Photometric, polarimetric, and spectroscopic studies of the luminous, slow-decaying Type Ib SN 2012au

Kumar, Amit; Kumar, Brijesh; Anupama, G. C.; Srivastav, Shubham; Sahu, D. K.; Vinkó, J.; Aryan, Amar; Pastorello, A.; Benetti, S.; Tomasella, L.; Singh, Avinash; Москвитин, А. С.; Соколов, В. В.; Gupta, Rahul; Misra, Kuntal; Ochner, P.; Valenti, S.

doi:10.1093/mnras/stab1889

Cited by 22 publications

(5 citation statements)

References 190 publications

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“…For this purpose, we used the default example make pre ccsn directory available in MESA. Most of the settings closely follow Aryan et al (2021a) and Pandey et al (2021) with only a few minor deviations. We do not consider rotation and assume an initial metallicity of Z = 0.01.…”

Section: Progenitor Modeling Using Mesasupporting

confidence: 76%

Core-collapse supernova from a possible progenitor star of 100 M$_{\odot}$

Aryan,

Pandey,

Yadav

et al. 2022

Preprint

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In this work, we study the synthetic explosions of a massive star. We take a 100 M zero-age mainsequence (ZAMS) star and evolve it until the onset of core-collapse using MESA. Then, the resulting star model is exploded using the publicly available stellar explosion code, STELLA. The outputs of STELLA calculations provide us the bolometric light curve and photospheric velocity evolution along with other physical properties of the underlying supernova. In this paper, the effects of having large Hydrogen-envelope on the supernova light curve have been explored. We also explore the effects of the presence of different amounts of nickel mass and the effect of changing the explosion energy of the resulting supernovae from such heavy progenitors, on their bolometric light curves and photospheric velocities.

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Section: Progenitor Modeling Using Mesasupporting

confidence: 76%

Core-collapse supernova from a possible progenitor star of 100 M$_{\odot}$

Aryan,

Pandey,

Yadav

et al. 2022

Preprint

Self Cite

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“…The above discussion implies that CCSNe with large kinetic energies of E exp 2 × 10 51 , e.g., SN 2020jfo (Ailawadhi et al 2022 -E exp = 2.9 × 10 51 erg); SN 2020qlb (West et al 2022 -E exp = 20 × 10 51 erg); SN 2012au (Pandey et al 2021 -E exp = 4.8 − 5.4 × 10 51 erg) require jets to drive the explosion.…”

Section: Introductionmentioning

confidence: 92%

The implications of large binding energies of massive stripped core collapse supernova progenitors on the explosion mechanism

Shishkin¹,

Soker²

2023

Preprint

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We examine the binding energy of massive stripped-envelope core collapse supernova (SECCSN) progenitors with the stellar evolution code mesa, and find that only the jittering jets explosion mechanism can account for explosions where carbon-oxygen cores with masses of 20M collapse to leave a neutron star (NS) remnant. We calculate the binding energy at core collapse under the assumption that the remnant is a NS. Namely, stellar gas above mass coordinate of 1.5 − 2.5M is ejected in the explosion. We find that the typical binding energy of the ejecta of stripped-envelope progenitors with carbon-oxygen core masses of M CO 20M is E bind 2 × 10 51 erg. Since only jet-driven explosion mechanisms can supply such high energies, we conclude that jets must explode such cores. We apply our results to SN 2020qlb, which is a SECCSN with a claimed core mass of 30 − 50M , and conclude that the jittering jets explosion mechanism best account for such an explosion that leaves a NS.

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“…4. PTF12dam: This SLSN-I was found to be a symmetric explosion showing null polarization (Cikota et al 2018;Pandey et al 2021;Poidevin et al 2022). 5.…”

Section: Geometrymentioning

confidence: 97%

Premaximum Spectroscopic Diversity of Hydrogen-poor Superluminous Supernovae

Könyves-Tóth

2022

ApJ

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We search for the reasons behind the spectroscopic diversity of hydrogen-poor superluminous supernovae (SLSNe-I) in the premaximum phase. Our analysis is a continuation of the paper of Könyves-Tóth & Vinkó, who disclosed two new subtypes of SLSNe-I characterized by the presence/absence of a W-shaped absorption feature in their premaximum spectra between 4000 and 5000 Å (called Type W and Type 15bn, respectively). However, the physical cause of this bimodality is still uncertain. Here we present premaximum spectral synthesis of 27 SLSNe-I with special attention to the photospheric temperature (T phot) and velocity (v phot) evolution. We find that a T phot limit of 12,000 K separates the Type W and Type 15bn SLSNe-I: Type W objects tend to show T phot ≥ 12,000 K, while Type 15bn ones have T phot ≤ 12,000 K. This is consistent with the chemical composition of the studied objects. Another difference between these groups may be found in their ejecta geometry: Type W SLSNe-I may show null polarization, implying spherical symmetry, while the polarization of Type 15bn objects may increase in time. This suggests a two-component model with a spherical outer carbon–oxygen layer and an asymmetric inner layer containing heavier ions. The two subgroups may have different light-curve evolution as well, since six Type W objects show early bumps, unlike Type 15bn SLSNe-I. This feature, however, needs further study, as it is based on only a few objects at present.

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Photometric, polarimetric, and spectroscopic studies of the luminous, slow-decaying Type Ib SN 2012au

Cited by 22 publications

References 190 publications

Core-collapse supernova from a possible progenitor star of 100 M$_{\odot}$

Core-collapse supernova from a possible progenitor star of 100 M$_{\odot}$

The implications of large binding energies of massive stripped core collapse supernova progenitors on the explosion mechanism

Premaximum Spectroscopic Diversity of Hydrogen-poor Superluminous Supernovae

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