Constraints on Explosion Timescale of Core-Collapse Supernovae Based on Systematic Analysis of Light Curves

Saito, Sei; Tanaka, Masaomi; Sawada, Ryo; Moriya, Takashi J.

doi:10.48550/arxiv.2205.00624

Cited by 2 publications

(2 citation statements)

References 63 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The jittering jets mechanism was developed to explode stars within about a second from core bounce, similar to the expectations from the delayed neutrino mechanism in the past. Some recent studies suggest that the explosion activity can last for over five seconds (e.g., Bollig et al 2021), while other studies, however, argue that the explosion should take place within less than a second (e.g., Saito et al 2022). The accretion rate in a fraction of the first second is indeed close to 1 M e s −1 , as I scale quantities in this study.…”

Section: On the Possibility Of Prolonged Jet Activitymentioning

confidence: 99%

Boosting Jittering Jets by Neutrino Heating in Core Collapse Supernovae

Soker¹

2022

Res. Astron. Astrophys.

View full text Add to dashboard Cite

I estimate the energy that neutrino heating adds to the outflow that jets induce in the collapsing core material in core collapse supernovae (CCSNe), and find that this energy crudely doubles the energy that the jets deposit into the outer core. I consider the jittering jets explosion mechanism where there are several stochastic jet-launching episodes, each lasting for about 0.01-0.1 seconds. The collapsing core material passes through the stalled shock at about 100 km and then slowly flows onto the proto-neutron star (NS). I assume that the proto-NS launches jittering jets, and that the jets break out from the stalled shock. I examine the boosting process by which the high-pressure gas inside the stalled shock, the gain region material, expands alongside the jets and does work on the material that the jets shock, the cocoon. This work is crudely equal to the energy that the original jets carry. I argue that the coupling between instabilities, stochastic rotation, magnetic fields, and jittering jets lead to most CCSN explosions. In other cases, the pre-collapse core is rapidly rotating and therefore ordered rotation replaces stochastic rotation and fixed jets replace jittering jets.

show abstract

Section: On the Possibility Of Prolonged Jet Activitymentioning

confidence: 99%

Boosting Jittering Jets by Neutrino Heating in Core Collapse Supernovae

Soker¹

2022

Res. Astron. Astrophys.

View full text Add to dashboard Cite

show abstract

“…Generally speaking, FBOTs together with SLSNe can be separated from SNe Ic-BL including GRB-SNe by the 4), by assuming that all the kinetic energy of the ejecta comes from the rotational energy of the magnetar. It is commonly believed that the mass of the 56 Ni synthesized during core-collapse SNe is very difficult to reach a few tens percent of the total mass of the SN ejecta (e.g., Suwa et al 2015;Saito et al 2022). So, both FBOTs and SLSNe of magnitudes above Equation (5) definitely cannot be primarily powered by radioactive decay of 56 Ni and an engine power is required.…”

Section: Shape Of Lightcurvesmentioning

confidence: 99%

Magnetar Engines in Fast Blue Optical Transients and Their Connections with SLSNe, SNe Ic-BL, and lGRBs

Liu¹,

Zhu²,

Liu³

et al. 2022

Preprint

View full text Add to dashboard Cite

We fit the multi-band lightcurves of 40 fast blue optical transients (FBOTs) with the magnetar engine model. The mass of the FBOT ejecta, the initial spin period and polar magnetic field of the FBOT magnetars are respectively constrained to M ej = 0.18 +0.52 −0.13 M , P i = 9.4 +8.1 −3.9 ms, and B p = 7 +16 −5 × 10 14 G. The wide distribution of the value of B p spreads the parameter ranges of the magnetars from superluminous supernovae (SLSNe) to broad-line Type Ic supernovae (SNe Ic-BL; some are observed to be associated with long-duration gamma-ray bursts), which are also suggested to be driven by magnetars. Combining FBOTs with the other transients, we find a strong universal anti-correlation as P i ∝ M −0.45 ej , indicating them could share a common origin. To be specific, it is suspected that all of these transients originate from collapse of extreme-stripped stars in close binary systems, but with different progenitor masses. As a result, FBOTs distinct themselves by their small ejecta masses with an upper limit of ∼1 M , which leads to an observational separation in the rise time of the lightcurves ∼ 12 d. In addition, the FBOTs together with SLSNe can be separated from SNe Ic-BL by an empirical line in the M peak − t rise plane corresponding to an energy requirement of a mass of 56 Ni of ∼ 0.3M ej , where M peak is the peak absolute magnitude of the transients and t rise is the rise time.

show abstract

Constraints on Explosion Timescale of Core-Collapse Supernovae Based on Systematic Analysis of Light Curves

Cited by 2 publications

References 63 publications

Boosting Jittering Jets by Neutrino Heating in Core Collapse Supernovae

Boosting Jittering Jets by Neutrino Heating in Core Collapse Supernovae

Magnetar Engines in Fast Blue Optical Transients and Their Connections with SLSNe, SNe Ic-BL, and lGRBs

Contact Info

Product

Resources

About