Light-curve modelling of superluminous supernova 2006gy: collision between supernova ejecta and a dense circumstellar medium

By T. Moriya, S. Blinnikov, Nozomu Tominaga, Naoki Yoshida, Masaomi Tanaka, K. Maeda, Ken'ichi Nomoto. 2012

153 citations recorded by the source corpus.

We show model light curves of superluminous supernova 2006gy on the assumption that the supernova is powered by the collision of supernova ejecta and its dense circumstellar medium. The initial conditions are constructed based on the shock breakout condition, assuming that the circumstellar medium is dense enough to cause the shock breakout within it. We perform a set of numerical light curve calculations by using a one-dimensional multigroup radiation hydrodynamics code STELLA. We succeeded in reproducing the overall features of the early light curve of SN 2006gy with the circumstellar medium whose mass is about 15 Msun (the average mass-loss rate ~ 0.1 Msun/yr). Thus, the progenitor of SN 2006gy is likely a very massive star. The density profile of the circumstellar medium is not well constrained by the light curve modeling only, but our modeling disfavors the circumstellar medium formed by steady mass loss. The ejecta mass is estimated to be comparable to or less than 15 Msun and the explosion energy is expected to be more than 4e51 erg. No 56Ni is required to explain the early light curve. We find that the multidimensional effect, e.g., the Rayleigh-Taylor instability, which is expected to take place in the cool dense shell between the supernova ejecta and the dense circumstellar medium, is important in understanding supernovae powered by the shock interaction. We also show the evolution of the optical and near-infrared model light curves of high-redshift superluminous supernovae. They can be potentially used to identify SN 2006gy-like superluminous supernovae in the future optical and near-infrared transient surveys.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/06d64445e787a928b17734c30f76186b21924f12

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Citations in the corpus

ANALYTICAL LIGHT CURVE MODELS OF SUPERLUMINOUS SUPERNOVAE: χ2-MINIMIZATION OF PARAMETER FITS (2013, methodology): “Moriya et al. (2013) noted that in the case of SN 2006gy CSM interaction is the dominant source of the input energy with any additional energy due to 56Ni and 56Co decays found to be negligible and not to contribute to any of the main features of the resulting LC.”
HIGH-DENSITY CIRCUMSTELLAR INTERACTION IN THE LUMINOUS TYPE IIn SN 2010jl: THE FIRST 1100 DAYS (2013, background): “The shock breakout for extended SNe has been discussed by several authors (Falk & Arnett 1977; Grasberg & Nadyozhin 1987; Moriya et al. 2011, 2013; Chevalier & Irwin 2011; Ginzburg & Balberg 2012).”
HYDROGEN-POOR SUPERLUMINOUS SUPERNOVAE AND LONG-DURATION GAMMA-RAY BURSTS HAVE SIMILAR HOST GALAXIES (2013, background): “…example, members of the subclass of the SLSNe that show hydrogen in their spectra can be classified as Type IIn SNe, with the origin of the extreme luminosity being interaction with a dense circumstellar medium (e.g., Ofek et al. 2007; Smith et al. 2007, 2010; Rest et al. 2011; Moriya et al. 2013).”
Spectroscopy of superluminous supernova host galaxies. A preference of hydrogen-poor events for extreme emission line galaxies (2014, background): “All SLSNe-II studied here are scaled-up SNe-IIn and their extreme luminosity can be primarily attributed to circum-stellar material (CSM) interaction (e.g. Chatzopoulos et al. 2013; Moriya et al. 2013).”
Pulsational Pair-instability Supernovae (2016, methodology): “Very few light curves of pure PPISN (i.e., PPISN without an artificial core explosion) have been calculated except for the 110 M model of Woosley et al. (2007); (e.g., Blinnikov 2010), or parametrized representations thereof (Moriya et al. 2013).”