Mass ejection in failed supernovae: variation with stellar progenitor

Fernández, Rodrigo; Quataert, Eliot; Kashiyama, Kazumi; Coughlin, Eric R.

doi:10.1093/mnras/sty306

Cited by 115 publications

(167 citation statements)

References 84 publications

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“…In Paper I, it was shown that the CQR self-similar solution very accurately reproduced the simulation results of Fernández et al (2018), who numerically studied the propagation of a weak shock through the envelope of a yellow supergiant (evolved from the zero-age main sequence with the stellar evolution code mesa; Paxton et al 2013Paxton et al , 2015Paxton et al , 2018 following its failure to explode in a traditional supernova. In their simulation, the shock was generated by the sudden decrease of the gravitational field that follows the formation of the proto-neutron star during core-collapse.…”

Section: Discussionmentioning

confidence: 80%

Weak Shock Propagation with Accretion. II. Stability of Self-similar Solutions to Radial Perturbations

Coughlin

Quataert

2019

ApJ

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Coughlin et al. (2018b) (Paper I) derived and analyzed a new regime of self-similarity that describes weak shocks (Mach number of order unity) in the gravitational field of a point mass. These solutions are relevant to low energy explosions, including failed supernovae. In this paper, we develop a formalism for analyzing the stability of shocks to radial perturbations, and we demonstrate that the self-similar solutions of Paper I are extremely weakly unstable to such radial perturbations. Specifically, we show that perturbations to the shock velocity and post-shock fluid quantities (the velocity, density, and pressure) grow with time as t α , where α ≤ 0.12, implying that the ten-folding timescale of such perturbations is roughly ten orders of magnitude in time. We confirm these predictions by performing high-resolution, time-dependent numerical simulations. Using the same formalism, we also show that the Sedov-Taylor blastwave is trivially stable to radial perturbations provided that the self-similar, Sedov-Taylor solutions extend to the origin, and we derive simple expressions for the perturbations to the post-shock velocity, density, and pressure. Finally, we show that there is a third, self-similar solution (in addition to the the solutions in Paper I and the Sedov-Taylor solution) to the fluid equations that describes a rarefaction wave, i.e., an outward-propagating sound wave of infinitesimal amplitude. We interpret the stability of shock propagation in light of these three distinct self-similar solutions.

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Section: Discussionmentioning

confidence: 80%

Weak Shock Propagation with Accretion. II. Stability of Self-similar Solutions to Radial Perturbations

Coughlin

Quataert

2019

ApJ

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“…Alternatively, the intrinsic dipole mag- (2018); (4) Tauris et al (2015); (5) E.g. Miyaji et al (1980);Nomoto et al (1982); Moriya et al (2014) and references there in; (6) Fernández et al (2018); (7) Andrews & Smith (2018), Metzger & Pejcha (2017).…”

Section: Millisecond Magnetar From Successful Supernova With Low Ejecmentioning

confidence: 99%

An Embedded X-Ray Source Shines through the Aspherical AT 2018cow: Revealing the Inner Workings of the Most Luminous Fast-evolving Optical Transients

Margutti

Metzger

Chornock

et al. 2019

ApJ

222

409

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We present the first extensive radio to γ-ray observations of a fast-rising blue optical transient (FBOT), AT 2018cow, over its first ∼100 days. AT 2018cow rose over a few days to a peak luminosity L pk ∼ 4 × 10 44 erg s −1 exceeding those of superluminous supernovae (SNe), before declining as L ∝ t −2 . Initial spectra at δt 15 days were mostly featureless and indicated large expansion velocities v ∼ 0.1 c and temperatures arXiv:1810.10720v1 [astro-ph.HE] 25 Oct 2018 2 MARGUTTI ET AL. reaching T ∼ 3 × 10 4 K. Later spectra revealed a persistent optically-thick photosphere and the emergence of H and He emission features with v ∼ 4000 km s −1 with no evidence for ejecta cooling. