Future Glast Observations of Supernova Remnants and Pulsar Wind Nebulae

Details Future Glast Observations of Supernova Remnants and Pulsar Wind Nebulae Future Glast Observations of Supernova Remnants and Pulsar Wind Nebulae

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006head....9.0115f&link_type=abstract

American Astronomical Society, HEAD meeting #9, #1.15; Bulletin of the American Astronomical Society, Vol. 38, p.331

Astronomy and Astrophysics

Astronomy

Scientific paper

Supernova remnants have long been considered to be responsible to accelerate charged particles to ultra-relativistic energies in the shocks of the expanding shells. These charged particles can subsequently emit X-ray photons or Gamma-rays through interactions with magnetic fields and surrounding material. In spite of recent detailed studies in these wavebands, the nature of the parent population responsible for the gamma-ray emission remains elusive. It is not yet evident, whether the bulk of the gamma-rays are produced by Inverse Compton scattering of electrons (e.g. on the CMBR), or by hadronic interactions and subsequent pi0-decay. If the hadronic origin of the gamma-ray emission can be established, this would be a great step towards the final proof that shell-type SNRs are the long sought source of cosmic rays in the Galaxy. The upcoming GLAST Large Area Telescope (LAT) will be able to distinguish between leptonic and hadronic gamma-ray emission scenarios and we will present predictions for expected signals from these objects. In addition to the shell emission, supernova remnants containing energetic pulsars may also show bright emission from pulsar wind nebulae (PWNe). With the recent successes of TeV detection of PWNe, these promise to be an exciting source class for the LAT, as well; we comment briefly on SNR with PWN components.

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