PROBING FINAL STAGES of STELLAR EVOLUTION with X-RAY OBSERVATIONS of SN 2013ej

Sayan Chakraborti, Alak Ray, Randall Smith, Raffaella Margutti, David Pooley, Subhash Bose, Firoza Sutaria, Poonam Chandra, Vikram V. Dwarkadas, Stuart Ryder, Keiichi Maeda

Research output: Contribution to journalArticlepeer-review

24 Scopus citations

Abstract

Massive stars shape their surroundings with mass loss from winds during their lifetimes. Fast ejecta from supernovae (SNe), from these massive stars, shock this circumstellar medium. Emission generated by this interaction provides a window into the final stages of stellar evolution, by probing the history of mass loss from the progenitor. Here we use Chandra and Swift X-ray observations of the type II-P/L SN 2013ej to probe the history of mass loss from its progenitor. We model the observed X-rays as emission from both heated circumstellar matter and SN ejecta. The circumstellar density profile probed by the SN shock reveals a history of steady mass loss during the final 400 years. The inferred mass loss rate of points back to a 14 progenitor. Soon after the explosion we find significant absorption of reverse shock emission by a cooling shell. The column depth of this shell observed in absorption provides an independent and consistent measurement of the circumstellar density seen in emission. We also determine the efficiency of cosmic ray acceleration from X-rays produced by Inverse Compton scattering of optical photons by relativistic electrons. Only about 1% of the thermal energy is used to accelerate electrons. Our X-ray observations and modeling provide stringent tests for models of massive stellar evolution and micro-physics of shocks.

Original languageEnglish (US)
Article number22
JournalAstrophysical Journal
Volume817
Issue number1
DOIs
StatePublished - Jan 20 2016

Keywords

  • X-rays: general
  • circumstellar matter
  • shock waves
  • stars: mass-loss
  • supernovae: individual (SN 2013ej)

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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