ON COSMIC-RAY PRODUCTION EFFICIENCY AT SU0PERNOVA REMNANT SHOCKS PROPAGATING INTO REALISTIC DIFFUSE INTERSTELLAR MEDIUM

Journal Article · Mon Apr 20 04:00:00 EDT 2015 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/803/2/98· OSTI ID:22522498

Shimoda, Jiro; Ohira, Yutaka; Yamazaki, Ryo; Bamba, Aya ^[1]; Inoue, Tsuyoshi ^[2]; Vink, Jacco ^[3]

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1. Department of Physics and Mathematics, Aoyama-Gakuin University, Sagamihara, Kanagawa 252-5258 (Japan)
2. National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588 (Japan)
3. Astronomical Institute Anton Pannekoek/Gravitation and AstroParticle Physics Amsterdam (GRAPPA), University of Amsterdam, Science Park 904, NL1098 XH Amsterdam (Netherlands)

Using three-dimensional magnetohydrodynamics simulations, we show that the efficiency of cosmic-ray (CR) production in supernova remnants is over-predicted if it could be estimated based on proper motion measurements of Hα filaments in combination with shock-jump conditions. Density fluctuations of the upstream medium cause shock waves to be rippled and oblique almost everywhere. The kinetic energy of the shock wave is transferred into downstream turbulence as well as thermal energy related to the shock velocity component normal to the shock surface. Our synthetic observation shows that the CR acceleration efficiency, as estimated from a lower downstream plasma temperature, is overestimated by 10%–40% because a rippled shock does not immediately dissipate all of the upstream kinetic energy.

• OSTI ID: 22522498
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 2 Vol. 803; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
ACCELERATION
COMPUTERIZED SIMULATION
COSMIC RADIATION
COSMIC RAY PROPAGATION
DENSITY
ELECTRON TEMPERATURE
FILAMENTS
FLUCTUATIONS
ION TEMPERATURE
KINETIC ENERGY
MAGNETOHYDRODYNAMICS
PROPER MOTION
SHOCK WAVES
SUPERNOVA REMNANTS
TURBULENCE
VELOCITY