Rapidly Evolving Transients from the Hyper Suprime-Cam SSP Transient Survey

Tampo, Yusuke; Tanaka, Masaomi; Maeda, Keiichi; Yasuda, Naoki; Tominaga, Nozomu; Jiang, Ji-an; Moriya, Takashi J.; Morokuma, Tomoki; Suzuki, N.; Takahashi, Ichiro; Kokubo, Mitsuru; Kawana, Kojiro

doi:10.3847/1538-4357/ab7ccc

Cited by 40 publications

(30 citation statements)

References 58 publications

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“…Alternatively, the jet launched in the progenitors could be choked and the explosions of some ULGRB progenitors may occur without GRBs (e.g., Milisavljevic et al 2015). The quickly-rising, luminous, blue SNe that we predict here match the properties of fast blue optical transients (FBOTs, Drout et al 2014;Tampo et al 2020). They have a rise time of less than 10 days and peak luminosities ranging from ∼10 42 erg s −1 to ∼10 44 erg s −1 .…”

Section: Discussionsupporting

confidence: 75%

Luminous supernovae associated with ultra-long gamma-ray bursts from hydrogen-free progenitors extended by pulsational pair-instability

Moriya

Marchant

Блинников

2020

A&A

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We show that the luminous supernovae associated with ultra-long gamma-ray bursts can be related to the slow cooling from the explosions of hydrogen-free progenitors that are extended by pulsational pair-instability. We have recently shown that some rapidly-rotating hydrogen-free gamma-ray burst progenitors that experience pulsational pair-instability can keep an extended structure caused by pulsational pair-instability until the core collapse. These types of progenitors have large radii exceeding 10 R⊙ and they sometimes reach beyond 1000 R⊙ at the time of the core collapse. They are, therefore, promising progenitors of ultra-long gamma-ray bursts. Here, we perform light-curve modeling of the explosions of one extended hydrogen-free progenitor with a radius of 1962 R⊙. The progenitor mass is 50 M⊙ and 5 M⊙ exists in the extended envelope. We use the one-dimensional radiation hydrodynamics code STELLA in which the explosions are initiated artificially by setting given explosion energy and 56Ni mass. Thanks to the large progenitor radius, the ejecta experience slow cooling after the shock breakout and they become rapidly evolving (≲10 days), luminous (≳1043 erg s−1) supernovae in the optical even without energy input from the 56Ni nuclear decay when the explosion energy is more than 1052 erg. The 56Ni decay energy input can affect the light curves after the optical light-curve peak and make the light-curve decay slowly when the 56Ni mass is around 1 M⊙. They also have a fast photospheric velocity above 10 000 km s−1 and a hot photospheric temperature above 10 000 K at around the peak luminosity. We find that the rapid rise and luminous peak found in the optical light curve of SN 2011kl, which is associated with the ultra-long gamma-ray burst GRB 111209A, can be explained as the cooling phase of the extended progenitor. The subsequent slow light-curve decline can be related to the 56Ni decay energy input. The ultra-long gamma-ray burst progenitors we proposed recently can explain both the ultra-long gamma-ray burst duration and the accompanying supernova properties. When the gamma-ray burst jet is off-axis or choked, the luminous supernovae could be observed as fast blue optical transients without accompanying gamma-ray bursts.

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Section: Discussionsupporting

confidence: 75%

Luminous supernovae associated with ultra-long gamma-ray bursts from hydrogen-free progenitors extended by pulsational pair-instability

Moriya

Marchant

Блинников

2020

A&A

Self Cite

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show abstract

“…Alternatively, the jet launched in the progenitors could be choked and the explosions of some ULGRB progenitors may occur without GRBs (e.g., Milisavljevic et al 2015). The quickly-rising, luminous, blue SNe we predict here match the properties of fast blue optical transients (FBOTs, Drout et al 2014;Tampo et al 2020). They have a rise time of less than 10 days and peak luminosities ranging from ∼ 10 42 erg s −1 to ∼ 10 44 erg s −1 .…”

Section: Discussionsupporting

confidence: 71%

Luminous supernovae associated with ultra-long gamma-ray bursts from hydrogen-free progenitors extended by pulsational pair-instability

