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Müller, Gerhard; Löffelholz, Josef

doi:10.1007/978-3-663-00090-7_8

Cited by 26 publications

(82 citation statements)

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“…Software: Kepler (Heger & Woosley 2010), Arepo (Springel 2010), STELLA (Blinnikov et al 1998(Blinnikov et al , 2000(Blinnikov et al , 2006,CoCoNuT-FMT (Müller et al2010;Müller & Janka 2015)…”

Section: Discussionmentioning

confidence: 99%

Fallback Accretion-powered Supernova Light Curves Based on a Neutrino-driven Explosion Simulation of a 40 M_⊙ Star

Moriya

Müller

Chan

et al. 2019

ApJ

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We present synthetic light curves of fallback-powered supernovae based on a neutrino-driven explosion of a 40 M ⊙ zero-metallicity star with significant fallback accretion onto a black hole that was previously simulated by Chan et al. (2018) until shock breakout. Here, we investigate the light curve properties of the explosion after shock breakout for various fallback models. Without extra power from fallback accretion, the light curve is that of a Type IIP supernova with a plateau magnitude of around −14 mag and a plateau duration of 40 days. With extra power for the light curve from fallback accretion, however, we find that the transient can be significantly more luminous. The light-curve shape can be SN 1987A-like or Type IIP-like, depending on the efficiency of the fallback engine. If the accretion disk forms soon after the collapse and more than 1% of the accretion energy is released as the central engine, fallback accretion powered supernovae become as luminous as superluminous supernovae. We suggest that Type II superluminous supernovae with broad hydrogen features could be related to such hydrogen-rich supernovae powered by fallback accretion. In the future, such superluminous supernovae powered by fallback accretion might be found among the supernovae from the first stars in addition to pair-instability supernovae and pulstational pair-instability supernovae.

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Section: Discussionmentioning

confidence: 99%

Fallback Accretion-powered Supernova Light Curves Based on a Neutrino-driven Explosion Simulation of a 40 M_⊙ Star

Moriya

Müller

Chan

et al. 2019

ApJ

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“…Based on the Mach number, we divide our 2D models into two groups, either showing "low-M a" or "high-M a". The criterion of high-M a is set as M a 2 1/2 max ≥ 0.1, because the turbulence with such a high Mach number potentially fosters the perturbation-aided explosion (Müller & Janka 2015;Müller et al 2016). It is noted that models 18M A and 21M A are exceptionally classified into low-M a in spite of their "large" Mach numbers.…”

Section: D Stellar Hydrodynamics Simulationsmentioning

confidence: 99%

“…Couch & Ott (2013) were the first to demonstrate that the inhomogeneities seeded by convective shell burning fosters the onset of a neutrino-driven explosion (see also Fernández et al (2014); Couch & Ott (2015); Müller & Janka (2015); Burrows et al (2018)). This is because the infalling perturbation that could be amplified in the supersonic accretion (Takahashi & Yamada 2014;Nagakura et al 2013Nagakura et al , 2019 enhances turbulence behind the postshock material leading to the reduction of the critical neutrino luminosity for shock revival (e.g., Müller & Janka (2015); Abdikamalov et al (2016)). In these studies, the non-spherical structures in the burning shells, although physically motivated, were treated in a parametric manner due to the paucity of the multi-D stellar evolution models covering the lifespan of massive stars up to the iron core-collapse.…”

Section: Introductionmentioning

confidence: 99%

One-, Two-, and Three-dimensional Simulations of Oxygen-shell Burning Just before the Core Collapse of Massive Stars

