The Library
Superluminous x-rays from a superluminous supernova
Tools
Levan, Andrew J., Read, A. M., Metzger, B. D., Wheatley, P. J. and Tanvir, N. R. (2013) Superluminous x-rays from a superluminous supernova. The Astrophysical Journal, Volume 771 (Number 2). Article number 136. doi:10.1088/0004-637X/771/2/136 ISSN 0004-637X.
Research output not available from this repository.
Request-a-Copy directly from author or use local Library Get it For Me service.
Official URL: http://dx.doi.org/10.1088/0004-637X/771/2/136
Abstract
The discovery of a population of superluminous supernovae (SLSNe), with peak luminosities a factor of ~100 brighter than normal supernovae (SNe; typically SLSNe have MV < ā21), has shown an unexpected diversity in core-collapse SN properties. Numerous models have been postulated for the nature of these events, including a strong interaction of the shockwave with a dense circumstellar environment, a re-energizing of the outflow via a central engine, or an origin in the catastrophic destruction of the star following a loss of pressure due to pair production in an extremely massive stellar core (so-called pair instability SNe). Here we consider constraints that can be placed on the explosion mechanism of hydrogen-poor SLSNe (SLSNe-I) via X-ray observations, with XMM-Newton, Chandra, and Swift, and show that at least one SLSN-I is likely the brightest X-ray SN ever observed, with LX ~ 1045 erg sā1, ~150 days after its initial discovery. This is a luminosity three orders of magnitude higher than seen in other X-ray SNe powered via circumstellar interactions. Such high X-ray luminosities are sufficient to ionize the ejecta and markedly reduce the optical depth, making it possible to see deep into the ejecta and any source of emission that resides there. Alternatively, an engine could have powered a moderately relativistic jet external to the ejecta, similar to those seen in gamma-ray bursts. If the detection of X-rays does require an engine it implies that these SNe do create compact objects, and that the stars are not completely destroyed in a pair instability event. Future observations will determine which, if any, of these mechanisms are at play in SLSNe.
Item Type: | Journal Article | ||||
---|---|---|---|---|---|
Divisions: | Faculty of Science, Engineering and Medicine > Science > Physics | ||||
Journal or Publication Title: | The Astrophysical Journal | ||||
Publisher: | Institute of Physics Publishing, Inc. | ||||
ISSN: | 0004-637X | ||||
Official Date: | 2013 | ||||
Dates: |
|
||||
Volume: | Volume 771 | ||||
Number: | Number 2 | ||||
Page Range: | Article number 136 | ||||
DOI: | 10.1088/0004-637X/771/2/136 | ||||
Status: | Peer Reviewed | ||||
Publication Status: | Published | ||||
Access rights to Published version: | Restricted or Subscription Access |
Request changes or add full text files to a record
Repository staff actions (login required)
View Item |