CHIPS: Complete History of Interaction-powered Supernovae

Takei, Yuki; Tsuna, D.; Kuriyama, Naoto; Ko, Takatoshi; Shigeyama, Toshikazu

doi:10.3847/1538-4357/ac60fe

Cited by 11 publications

(20 citation statements)

References 90 publications

(108 reference statements)

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“…The CSM density scale in the inner CSM component (2 × 10 15 cm) of SN 2018ivc is within the range estimated for the confined CSM around SN IIP 2013fs, while the spatial extent is different by a factor of ∼2. There could be some diversity in the nature of the confined CSM in terms of its mass and radial scale, either in the timing when the final activity sets in or in the energy provided by the core relative to the envelope binding energy (Morozova et al 2020;Takei et al 2022). Indeed, the inner CSM component of SN 2018ivc matches well to that derived for SN IIb 2013cu from optical "flash spectroscopy" (Gal-Yam et al 2014;Groh 2014).…”

Section: The Inner Csm Properties: Pre-sn Dynamical Activity?mentioning

confidence: 70%

A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction

Maeda

Chandra

Moriya

et al. 2022

ApJ

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SN 2018ivc is an unusual Type II supernova (SN II). It is a variant of SNe IIL, which might represent a transitional case between SNe IIP with a massive H-rich envelope and SNe IIb with only a small amount of the H-rich envelope. However, SN 2018ivc shows an optical light-curve evolution more complicated than that of canonical SNe IIL. In this paper, we present the results of prompt follow-up observations of SN 2018ivc with the Atacama Large Millimeter/submillimeter Array. Its synchrotron emission is similar to that of SN IIb 1993J, suggesting that it is intrinsically an SN IIb–like explosion of an He star with a modest (∼0.5–1M ⊙) extended H-rich envelope. Its radio, optical, and X-ray light curves are explained primarily by the interaction between the SN ejecta and the circumstellar material (CSM); we thus suggest that it is a rare example (and the first involving the “canonical” SN IIb ejecta) for which the multiwavelength emission is powered mainly by the SN–CSM interaction. The inner CSM density, reflecting the progenitor activity in the final decade, is comparable to that of SN IIb 2013cu, which shows a flash spectral feature. The outer CSM density, and therefore the mass-loss rate in the final ∼200 yr, is higher than that of SN 1993J by a factor of ∼5. We suggest that SN 2018ivc represents a missing link between SNe IIP and SNe IIb/Ib/Ic in the binary evolution scenario.

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Section: The Inner Csm Properties: Pre-sn Dynamical Activity?mentioning

confidence: 70%

A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction

Maeda

Chandra

Moriya

et al. 2022

ApJ

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“…For this scenario, we follow and extend the methods of , which used the open-source code CHIPS (Takei et al 2022) to simulate mass eruption, followed by SNEC (Morozova et al 2015) for calculating the bolometric light curve. The mass loss is assumed to be triggered by energy injection at the base of the envelope, which forms a shock that propagates to the surface and expels a part of the envelope.…”

Section: Eruptive Mass Lossmentioning

confidence: 99%

From Discovery to the First Month of the Type II Supernova 2023ixf: High and Variable Mass Loss in the Final Year before Explosion

Hiramatsu,

Tsuna,

Berger

et al. 2023

ApJL

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We present the discovery of the Type II supernova SN 2023ixf in M101 and follow-up photometric and spectroscopic observations, respectively, in the first month and week of its evolution. Our discovery was made within a day of estimated first light, and the following light curve is characterized by a rapid rise (≈5 days) to a luminous peak (M V ≈ − 18.2 mag) and plateau (M V ≈ − 17.6 mag) extending to 30 days with a fast decline rate of ≈0.03 mag day−1. During the rising phase, U − V color shows blueward evolution, followed by redward evolution in the plateau phase. Prominent flash features of hydrogen, helium, carbon, and nitrogen dominate the spectra up to ≈5 days after first light, with a transition to a higher ionization state in the first ≈2 days. Both the U−V color and flash ionization states suggest a rise in the temperature, indicative of a delayed shock breakout inside dense circumstellar material (CSM). From the timescales of CSM interaction, we estimate its compact radial extent of ∼(3–7) × 1014 cm. We then construct numerical light-curve models based on both continuous and eruptive mass-loss scenarios shortly before explosion. For the continuous mass-loss scenario, we infer a range of mass-loss history with 0.1–1.0 M ⊙ yr−1 in the final 2−1 yr before explosion, with a potentially decreasing mass loss of 0.01–0.1 M ⊙ yr−1 in ∼0.7–0.4 yr toward the explosion. For the eruptive mass-loss scenario, we favor eruptions releasing 0.3–1 M ⊙ of the envelope at about a year before explosion, which result in CSM with mass and extent similar to the continuous scenario. We discuss the implications of the available multiwavelength constraints obtained thus far on the progenitor candidate and SN 2023ixf to our variable CSM models.

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“…Our calculation of mass eruption is based on the onedimensional radiation hydrodynamical simulation code from , which is made public as part of the open-source code CHIPS (Takei et al 2022). The simulation follows the hydrodynamical evolution of the hydrogen-rich envelope after energy injection, assuming local thermodynamic equilibrium.…”

Section: Mass-eruption Calculationmentioning

confidence: 99%

Precursors of Supernovae from Mass Eruption: Prospects for Early Warning of Nearby Core-collapse Supernovae

Tsuna

Takei

Shigeyama

2023

ApJ

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Recent observations of a large fraction of Type II supernovae (SNe) show traces of dense circumstellar medium (CSM) very close to the progenitor star. If this CSM is created by eruptive mass loss several months before core collapse, the eruption itself may be visible as a precursor, helpful as an early warning of a near-future SN. Using radiation hydrodynamical simulations based on the open-source code CHIPS, we theoretically model the emission from the mass eruption of a red supergiant star. We find that for a modest mass eruption the luminosity is typically on the order of 1039 erg s−1, can last as long as hundreds of days until the star explodes, and is mainly bright in the infrared (from −9 to −11 mag around peak). We discuss observational strategies to find these signatures from Galactic and local Type II SNe.

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CHIPS: Complete History of Interaction-powered Supernovae

Cited by 11 publications

References 90 publications

A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction

A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction

From Discovery to the First Month of the Type II Supernova 2023ixf: High and Variable Mass Loss in the Final Year before Explosion

Precursors of Supernovae from Mass Eruption: Prospects for Early Warning of Nearby Core-collapse Supernovae

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