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Constraints On the Diffusive Shock Acceleration From the Nonthermal X-ray Thin Shells In SN
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Astronomy Astrophysics manuscript no. paper February 2, 2008
(DOI: will be inserted by hand later)
Constraints On the Diffusive Shock Acceleration From the
Nonthermal X-ray Thin Shells In SN 1006 NE Rim
Ryo Yamazaki1, Tatsuo Yoshida2, Toshio Terasawa3, Aya Bamba1, and Katsuji Koyama1
1 Department of Physics, Kyoto University, Kyoto 606-8502, Japan
e-mail: yamazaki@tap.scphys.kyoto-u.ac.jp , e-mail: bamba@cr.scphys.kyoto-u.ac.jp ,
e-mail: koyama@cr.scphys.kyoto-u.ac.jp
2 Faculty of Science, Ibaraki University, Mito 310-8512, Japan
e-mail: yoshidat@mx.ibaraki.ac.jp
3 Earth Planetary Science, Graduate School of Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, 113
Tokyo, Japan
e-mail: terasawa@eps.s.u-tokyo.ac.jp
Received date/ Accepted date
Abstract. Characteristic scale lengths of nonthermal X-rays from the SN 1006 NE rim, which are observed by
Chandra, are interpreted in the context of the diffusive shock acceleration on the assumption that the observed
spatial profile of nonthermal X-rays corresponds to that of accelerated electrons with energies of a few tens of
TeV. To explain the observed scale lengths, we construct two simple models with a test particle approximation,
where the maximum energy of accelerated electrons is determined by the age of SN 1006 (age-limited model)
or the energy loss (energy loss-limited model), and constrain the magnetic field configuration and the diffusion
coefficients of accelerated electrons. When the magnetic field is nearly parallel to the shock normal, the magnetic
field should be in the range of 20–85 μG and highly turbulent both in upstream and downstream, which means
that the mean free path of accelerated electrons is on the order of their gyro-radius (Bohm limit). This situation
can be realized both in the age-limited and energy loss-limited model. On the other hand, when the magnetic
field is nearly perpendicular to the shock normal, which can exist
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