An analytic bolometric light curve model of interaction-powered supernovae and its application to Type IIn supernovae

Moriya, Takashi J.; Maeda, Keiichi; Taddia, F.; Sollerman, J.; Блинников, С. И.; Sorokina, E. I.

doi:10.1093/mnras/stt1392

Cited by 125 publications

(199 citation statements)

References 88 publications

Supporting

Mentioning

183

Contrasting

Order By: Relevance

“…Furthermore, in such a situation a bulk of the radiated energy is either in radio or X-rays, not in the optical wavelengths. Also, we neglect the radiation cooling feedback to hydrodynamics, motivated by previous studies where the adiabatic treatment provides a reasonable description of the shock wave dynamics for SNe IIn as calibrated by radiationhydrodynamic simulations (Moriya et al 2013. Fig.…”

Section: Calculation Methodsmentioning

confidence: 99%

Mass ejection by pulsational pair instability in very massive stars and implications for luminous supernovae

Yoshida

Umeda

Maeda

et al. 2016

Mon. Not. R. Astron. Soc.

Self Cite

115

105

View full text Add to dashboard Cite

Massive stars having a CO core of ∼40-60 M ⊙ experience pulsational pair-instability (PPI) after carbon-burning. This instability induces strong pulsations of the whole star and a part of outer envelope is ejected. We investigate the evolution and mass ejection of metal-poor very massive stars which experience PPI. We use stellar models with initial masses of 140, 200, and 250 M ⊙ and the metallicity Z = 0.004. Their masses decrease to 54.09, 58.65, and 61.03 M ⊙ before the neon-burning owing to massloss and He mass fraction at the surface becomes about 20 per cent. During the PPI period of ∼1-2000 yr, they experience six, four, and three pulsations, respectively. The larger CO-core model has the longer PPI period and ejects the larger amount of mass. Since almost all surface He has been lost by the pulsations, these stars become Type Ic supernovae if they explode. Light curves during the PPI stage and supernovae are investigated and are implicated in luminous supernovae. The luminosity created by the interaction of different PPI ejecta becomes M bol ∼ −16 to −20. The interaction between the circumstellar shell ejected by PPI and the supernova ejecta can be more luminous. These luminous transients could be an origin of Type I superluminous supernovae and supernovae with precursor.

show abstract

Section: Calculation Methodsmentioning

confidence: 99%

Mass ejection by pulsational pair instability in very massive stars and implications for luminous supernovae

Yoshida

Umeda

Maeda

et al. 2016

Mon. Not. R. Astron. Soc.

Self Cite

115

105

View full text Add to dashboard Cite

show abstract

“…Specifically, for an ejecta density ρ ejecta ∝ r −n (e.g., Matzner & McKee 1999) and a CSM density ρ CSM ∝ r −s , Moriya et al (2013) found that the bolometric luminosity decays as a power law as a function of time since explosion t ,…”

Section: Intrinsic Light Curvesmentioning

confidence: 99%

“…The observed light curves are determined by the morphology of the CSM and by the progenitor star (van Marle et al 2010). For example, the shape of the light curves of type IIn SNe depend on the initial radius of the star, the ejecta mass and the explosion energy of the SNe, and the density structures of the ejecta and CSM (van Marle et al 2010;Moriya et al 2013;Taddia et al 2015). The range of potential progenitors is large and may include any star with a significant pre-SN eruption, for example, red supergiants or luminous blue variables (LBVs) (Gall et al 2011;Stritzinger et al 2012;Van Dyk 2013).…”

Section: Introductionmentioning

confidence: 99%

Early gray dust formation in the type IIn SN 2005ip

Nielsen

Hjorth

Gall

2018

A&A

View full text Add to dashboard Cite

The physical characteristics of dust formed in supernovae is poorly known. In this paper, we investigate the extinction properties of dust formed in the type IIn SN 2005ip. The observed light curves of SN 2005ip all exhibit a sudden drop around 50 days after discovery. This has been attributed to dust formation in the dense circumstellar medium. We modeled the intrinsic light curves in six optical bands, adopting a theoretical model for the luminosity evolution of supernovae interacting with their circumstellar material. From the difference between the observed and intrinsic light curves, we calculated extinction curves as a function of time. The totalto-selective extinction ratio, R V , was determined from the extinction in the B and V bands. The resulting extinction, A V , increases monotonically up to about 1 mag, 150 days after discovery. The inferred R V value also increases slightly with time, but appears constant in the range 4.5-8, beyond 100 days after discovery. The analysis confirms that dust is likely formed in SN 2005ip, starting about two months after explosion. The high value of R V , that is, gray dust, suggests dust properties different from of the Milky Way. While this result hinges on the assumed theoretical intrinsic light curve evolution, it is encouraging that the fitted light curves are as expected for standard ejecta and circumstellar medium density structures.

show abstract

“…We refer to Moriya et al (2013b) for further details. In this paper, we set n = 9 and δ = 0 to compare the model with that of van Veelen (2010) but the LC does not strongly depend on the choice of n and δ within the reasonable range (n 7-12 and δ 0-1).…”

Section: Light Curve Propertiesmentioning

confidence: 99%

Electron-capture supernovae exploding within their progenitor wind

Moriya

Tominaga

Langer

et al. 2014

A&A

Self Cite

View full text Add to dashboard Cite

The most massive stars on the asymptotic giant branch (AGB), or the so-called super-AGB stars, are thought to produce supernovae triggered by electron captures in their degenerate O+Ne+Mg cores. Super-AGB stars are expected to have slow winds with high mass-loss rates, so their circumstellar density is high. The explosions of super-AGB stars are therefore presumed to occur in this dense circumstellar environment. We provide the first synthetic light curves for such events by exploding realistic electron-capture supernova progenitors within their super-AGB winds. We find that the early light curve -that is, before the recombination wave reaches the bottom of the hydrogen-rich envelope of supernova ejecta (the plateau phase) -is not affected by the dense wind. However, after the luminosity drop following the plateau phase, the luminosity remains much higher when the super-AGB wind is taken into account. We compare our results to the historical light curve of SN 1054, the progenitor of the Crab Nebula, and show that the explosion of an electron-capture supernova within an ordinary super-AGB wind can explain the observed light curve features. We conclude that SN 1054 could have been a Type IIn supernova without any extra extreme mass loss, which was previously suggested to be necessary to account for its early high luminosity. We also show that our light curves match Type IIn supernovae with an early plateau phase or the so-called Type IIn-P supernovae, and suggest that they are electron-capture supernovae within super-AGB winds. Although some electron-capture supernovae can be bright in the optical spectral range due to the large progenitor radius, their X-ray luminosity from the interaction does not necessarily get as bright as other Type IIn supernovae whose optical luminosities are also powered by the interaction. Thus, we suggest that optically bright X-ray-faint Type IIn supernovae can emerge from electron-capture supernovae. Optically faint Type IIn supernovae, such as SN 2008S, can also originate from electron-capture supernovae if their hydrogen-rich envelope masses are small. We argue that some of them can be observed as Type IIn-b supernovae due to the small hydrogen-rich envelope mass.

show abstract

An analytic bolometric light curve model of interaction-powered supernovae and its application to Type IIn supernovae

Cited by 125 publications

References 88 publications

Mass ejection by pulsational pair instability in very massive stars and implications for luminous supernovae

Mass ejection by pulsational pair instability in very massive stars and implications for luminous supernovae

Early gray dust formation in the type IIn SN 2005ip

Electron-capture supernovae exploding within their progenitor wind

Contact Info

Product

Resources

About