Small-Scale Structure of the SN 1006 Shock with Chandra Observations

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

249 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/a3cf782462aa56e67fb04abf615ecdda64efe16e

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

In Nuclear and High Energy Physics

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

Citations in the corpus

• 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).”
• 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.”
• 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).”
• 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.…”
• 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.”
• TURBULENCE AND MAGNETIC FIELD AMPLIFICATION IN SUPERNOVA REMNANTS: INTERACTIONS BETWEEN A STRONG SHOCK WAVE AND MULTIPHASE INTERSTELLAR MEDIUM (2009, background): “The evidence for magnetic field amplification in SNR has been also obtained from the thickness of X-ray filaments that shows typicallyB ∼ 100 microGauss (Bamba et al. 2003, 2005a, 2005b; Vink & Laming 2003).”
• Nonlinear Diffusive Shock Acceleration with Magnetic Field Amplification (2006, background): “…et al. 2002), (2) broadband fits of synchrotron emission between radio and nonthermal X-rays (e.g., Berezhko et al. 2003; Völk et al. 2005; see also Cowsik & Sarkar 1980), and (3) sharp X-ray edges (e.g., Vink & Laming 2003; Bamba et al. 2003; Völk et al. 2005; Ellison&Cassam-Chenaı̈ 2005).”
• 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.”