Three-dimensional Hydrodynamic Simulations of Supernova Ejecta with a Central Energy Source

Suzuki, Akihiro; Maeda, Keiichi

doi:10.3847/1538-4357/ab2ad3

Cited by 29 publications

(12 citation statements)

References 182 publications

(272 reference statements)

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“…We take for the mass of the CCSN ejecta M ej = 5M and for its kinetic energy is E SN = 4×10 51 erg. We take the initial density and velocity profiles of the ejecta from Suzuki & Maeda (2019) (their equations 1-6, with l = 1 and m = 10). Namely, we assume the ejecta outflows in its terminal velocity v(t) = r/t e , where t e is the time from explosion.…”

Section: Three-dimensional Hydrodynamical Proceduresmentioning

confidence: 99%

Post-explosion positive jet-feedback activity in inner ejecta of core collapse supernovae

Akashi,

Soker

2022

Preprint

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We conduct three-dimensional hydrodynamical simulations of weak jets that we launch into a core collapse supernovae (CCSNe) ejecta half an hour after the explosion and find that the interaction of the fast jets with the CCSN ejecta creates high pressure zones that induce a backflow that results in mass accretion onto the newly born neutron star. In cases of weak jets, a total power of ≈ 10 45 −10 46 erg, the backflow mass accretion might power up to an order of magnitude more energetic jets. In total, the jets of the two post-explosion jet-launching episodes have enough energy to influence the morphology of the very inner ejecta, a mass of ≈ 0.1M . Our results imply that in some, probably a minority of, CCSN remnants the very inner regions might display a bipolar structure that results from post-explosion weak jets. The regions outside this part might display the morphology of jittering jets.

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Section: Three-dimensional Hydrodynamical Proceduresmentioning

confidence: 99%

Post-explosion positive jet-feedback activity in inner ejecta of core collapse supernovae

Akashi,

Soker

2022

Preprint

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“…An observational effect of this density spike could be a flat or very slow velocity evolution in spectroscopic lines. However, this density spike may also be an artefact of one-dimensional simulations, and can be washed out by turbulent mixing in higher dimensions (Chen et al 2016), but simulations suggest this is energydependent (Suzuki & Maeda 2019, 2021.…”

Section: Powering Mechanismsmentioning

confidence: 99%

Transitional events in the spectrophotometric regime between stripped envelope and superluminous supernovae

Prentice

Inserra

Schulze

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The division between stripped-envelope supernovae (SE-SNe) and superluminous supernovae (SLSNe) is not well defined in either photometric or spectroscopic space. While a sharp luminosity threshold has been suggested, there remains an increasing number of transitional objects that reach this threshold without the spectroscopic signatures common to SLSNe. In this work we present data and analysis on four SNe transitional between SE-SNe and SLSNe; the He-poor SNe 2019dwa and 2019cri, and the He-rich SNe 2019hge and 2019unb. Each object displays long-lived and variable photometric evolution with luminosities around the SLSN threshold of Mr < −19.8 mag. Spectroscopically however, these objects are similar to SE-SNe, with line velocities lower than either SE-SNe and SLSNe, and thus represent an interesting case of rare transitional events.

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“…We take the ejecta a long time after the explosion, such that the initial (when we start the simulation) velocity at each radius is v(r) = r/t 0 , where t 0 is the time after explosion when we start the simulation. We take the initial density profile from Suzuki & Maeda (2019) (their equation 1-6, with l = 1 and m = 10), which reads…”

Section: Numerical Setupmentioning

confidence: 99%

Simulating the inflation of bubbles by late jets in core collapse supernova ejecta

Akashi,

Soker

2020

Preprint

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We conducted three-dimensional hydrodynamical simulations to study the interaction of two late opposite jets with the ejecta of a core collapse supernova (CCSN), and study the bipolar structure that results from this interaction as the jets inflate hot-low-density bubbles. The newly born central object, a neutron star (NS; or a black hole), launches these jets at about 50 to 100 days after explosion. The bubbles cross the photosphere in the polar directions at much earlier times than the regions at the same radii near the equatorial plane. The hot bubbles releases more radiation and the photosphere recedes more rapidly in the tenuous bubble. Our results strengthen earlier claims that were based on toy models that such an interaction might lead to a late peak in the light curve, and that an equatorial observer might see a rapid drop in the light curve. Our results have implications to much earlier jets that explode the star, either jets that the newly born NS launches in a CCSN, or jets that a NS companion that merges with the core of a massive star launches in a common envelope jets supernova (CEJSN) event. Our results add indirect support to the CEJSN scenario for fast blue optical transients, e.g.,

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Three-dimensional Hydrodynamic Simulations of Supernova Ejecta with a Central Energy Source

Cited by 29 publications

References 182 publications

Post-explosion positive jet-feedback activity in inner ejecta of core collapse supernovae

Post-explosion positive jet-feedback activity in inner ejecta of core collapse supernovae

Transitional events in the spectrophotometric regime between stripped envelope and superluminous supernovae

Simulating the inflation of bubbles by late jets in core collapse supernova ejecta

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