TY - GEN
T1 - Light curve modeling of superluminous supernovae
AU - Moriya, Takashi
AU - Blinnikov, Sergei I.
AU - Tominaga, Nozomu
AU - Yoshida, Naoki
AU - Tanaka, Masaomi
AU - Maeda, Keiichi
AU - Nomoto, Ken'ichi
PY - 2014/3/27
Y1 - 2014/3/27
N2 - Origins of superluminous supernovae (SLSNe) discovered by recent SN surveys are still not known well. One idea to explain the huge luminosity is the collision of dense CSM and SN ejecta. If SN ejecta is surrounded by dense CSM, the kinetic energy of SN ejecta is efficiently converted to radiation energy, making them very bright. To see how well this idea works quantitatively, we performed numerical simulations of collisions of SN ejecta and dense CSM by using one-dimensional radiation hydrodynamics code STELLA and obtained light curves (LCs) resulting from the collision. First, we show the results of our LC modeling of SLSN 2006gy. We find that physical parameters of dense CSM estimated by using the idea of shock breakout in dense CSM (e.g., Chevalier & Irwin 2011, Moriya & Tominaga 2012) can explain the LC properties of SN 2006gy well. The dense CSM's radius is about 1016 cm and its mass about 15 M ⊙. It should be ejected within a few decades before the explosion of the progenitor. We also discuss how LCs change with different CSM and SN ejecta properties and origins of the diversity of H-rich SLSNe. This can potentially be a probe to see diversities in mass-loss properties of the progenitors. Finally, we also discuss a possible signature of SN ejecta-CSM interaction which can be found in H-poor SLSN.
AB - Origins of superluminous supernovae (SLSNe) discovered by recent SN surveys are still not known well. One idea to explain the huge luminosity is the collision of dense CSM and SN ejecta. If SN ejecta is surrounded by dense CSM, the kinetic energy of SN ejecta is efficiently converted to radiation energy, making them very bright. To see how well this idea works quantitatively, we performed numerical simulations of collisions of SN ejecta and dense CSM by using one-dimensional radiation hydrodynamics code STELLA and obtained light curves (LCs) resulting from the collision. First, we show the results of our LC modeling of SLSN 2006gy. We find that physical parameters of dense CSM estimated by using the idea of shock breakout in dense CSM (e.g., Chevalier & Irwin 2011, Moriya & Tominaga 2012) can explain the LC properties of SN 2006gy well. The dense CSM's radius is about 1016 cm and its mass about 15 M ⊙. It should be ejected within a few decades before the explosion of the progenitor. We also discuss how LCs change with different CSM and SN ejecta properties and origins of the diversity of H-rich SLSNe. This can potentially be a probe to see diversities in mass-loss properties of the progenitors. Finally, we also discuss a possible signature of SN ejecta-CSM interaction which can be found in H-poor SLSN.
KW - circumstellar matter
KW - stars: mass loss
KW - supernovae: general
KW - supernovae: individual (SN 2006gy, SN 2006oz)
UR - http://www.scopus.com/inward/record.url?scp=84897906451&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84897906451&partnerID=8YFLogxK
U2 - 10.1017/S1743921313009277
DO - 10.1017/S1743921313009277
M3 - Conference contribution
AN - SCOPUS:84897906451
SN - 9781107044777
T3 - Proceedings of the International Astronomical Union
SP - 86
EP - 89
BT - Supernova Environmental Impacts
A2 - Ray, Alak
A2 - McCray, Richard
ER -