Moriya,

Marchant,

Blinnikov

2020

Preprint

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We show that the luminous supernovae associated with ultra-long gamma-ray bursts can be related to the slow cooling from the explosions of hydrogen-free progenitors extended by pulsational pair-instability. In the accompanying paper (Marchant & Moriya 2020), we have shown that some rapidly-rotating hydrogen-free gamma-ray burst progenitors that experience pulsational pair-instability can keep an extended structure caused by pulsational pair-instability until the core collapse. Such progenitors have large radii exceeding 10 R ⊙ and they sometimes reach beyond 1000 R ⊙ at the time of the core collapse. They are, therefore, promising progenitors of ultra-long gamma-ray bursts. We here perform the light-curve modeling of the explosions of one extended hydrogen-free progenitor with a radius of 1962 R ⊙ . The progenitor mass is 50 M ⊙ and 5 M ⊙ exists in the extended envelope. We use one-dimensional radiation hydrodynamics code STELLA in which the explosions are initiated artificially by setting given explosion energy and 56 Ni mass. Thanks to the large progenitor radius, the ejecta experience slow cooling after the shock breakout and they become rapidly evolving ( 10 days) luminous ( 10 43 erg s −1 ) supernovae in optical even without the energy input from the 56 Ni nuclear decay when the explosion energy is more than 10 52 erg. The 56 Ni decay energy input can affect the light curves after the optical light-curve peak and make the light-curve decay slow when the 56 Ni mass is around 1 M ⊙ . They also have fast photospheric velocity above 10,000 km s −1 and hot photospheric temperature above 10,000 K at around the peak luminosity. We find that the rapid rise and luminous peak found in the optical light curve of SN 2011kl, which is associated with the ultra-long gamma-ray burst GRB 111209A, can be explained as the cooling phase of the extended progenitor. The subsequent slow light-curve decline can be related to the 56 Ni decay energy input. The ultra-long gamma-ray burst progenitors proposed in Marchant & Moriya (2020) can explain both the ultra-long gamma-ray burst duration and the accompanying supernova properties. When the gamma-ray burst jet is off-axis or choked, the luminous supernovae could be observed as fast blue optical transients without accompanying gamma-ray bursts.

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“…This is an analog of the post-shock breakout cooling emission in canonical SNe. We consider a potential link between the thermal emission and an emerging population of peculiar optical transients detected by recent transient surveys (e.g., Drout et al 2014;Arcavi et al 2016;Pursiainen et al 2018;Tampo et al 2020;Ho et al 2021).…”

Section: Post-shock Breakout Cooling Emissionmentioning

confidence: 99%

Chemical stratification in a long gamma-ray burst cocoon and early-time spectral signatures of supernovae associated with gamma-ray bursts

Suzuki,

Maeda

2021

Preprint

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We present the results of 3D hydrodynamic simulations of gamma-ray burst (GRB) jet emanating from a massive star with a particular focus on the formation of high-velocity quasi-spherical ejecta and the jet-induced chemical mixing. Recent early-time optical observations of supernovae associated with GRBs (e.g., GRB 171205A/SN 2017iuk) indicate a considerable amount of heavy metals in the highvelocity outer layers of the ejecta. Using our jet simulations, we show that the density and chemical structure of the outer ejecta implied by observations can be naturally reproduced by a powerful jet penetrating the progenitor star. We consider three representative jet models with a stripped massive star, a standard jet, a weak jet, and a jet choked by an extended circumstellar medium, to clarify the differences in the dynamical evolution and the chemical properties of the ejected materials. The standard jet successfully penetrates the progenitor star and creates a quasi-spherical ejecta component (cocoon). The jet-induced mixing significantly contaminates the cocoon with heavy elements that have been otherwise embedded in the inner layer of the ejecta. The weak and choked jet models fail to produce an ultra-relativistic jet but produce a quasi-spherical cocoon with different chemical properties. We discuss the impact of the different jet-star interactions on the expected early-time electromagnetic signatures of long GRBs and how to probe the jet dynamics from observations.

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Rapidly Evolving Transients from the Hyper Suprime-Cam SSP Transient Survey

Cited by 40 publications

References 58 publications

Luminous supernovae associated with ultra-long gamma-ray bursts from hydrogen-free progenitors extended by pulsational pair-instability

Luminous supernovae associated with ultra-long gamma-ray bursts from hydrogen-free progenitors extended by pulsational pair-instability

Luminous supernovae associated with ultra-long gamma-ray bursts from hydrogen-free progenitors extended by pulsational pair-instability

Chemical stratification in a long gamma-ray burst cocoon and early-time spectral signatures of supernovae associated with gamma-ray bursts

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