Jet-shaped geometrically modified light curves of core-collapse supernovae

Kaplan, Noa; Soker, Noam

doi:10.1093/mnras/staa1201

Cited by 15 publications

(14 citation statements)

References 47 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…As well, it does not fit to the present extension (section 4.1) of the toy model of Kaplan & Soker (2020a). Kaplan & Soker (2020b) modelled the light curve of SN 2018don with jet-driven bipolar explosion, rather than with long-lived jets. The bipolar explosion model is probably not unique.…”

Section: Sn 2018donmentioning

confidence: 72%

“…Such energetic jets might lead to a bipolar explosion, and therefore the viewing angle is also an important parameter in the fitting. Kaplan & Soker (2020b) demonstrated the possible importance of the viewing angle in the their bipolar explosion model of SN 2018don (section 4.3). I argue in section 4.3 that a similar model of energetic jet-driven bipolar explosion (that works without late jets) account also for SN 2020wnt.…”

Section: Discussionmentioning

confidence: 91%

“…Kaplan & Soker (2020b) modelled the light curve of SN 2018don, one of the 40 LSNe that Gomez et al (2022) study. Kaplan & Soker (2020b) described the case where strong jets power a bipolar explosion and argued that for an observer in the equatorial plane of the bipolar ejecta the light curve has a rapid luminosity decline. Then there is a 'knee' and the decline becomes more moderate.…”

Section: A Toy Modelmentioning

confidence: 99%

“…1. I suggest that a jet-driven energetic bipolar explosion accounts also for the behavior of SN 2020wnt, including the knee in its light curve (Tinyanont et al 2022), something the bipolar explosion model can account for (Kaplan & Soker 2020b).…”

Section: Sn 2018donmentioning

confidence: 99%

See 3 more Smart Citations

Powering luminous core collapse supernovae with jets

Soker¹

2022

Preprint

Self Cite

View full text Add to dashboard Cite

I examine recent fitting of luminous supernovae (LSNe) with extra energy sources of magnetar and helium burning and find that in about half of these LSNe the fitting parameters have some problems. In some LSNe the total energy of these two energy sources is larger than the kinetic energy of the ejecta that the fitting yields. In some others LSNe the total energy of the delayed neutrino explosion mechanism and these two extra sources combined is smaller than the kinetic energy that the fitting yields. These difficulties suggest that, like earlier claims that jets power superluminous supernovae (SLSNe), jets also power the less luminous LSNe. A magnetar might also supply energy. However, in most cases jets supply more energy than the magnetar, during the explosion and possibly at late times. I strengthen an earlier claim that jets launched at magnetar birth cannot be ignored. I explain the trend of maximum rise time for a given luminosity of hydrogen deficient core collapse supernovae (CCSNe), in particular LSNe and SLSNe, with a toy model of jets that are active for a long time after explosion.

show abstract

Section: Sn 2018donmentioning

confidence: 72%

Section: Discussionmentioning

confidence: 91%

Section: A Toy Modelmentioning

confidence: 99%

Section: Sn 2018donmentioning

confidence: 99%

See 2 more Smart Citations

Powering luminous core collapse supernovae with jets

Soker¹

2022

Preprint

Self Cite

View full text Add to dashboard Cite

show abstract

“…The energy injection for the magnetar could be anisotropic with a jet-like structure (e.g., Bucciantini et al 2009), which may lead to the breakout emission that is easier to see from the polar viewing angle. Kaplan & Soker (2020) considered a bipolar ejecta and found that radiation can escape much easier on the polar direction, leading to a more rapid luminosity drop in the light curve.…”

Section: Light-curves Fittingmentioning

confidence: 99%

Magnetar-Driven Shock Breakout Revisited and Implications for Double-Peaked Type I Superluminous Supernovae

Liu,

Gao,

Wang

et al. 2021

Preprint

View full text Add to dashboard Cite

The discovery of early bumps in some type-I superluminous supernovae (SLSNe-I) before the main peaks offers an important clue to their energy source mechanisms. In this paper, we updated an analytic magnetar-powered model for fitting the multi-band light curves of double-peaked SLSNe-I: the early bump is powered by magnetar-driven shock breakout thermal emission, and the main peak is powered by a radiative diffusion through the SN ejecta as in the standard magnetar-powered model. Generally, the diffusive luminosity is greater than the shock breakout luminosity at the early time, which makes the shock breakout bumps usually not clearly seen as observed. To obtain a clear doublepeaked light curve, inefficient magnetar heating at early times is required. This model is applied to three well-observed double-peaked SLSNe-I (i.e., SN2006oz, LSQ14bdq, and DES14Xtaz). We find that a relative massive SN ejecta with M ej 10.2 − 18.1M and relative large kinetic energy of SN ejecta E sn (3.8 − 6.5) × 10 51 erg are required, and the thermalization efficiency of the magnetar heating is suppressed before t delay , which are in the range of 15 − 43 days. The model can well reproduce the observed light curves, with a reasonable and similar set of physical parameters for both the early bump and the main peak, strengthening support for magnetar-powered model. In the future, modeling of the double-peaked SLSNe-I will become more feasible as more events are discovered before the early bump.

show abstract

SN 2020qlb: A hydrogen-poor superluminous supernova with well-characterized light curve undulations

West

Lunnan

Omand

et al. 2023

A&A

View full text Add to dashboard Cite

Context. SN 2020qlb (ZTF20abobpcb) is a hydrogen-poor superluminous supernova (SLSN-I) that is among the most luminous (maximum M g = −22.25 mag) and that has one of the longest rise times (77 days from explosion to maximum). We estimate the total radiated energy to be > 2.1 × 10 51 erg. SN 2020qlb has a well-sampled light curve that exhibits clear near and post peak undulations, a phenomenon seen in other SLSNe, whose physical origin is still unknown. Aims. We discuss the potential power source of this immense explosion as well as the mechanisms behind its observed light curve undulations. Methods. We analyze photospheric spectra and compare them to other SLSNe-I. We construct the bolometric light curve using photometry from a large data set of observations from the Zwicky Transient Facility (ZTF), Liverpool Telescope (LT) and Neil Gehrels Swift Observatory and compare it with radioactive, circumstellar interaction and magnetar models. Model residuals and light curve polynomial fit residuals are analyzed to estimate the undulation timescale and amplitude. We also determine host galaxy properties based on imaging and spectroscopy data, including a detection of the [O III]λ4363, auroral line, allowing for a direct metallicity measurement. Results. We rule out the Arnett 56 Ni decay model for SN 2020qlb's light curve due to unphysical parameter results. Our most favored power source is the magnetic dipole spin-down energy deposition of a magnetar. Two to three near peak oscillations, intriguingly similar to those of SN 2015bn, were found in the magnetar model residuals with a timescale of 32 ± 6 days and an amplitude of 6% of peak luminosity. We rule out centrally located undulation sources due to timescale considerations; and we favor the result of ejecta interactions with circumstellar material (CSM) density fluctuations as the source of the undulations.

show abstract

Jet-shaped geometrically modified light curves of core-collapse supernovae

Cited by 15 publications

References 47 publications

Powering luminous core collapse supernovae with jets

Powering luminous core collapse supernovae with jets

Magnetar-Driven Shock Breakout Revisited and Implications for Double-Peaked Type I Superluminous Supernovae

SN 2020qlb: A hydrogen-poor superluminous supernova with well-characterized light curve undulations

Contact Info

Product

Resources

About