X-ray synchrotron emission from 10-100 TeV cosmic-ray electrons in the supernova remnant SN 1006

被引:72
|
作者
Allen, GE
Petre, R
Gotthelf, EV
机构
[1] MIT, Ctr Space Res, Cambridge, MA 02139 USA
[2] NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA
[3] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA
来源
ASTROPHYSICAL JOURNAL | 2001年 / 558卷 / 02期
关键词
acceleration of particles; cosmic rays; ISM : individual (SN 1006); radiation mechanisms : nonthermal; supernova remnants; X-rays : general;
D O I
10.1086/322470
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present the results of a joint spectral analysis of RXTE PCA, ASCA SIS, and ROSAT PSPC data of the supernova remnant SN 1006. This work represents the first attempt to model both the thermal and nonthermal X-ray emission over the entire X-ray energy band from 0.12 to 17 keV. The thermal flux is described by a nonequilibrium ionization model with an electron temperature kT(e) = 0.6 keV, an ionization timescale n(0)t = 9x10(9) cm(-3) s, and a relative elemental abundance of silicon that is 10-18 times larger than the solar abundance. The nonthermal X-ray spectrum is described by a broken power law model with low- and high-energy photon indices Gamma (1) = 2.1 and Gamma (2) = 3.0, respectively. Since the non- thermal X-ray spectrum steepens with increasing energy, the results of the present analysis corroborate previous claims that the nonthermal X-ray emission is produced by synchrotron radiation. We argue that the magnetic field strength is significantly larger than previous estimates of about 10 muG and arbitrarily use a value of 40 muG to estimate the parameters of the cosmic-ray electron, proton, and helium spectra of the remnant. The results for the ratio of the number densities of protons and electrons (R=160 at 1 GeV), the total energy in cosmic rays (E-cr = 1x10(50) ergs), and the spectral index of the electrons at 1 GeV (Gamma (e) = 2.14 +/-0.12) are consistent with the hypothesis that Galactic cosmic rays are accelerated predominantly in the shocks of supernova remnants. Yet, the remnant may or may not accelerate nuclei to energies as high as the energy of the "knee" depending on the reason why the maximum energy of the electrons is only 10 TeV.
引用
收藏
页码:739 / 752
页数:14
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