Physics
Scientific paper
Mar 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009phdt........98y&link_type=abstract
PhD Thesis, University of Tokyo, March 2009, 164 pages.
Physics
Scientific paper
Supernova Remnants (SNR) are believed to the sites for cosmic-ray acceleration up to the knee (˜ 10^15 eV) region, and the supernova rate and efficiency of diffusive shock acceleration can account for energetics of cosmic-ray in the Galaxy. Cosmic-ray accelerators also produce gamma-rays via interaction with ambient matter and/or photon field. Thus gamma-ray observation from SNRs can provide keys to solve the mystery of cosmic ray origin. Recent advances in atmospheric Cherenkov technique have made possible to detect TeV gamma-rays from several SNRs. However, origin of gamma-ray emission from SNRs is still unclear; hadronic origin scenario favor for some SNRs, but electronic origin is not ruled out. In order to disentangle the situation, various classes of SNRs with different environment are worth studying, e.g. SNRs interacting with molecular clouds could be hadronic gamma-ray emitters since molecular clouds could act as efficient target matter for high energy proton injection. In this theses, we will pick up SNR W44, which belongs to the mixed-morphology SNR class and is linked to the interaction with dense molecular clouds as well as W28 and IC 443, which recently very high energy gamma-ray signals were reported. The coincidence of gamma-ray signals and molecular clouds is thought to be a feature of proton acceleration. A mixed-morphology supernova remnant W44 was observed by the CANGAROO-III telescopes, 25 hours in 2005 Jun and July. After standard analysis procedure, we obtained no significant gamma-ray excess but integral flux 2 σ upper limit at 1.36 TeV. Based on this result, multi-wavelength spectral analysis and energetics are studied, considering both leptonic and hadronic models.
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