Analytical light curve models of superluminous supernovae: χ2-minimization of parameter fits

E. Chatzopoulos, J. Craig Wheeler, J. Vinkó, Z. L. Horvath, A. Nagy

Research output: Contribution to journalArticle

97 Citations (Scopus)

Abstract

We present fits of generalized semi-analytic supernova (SN) light curve (LC) models for a variety of power inputs including 56Ni and 56Co radioactive decay, magnetar spin-down, and forward and reverse shock heating due to supernova ejecta-circumstellar matter (CSM) interaction. We apply our models to the observed LCs of the H-rich superluminous supernovae (SLSN-II) SN 2006gy, SN 2006tf, SN 2008am, SN 2008es, CSS100217, the H-poor SLSN-I SN 2005ap, SCP06F6, SN 2007bi, SN 2010gx, and SN 2010kd, as well as to the interacting SN 2008iy and PTF 09uj. Our goal is to determine the dominant mechanism that powers the LCs of these extraordinary events and the physical conditions involved in each case. We also present a comparison of our semi-analytical results with recent results from numerical radiation hydrodynamics calculations in the particular case of SN 2006gy in order to explore the strengths and weaknesses of our models. We find that CS shock heating produced by ejecta-CSM interaction provides a better fit to the LCs of most of the events we examine. We discuss the possibility that collision of supernova ejecta with hydrogen-deficient CSM accounts for some of the hydrogen-deficient SLSNe (SLSN-I) and may be a plausible explanation for the explosion mechanism of SN 2007bi, the pair-instability supernova candidate. We characterize and discuss issues of parameter degeneracy.

Original languageEnglish
Article number76
JournalAstrophysical Journal
Volume773
Issue number1
DOIs
Publication statusPublished - Aug 10 2013

Fingerprint

ejecta
light curve
supernovae
optimization
hydrogen
heating
radioactive decay
explosion
collision
stellar envelopes
hydrodynamics
shock heating
parameter
magnetars
explosions

Keywords

  • circumstellar matter
  • stars: evolution
  • stars: mass-loss
  • supernovae: general

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics
  • Nuclear and High Energy Physics

Cite this

Analytical light curve models of superluminous supernovae : χ2-minimization of parameter fits. / Chatzopoulos, E.; Wheeler, J. Craig; Vinkó, J.; Horvath, Z. L.; Nagy, A.

In: Astrophysical Journal, Vol. 773, No. 1, 76, 10.08.2013.

Research output: Contribution to journalArticle

Chatzopoulos, E. ; Wheeler, J. Craig ; Vinkó, J. ; Horvath, Z. L. ; Nagy, A. / Analytical light curve models of superluminous supernovae : χ2-minimization of parameter fits. In: Astrophysical Journal. 2013 ; Vol. 773, No. 1.
@article{3ddc55d59331434da8fe4c84e3bbba0a,
title = "Analytical light curve models of superluminous supernovae: χ2-minimization of parameter fits",
abstract = "We present fits of generalized semi-analytic supernova (SN) light curve (LC) models for a variety of power inputs including 56Ni and 56Co radioactive decay, magnetar spin-down, and forward and reverse shock heating due to supernova ejecta-circumstellar matter (CSM) interaction. We apply our models to the observed LCs of the H-rich superluminous supernovae (SLSN-II) SN 2006gy, SN 2006tf, SN 2008am, SN 2008es, CSS100217, the H-poor SLSN-I SN 2005ap, SCP06F6, SN 2007bi, SN 2010gx, and SN 2010kd, as well as to the interacting SN 2008iy and PTF 09uj. Our goal is to determine the dominant mechanism that powers the LCs of these extraordinary events and the physical conditions involved in each case. We also present a comparison of our semi-analytical results with recent results from numerical radiation hydrodynamics calculations in the particular case of SN 2006gy in order to explore the strengths and weaknesses of our models. We find that CS shock heating produced by ejecta-CSM interaction provides a better fit to the LCs of most of the events we examine. We discuss the possibility that collision of supernova ejecta with hydrogen-deficient CSM accounts for some of the hydrogen-deficient SLSNe (SLSN-I) and may be a plausible explanation for the explosion mechanism of SN 2007bi, the pair-instability supernova candidate. We characterize and discuss issues of parameter degeneracy.",
keywords = "circumstellar matter, stars: evolution, stars: mass-loss, supernovae: general",
author = "E. Chatzopoulos and Wheeler, {J. Craig} and J. Vink{\'o} and Horvath, {Z. L.} and A. Nagy",
year = "2013",
month = "8",
day = "10",
doi = "10.1088/0004-637X/773/1/76",
language = "English",
volume = "773",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "1",

