Computer Science
Scientific paper
Jan 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004phdt........26b&link_type=abstract
Ph.D. thesis, Kyoto University Japan, 2004, ISAS research note 777
Computer Science
5
Scientific paper
We present the first results of a systematic spatial and spectral X-ray study of small scale structures on the shock of five supernova remnants (Cas A, Kepler, Tycho, SN 1006, and RCW 86) and a super bubble (30 Dor C), with excellent spatial resolution of the Chandra X-ray observatory. All targets have synchrotron X-ray emission which concentrate on a very narrow region of the outer edge of the shock. The scale length of the region emitting synchrotron X-rays is incredibly small, less than 1% of the radius of the system both in the upstream and the downstream, in which smaller lengths are seen in the upstream than in the downstream. Together with the information of wide band spectra from radio to X-ray, both age-limited and loss-limited assumptions are checked for the acceleration history of all the SNRs. We found a possible magnetic field strength and configuration, and the maximum energy of accelerated electrons have been estimated for each target. The perpendicular magnetic field to the shock normal is accepted in all SNR cases, with highly turbulent magnetic field downstream.
Comparing the samples, we found that the scale length of shocks grows as its age increases, in the same rate of Sedov similar solution for upstream (∝ t4/5) and in a faster rate for downstream (∝ t1/2). The energy density of magnetic field and cosmic rays evolve keeping an equipartition with the thermal and kinetic energies of the shock (∝ t-6/5) under the assumption that the system is in the age-limited case, implying that there are strong energy interaction between kinetic, thermal, magnetic field, and cosmic ray energy densities. The magnetic field is always near to perpendicular. These are the first results to estimate observationally the magnetic field and its direction, energy density of magnetic field and cosmic rays, and their evolutions.
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