Are models for core-collapse supernova progenitors consistent with the properties of supernova remnants?

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

DOI:https://doi.org/10.1088/0004-637X/803/2/101· OSTI ID:22883264

Patnaude, Daniel J.; Slane, Patrick O. ^[1]; Lee, Shiu-Hang ^[2]; Badenes, Carles ^[3]; Heger, Alexander ^[4]; Ellison, Donald C. ^[5]; Nagataki, Shigehiro ^[6]

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1. Smithsonian Astrophysical Observatory, Cambridge, MA 02138 (United States)
2. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252-5210 (Japan)
3. Department of Physics and Astronomy and Pittsburgh Particle Physics, Astrophysics and Cosmology Center (PITT PACC), University of Pittsburgh, 3941 O’Hara Street, Pittsburgh, PA 15260 (United States)
4. Monash Center for Astrophysics, School of Mathematical Sciences, Building 28, Monash University, Vic 3800 (Australia)
5. Physics Department, North Carolina State University, Box 8202, Raleigh, NC 27695 (United States)
6. RIKEN, Astrophysical Big Bang Laboratory, 2-1 Hirosawa, Wako, Saitama 351-0198 (Japan)

The recent discovery that the Fe–K line luminosities and energy centroids observed in nearby supernova remnants are a strong discriminant of both progenitor type and circumstellar environment has implications for our understanding of supernova progenitor evolution. Using models for the chemical composition of core-collapse supernova (CCSN) ejecta, we model the dynamics and thermal X-ray emission from shocked ejecta and circumstellar material, modeled as an r{sup −2} wind, to ages of 3000 yr. We compare the X-ray spectra expected from these models to observations made with the Suzaku satellite. We also model the dynamics and X-ray emission from Type Ia progenitor models. We find a clear distinction in Fe–K line energy centroid between core-collapse and Type Ia models. The CCSN models predict higher Fe–K line centroid energies than the Type Ia models, in agreement with observations. We argue that the higher line centroids are a consequence of the increased densities found in the circumstellar environment created by the expansion of the slow-moving wind from the massive progenitors.

• OSTI ID: 22883264
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 2 Vol. 803; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United Kingdom
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
COMPARATIVE EVALUATIONS
DENSITY
EMISSION
EXPANSION
LUMINOSITY
MASS TRANSFER
SATELLITES
STAR EVOLUTION
STELLAR WINDS
SUPERNOVA REMNANTS
TYPE I SUPERNOVAE
X-RAY SPECTRA