Supernova Remnants in the Sedov Expansion Phase: Thermal X-Ray Emission

By K. Borkowski, William J. Lyerly, S. Reynolds. 2000

356 citations recorded by the source corpus.

Improved calculations of X-ray spectra for supernova remnants (SNRs) in the Sedov-Taylor phase are reported, which for the first time include reliable atomic data for Fe L-shell lines. This new set of Sedov models also allows for a partial collisionless heating of electrons at the blast wave and for energy transfer from ions to electrons through Coulomb collisions. X-ray emission calculations are based on the updated Hamilton-Sarazin spectral model. The calculated X-ray spectra are successfully interpreted in terms of three distribution functions: the electron temperature and ionization timescale distributions, and the ionization timescale-averaged electron temperature distribution. The comparison of Sedov models with a frequently used single nonequilibrium ionization (NEI) timescale model reveals that this simple model is generally not an appropriate approximation to X-ray spectra of SNRs. We find instead that plane-parallel shocks provide a useful approximation to X-ray spectra of SNRs, particularly for young SNRs. Sedov X-ray models described here, together with simpler plane shock and single-ionization timescale models, have been implemented as standard models in the widely used XSPEC v11 spectral software package.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/307e72465ca1e58839ad54a946479d78e62c859a

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. J. Vink
2. R. Yamazaki
3. C. Badenes
4. N. Langer
5. C. Rakowski
6. Utrecht
7. U. Hwang
8. T. Yoshida

In Nuclear and High Energy Physics

1. J. Vink
2. R. Yamazaki
3. C. Badenes
4. C. Rakowski
5. U. Hwang
6. T. Yoshida
7. N. Langer
8. Eduardo Bravo

Citations in the corpus

• Supernova remnant energetics and magnetars: no evidence in favour of millisecond proto-neutron stars (2006, methodology): “XSPEC contains a Sedov model (VSEDOV, Borkowski et al. 2001) that also includes non-equilibration of electron and ion temperatures, an effect that is known to be important for in particular SNRs with a short ionization age (net) and high shock velocity (Rakowski 2005).”
• A Spatial and Spectral Study of Nonthermal Filaments in Historical Supernova Remnants: Observational Results with Chandra (2004, background): “(2000)and Borkowski et al.(2001b) independently found that the hard X-rays show a nontherm alfeature,and concentrate on the south-western (SW ) shellofthe SNR.”
• Small-Scale Structure of the SN 1006 Shock with Chandra Observations (2003, unknown): “3 0.5 (Koyama et al. 1997; Slane et al. 1999; Muraishi et al. 2000; Enomoto et al. 2002), RCW 86 (Bamba, Tomida, & Koyama 2000; Borkowski et al. 2001b), and G266.”
• Constraints on the Physics of Type Ia Supernovae from the X-Ray Spectrum of the Tycho Supernova Remnant (2005, methodology): “In Papers I and II, we used the Hamilton & Sarazin (HS) code to calculate synthetic spectra (for a description of the original code and the most important updates, see Hamilton et al. 1983; Borkowski et al. 2001).”
• Are the Models for Type Ia Supernova Progenitors Consistent with the Properties of Supernova Remnants? (2007, background): “However, the values of Te and net obtained in a particular spectral fit are model dependent, and can be affected by uncertainties in the atomic data and other factors (for discussions, see Borkowski et al. 2001; Rakowski et al. 2006).”
• Cosmic-Ray Acceleration at the Forward Shock in Tycho’s Supernova Remnant: Evidence from Chandra X-Ray Observations (2005, result): “These calculations are very similar to those described in Borkowski et al. (2001) - the reader is referred to that paper for details.”