Supernova Remnants at High Energy

By S. Reynolds. 2008

349 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/c4075ade06d52a050cd56decb30afb7f598d089a

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. D. M. Alexander
2. W. N. Brandt
3. Bing Zhang
4. A. C. Fabian
5. J. Vink
6. F. E. Bauer
7. N. Smith
8. A. Comastri

In Nuclear and High Energy Physics

1. D. M. Alexander
2. W. N. Brandt
3. J. Vink
4. E. Orlando
5. F. E. Bauer
6. S. Reynolds
7. S. Puccetti
8. B. Gaensler

Citations in the corpus

• DIFFUSIVE SHOCK ACCELERATION SIMULATIONS OF RADIO RELICS (2012, background): “Observationally, the ratio of CR electron number to proton number, Ke/p ∼ 0.01, is commonly inferred for strong supernova remnant shocks, since about 1% of the Galactic CR flux near a GeV is due to electrons (Reynolds 2008).”
• MAXIMALLY STAR-FORMING GALACTIC DISKS. I. STARBURST REGULATION VIA FEEDBACK-DRIVEN TURBULENCE (2011, neutral): “Taking ζcr ∼ 0.1 (Reynolds 2008), vA ∼ 10 km s−1, and ESN = 1051 erg, (ESNζcr)/(2vAm∗) = 2500 km s−1; this is comparable to the kinetic input p∗/m∗ from supernovae.”
• Sensitivity of the high altitude water Cherenkov detector to sources of multi-TeV gamma rays (2013, neutral): “As a specific example, the TeV emission from the SNR IC 443 measured The sensitivity is found by calculating the flux needed for a 5 σ detection for quarter-decade energy bins using Eqn.”
• THE NUCLEAR SPECTROSCOPIC TELESCOPE ARRAY (NuSTAR) HIGH-ENERGY X-RAY MISSION (2013, background): “All Galactic SNRs less than 2000 yr old, and some older examples, show evidence of synchrotron X-ray emission (Reynolds 2008; Allen, Gotthelf, & Petre 1999).”
• A Markov Chain Monte Carlo technique to sample transport and source parameters of Galactic cosmic rays - II. Results for the diffusion model combining B/C and radioactive nuclei (2010, background): “…Ptuskin et al. 2006; Minnie et al. 2007; Tautz et al. 2008, Yan & Lazarian 2008 and references therein), or related to the source spectra predicted in acceleration models (e.g., Marcowith et al. 2006; Uchiyama et al. 2007; Plaga 2008; Reville et al. 2008, Reynolds 2008 and references therein).”
• Magnetic Fields in Supernova Remnants and Pulsar-Wind Nebulae (2011, methodology): “…radio emission from adiabatic-phase SNRs, with low shock compression ratios, indicates that particle acceleration must be ongoing; simple compression of ambient Galactic magnetic field and cosmic-ray electrons would produce both insufficiently bright emission and the wrong spectrum (Reynolds 2008).”
• The Youngest Galactic Supernova Remnant: G1.9+0.3 (2008, methodology): “9 0.3, using results quoted in Reynolds (2008).”
• Supernova remnants: the X-ray perspective (2011, background): “Type Ib and Ic supernovae are now understood to be explosions of stars that have lost their hydrogen-rich envelope as a result of stellar wind mass loss (e.g. Heger et al., 1But see Vink (2006); Reynolds (2008); Badenes (2010) for recent, more topical reviews.”
• NEUTRAL PION EMISSION FROM ACCELERATED PROTONS IN THE SUPERNOVA REMNANT W44 (2011, background): “…the spectral index found in this analysis is quite steep in comparison with the expectations for the spectrum of particles accelerated in SNRs (e.g. Reynolds 2008) and that the cosmic-ray spectrum can be altered (softened) by the interaction with sites where the target gas is confined, for example…”
• Observational Signatures of Particle Acceleration in Supernova Remnants (2012, background): “3 (Reynolds, 2008; Borkowski et al., 2010; Carlton et al., 2011) it seems likely that the spectrum is age- rather than loss limited.”
• Teraelectronvolt Astronomy (2010, background): “…energies achievable in supernova shocks of age 1000 t3 yr are of order Emax ∼ u28t3BµGTeV (2) where u8 is the shock speed in units of 1000 km s −1 (e.g. Reynolds (2008)); for electrons, synchrotron losses limit the peak energy to Emax ∼ 100u8B−1/2µG TeV (3) See Zirakashvili & Aharonian (2007).”
• FERMI LAT DISCOVERY OF EXTENDED GAMMA-RAY EMISSION IN THE DIRECTION OF SUPERNOVA REMNANT W51C (2009, background): “This conjecture has been strengthened by recent observations of young SNRs in synchrotron X-rays and very-high-energy (VHE) gamma-rays (see e.g., Reynolds 2008; Aharonian et al. 2008).”
• Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars (2014, background): “Shock fronts in their beautifully complex SN remnants echo through the ISM for thousands of years after the bright SN display has faded (Reynolds 2008).”