}

TY - JOUR

T1 - Analytical light curve models of superluminous supernovae

T2 - χ2-minimization of parameter fits

AU - Chatzopoulos, E.

AU - Wheeler, J. Craig

AU - Vinkó, J.

AU - Horvath, Z. L.

AU - Nagy, A.

PY - 2013/8/10

Y1 - 2013/8/10

N2 - We present fits of generalized semi-analytic supernova (SN) light curve (LC) models for a variety of power inputs including 56Ni and 56Co radioactive decay, magnetar spin-down, and forward and reverse shock heating due to supernova ejecta-circumstellar matter (CSM) interaction. We apply our models to the observed LCs of the H-rich superluminous supernovae (SLSN-II) SN 2006gy, SN 2006tf, SN 2008am, SN 2008es, CSS100217, the H-poor SLSN-I SN 2005ap, SCP06F6, SN 2007bi, SN 2010gx, and SN 2010kd, as well as to the interacting SN 2008iy and PTF 09uj. Our goal is to determine the dominant mechanism that powers the LCs of these extraordinary events and the physical conditions involved in each case. We also present a comparison of our semi-analytical results with recent results from numerical radiation hydrodynamics calculations in the particular case of SN 2006gy in order to explore the strengths and weaknesses of our models. We find that CS shock heating produced by ejecta-CSM interaction provides a better fit to the LCs of most of the events we examine. We discuss the possibility that collision of supernova ejecta with hydrogen-deficient CSM accounts for some of the hydrogen-deficient SLSNe (SLSN-I) and may be a plausible explanation for the explosion mechanism of SN 2007bi, the pair-instability supernova candidate. We characterize and discuss issues of parameter degeneracy.

AB - We present fits of generalized semi-analytic supernova (SN) light curve (LC) models for a variety of power inputs including 56Ni and 56Co radioactive decay, magnetar spin-down, and forward and reverse shock heating due to supernova ejecta-circumstellar matter (CSM) interaction. We apply our models to the observed LCs of the H-rich superluminous supernovae (SLSN-II) SN 2006gy, SN 2006tf, SN 2008am, SN 2008es, CSS100217, the H-poor SLSN-I SN 2005ap, SCP06F6, SN 2007bi, SN 2010gx, and SN 2010kd, as well as to the interacting SN 2008iy and PTF 09uj. Our goal is to determine the dominant mechanism that powers the LCs of these extraordinary events and the physical conditions involved in each case. We also present a comparison of our semi-analytical results with recent results from numerical radiation hydrodynamics calculations in the particular case of SN 2006gy in order to explore the strengths and weaknesses of our models. We find that CS shock heating produced by ejecta-CSM interaction provides a better fit to the LCs of most of the events we examine. We discuss the possibility that collision of supernova ejecta with hydrogen-deficient CSM accounts for some of the hydrogen-deficient SLSNe (SLSN-I) and may be a plausible explanation for the explosion mechanism of SN 2007bi, the pair-instability supernova candidate. We characterize and discuss issues of parameter degeneracy.

KW - circumstellar matter

KW - stars: evolution

KW - stars: mass-loss

KW - supernovae: general

UR - http://www.scopus.com/inward/record.url?scp=84881160056&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84881160056&partnerID=8YFLogxK

U2 - 10.1088/0004-637X/773/1/76

DO - 10.1088/0004-637X/773/1/76

M3 - Article

AN - SCOPUS:84881160056

VL - 773

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1

M1 - 76

ER -