Fine Structures of Shock of SN 1006 with the Chandra Observation

By A. Bamba, R. Yamazaki, M. Ueno, K. Koyama. 2003

183 citations recorded by the source corpus.

The north east shell of SN 1006 is the most probable acceleration site of high energy electrons (up to ~ 100 TeV) with the Fermi acceleration mechanism at the shock front. We resolved non-thermal filaments from thermal emission in the shell with the excellent spatial resolution of Chandra. The thermal component is extended widely over about ~ 100 arcsec (about 1 pc at 1.8 kpc distance) in width, consistent with the shock width derived from the Sedov solution. The spectrum is fitted with a thin thermal plasma of kT = 0.24 keV in non-equilibrium ionization (NEI), typical for a young SNR. The non-thermal filaments are likely thin sheets with the scale widths of ~ 4 arcsec (0.04 pc) and ~ 20 arcsec (0.2 pc) at upstream and downstream, respectively. The spectra of the filaments are fitted with a power-law function of index 2.1--2.3, with no significant variation from position to position. In a standard diffusive shock acceleration (DSA) model, the extremely small scale length in upstream requires the magnetic field nearly perpendicular to the shock normal. The injection efficiency (eta) from thermal to non-thermal electrons around the shock front is estimated to be ~ 1e-3 under the assumption that the magnetic field in upstream is 10 micro G. In the filaments, the energy densities of the magnetic field and non-thermal electrons are similar to each other, and both are slightly smaller than that of thermal electrons. in the same order for each other. These results suggest that the acceleration occur in more compact region with larger efficiency than previous studies.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/6bfdb9b078b1890847d5a36b7fa61902c97822e8

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Y. Fukui
2. L. Ksenofontov
3. H. Völk
4. E. Berezhko
5. Tsuyoshi Inoue
6. F. Aharonian
7. B. Gaensler
8. F. Bocchino

In Nuclear and High Energy Physics

1. L. Ksenofontov
2. H. Völk
3. E. Berezhko
4. Y. Fukui
5. F. Aharonian
6. Tsuyoshi Inoue
7. B. Gaensler
8. F. Bocchino

Citations in the corpus

• Magnetic Fields in Supernova Remnants and Pulsar-Wind Nebulae (2011, background): “Bamba et al. (2003) and Vink & Laming (2003) argued that the small radial extent resulted from synchrotron losses on electrons, to infer strong amplification of B: B ∼ 200(us/1000 km s−1)2/3(w/0.01 pc)−2/3 G (2) (Parizot et al. 2006), where w is the filament width.”
• Magnetic field amplification in Tycho and other shell-type supernova remnants (2004, methodology): “The spectra of these filaments have been found to be hard without linestructures by Bamba et al. (2003b) and by Bamba (2004), from Chandra archival data, with the conclusion that the filaments are the result of synchrotron emission.”
• Broad-band non-thermal emission from molecular clouds illuminated by cosmic rays from nearby supernova remnants (2009, background): “…support to the hadronic scenario for the gamma ray emission, comes from the observation of thin X-ray synchrotron filaments surrounding some SNRs (Bamba et al. 2003; Vink and Laming 2003; Völk et al. 2005) and of the rapid variability time scale of the synchrotron X–rays (Uchiyama et al.…”
• Confirmation of strong magnetic field amplification and nuclear cosmic ray acceleration in SN 1006 (2003, methodology): “It is important to note that there is direct experimental evidence that not only the inner part (ρ < ρm) of the brightness distribution Jν(ρ) but also the outer part (ρ > ρm) is due to emission from the downstream regionr < Rs, in contrast to the arguments of Bamba et al. (2003).”
• Interstellar Turbulence II: Implications and Effects (2004, background): “About 10−3 of the incoming thermal particles are injected into cosmic rays (Pryadko & Petrosian 1997; Kang, Jones & Gieseler 2002; Bamba et al. 2003), with an efficiency depending on obliqueness A nn u.”
• TOWARD UNDERSTANDING THE COSMIC-RAY ACCELERATION AT YOUNG SUPERNOVA REMNANTS INTERACTING WITH INTERSTELLAR CLOUDS: POSSIBLE APPLICATIONS TO RX J1713.7−3946 (2011, background): “…the magnetic field strength can be as large as B∼ 1 mG, and the thickness of the X-ray filaments indicates B∼ 100 µG around the shock front (Ballet 2006, Uchiyama et al. 2007, Tanaka et al. 2008, Acero et al. 2009), which is similar to other young SNRs (Vink & Laming 2003, Bamba et al. 2003, 2005).”