Yoshida

Takiwaki

Kotake

et al. 2019

ApJ

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We perform two-(2D) and three-dimensional (3D) hydrodynamics simulations of convective oxygen shell-burning that takes place deep inside a massive progenitor star of a core-collapse supernova. Using one dimensional (1D) stellar evolution code, we first calculate the evolution of massive stars with an initial mass of 9-40 M . Four different overshoot parameters are applied, and CO core mass trend similar to previous works is obtained in the 1D models. Selecting eleven 1D models that have a silicon and oxygen coexisting layer, we perform 2D hydrodynamics simulations of the evolution for ∼100 s until the onset of core-collapse. We find that convection with large-scale eddies and the turbulent Mach number ∼0.1 is obtained in the models having a Si/O layer with a scale of 10 8 cm, whereas most models that have an extended O/Si layer up to a few ×10 9 cm exhibit lower turbulent velocity.Our results indicate that the supernova progenitors that possess a thick Si/O layer could provide a preferable condition for perturbation-aided explosions. We perform 3D simulation of a 25 M model, which exhibits large-scale convection in the 2D models. The 3D model develops large-scale ( = 2) convection similar to the 2D model, however, the turbulent velocity is lower. By estimating the neutrino emission properties of the 3D model, we point out that a time modulation of the event rates, if observed in KamLAND and Hyper-Kamiokande, would provide an important information about structural changes in the presupernova convective layer.

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“…Although this mechanism was first proposed more than five decades ago (Colgate & White 1966), it is only in recent years that neutrino-driven CCSNe simulations have begun to successfully explode (for reviews, see Janka et al 2016;Müller 2016). As computer processing power has advanced, astronomers have been able to include additional physics into their 3D models, such as precollapse perturbations (Couch & Ott 2013;Couch et al 2015;Müller & Janka 2015;Müller et al 2016Müller et al , 2017aMüller 2016), rotation (Kuroda et al 2014;Nakamura et al 2015;Takiwaki et al 2016;Summa et al 2018), Supernova remnants (SNRs) are a useful sample for comparison to simulation predictions. The heavy elements synthesized in the explosions as well as NSs are observable in young SNRs of ages 10 4 years (see reviews by Weisskopf &Vink 2012).…”

Section: Introductionmentioning

confidence: 99%

Asymmetries of Heavy Elements in the Young Supernova Remnant Cassiopeia A

Holland-Ashford

Lopez

Auchettl

2020

ApJ

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Supernova remnants (SNRs) offer the means to study supernovae (SNe) long after the original explosion and can provide a unique insight into the mechanism that governs these energetic events. In this work, we examine the X-ray morphologies of different elements from oxygen to iron found in the youngest known core-collapse (CC) SNR in the Milky Way, Cassiopeia A. The heaviest elements exhibit the highest levels of asymmetry, which we relate to the burning process that created the elements and their proximity to the center of explosion. Our findings support recent model predictions that the material closest to the source of explosion will reflect the asymmetries inherent to the SN mechanism. Additionally, we find that the heaviest elements are moving more directly opposed to the neutron star (NS) than the lighter elements. This result is consistent with NS kicks arising from ejecta asymmetries.

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Cited by 26 publications

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Fallback Accretion-powered Supernova Light Curves Based on a Neutrino-driven Explosion Simulation of a 40 M_⊙ Star

Fallback Accretion-powered Supernova Light Curves Based on a Neutrino-driven Explosion Simulation of a 40 M_⊙ Star

One-, Two-, and Three-dimensional Simulations of Oxygen-shell Burning Just before the Core Collapse of Massive Stars

Asymmetries of Heavy Elements in the Young Supernova Remnant Cassiopeia A

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Cited by 26 publications

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Fallback Accretion-powered Supernova Light Curves Based on a Neutrino-driven Explosion Simulation of a 40 M⊙ Star

Fallback Accretion-powered Supernova Light Curves Based on a Neutrino-driven Explosion Simulation of a 40 M⊙ Star

One-, Two-, and Three-dimensional Simulations of Oxygen-shell Burning Just before the Core Collapse of Massive Stars

Asymmetries of Heavy Elements in the Young Supernova Remnant Cassiopeia A

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Fallback Accretion-powered Supernova Light Curves Based on a Neutrino-driven Explosion Simulation of a 40 M_⊙ Star

Fallback Accretion-powered Supernova Light Curves Based on a Neutrino-driven Explosion Simulation of a 40 M_⊙ Star