rays from the Crab Nebula and other plerions-testing MHD models Gamma-rays from the Crab Nebula and other plerions-testing MHD models

Apr 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aipc..558..154d&link_type=abstract

HIGH ENERGY GAMMA-RAY ASTRONOMY: International Symposium. AIP Conference Proceedings, Volume 558, pp. 154-167 (2001).

Astronomy and Astrophysics

Astronomy

2

Supernova Remnants, Radiation Mechanisms, Polarization, Gamma-Ray

Scientific paper

A brief review of the status of γ-ray observations of plerions with their theoretical interpretations are given. This review concentrates further on the Crab Nebula, with special emphasis on the inner region near the pulsar wind shock. Two independent approaches are used to test MHD flow solutions (phenomological and a particle-in-cell approach), using the tails of the synchrotron and inverse Compton spectra, as well as information on the synchrotron surface brightness distribution: the frequency dependent underluminous inner region of the torus, as well as the terminating outer radius of this structure requires a MHD post shock flow solution where the magnetic field strength increases with radius in the torus, whereas the flow speed decreases correspondingly. We find that the solution of Kennel & Coroniti (1984) for σ=0.003 fits this constraint, and simultaneously predicts the observed multi-TeV spectrum of the Crab Nebula correctly-without any free parameters! Any MHD flow solution which predicts a constant field and flow speed inside the torus (e.g., σ~1) will fail to predict the hollow inner structure of the X-ray torus beyond the pulsar wind shock. Whereas the Kennel & Coroniti solution appears to be successful for the toroidal component (at r<0.5 pc), the same solution fails to describe the observed inverse Compton emission outside this radius, which hints at the need to develop a 2-D MHD flow solution. .

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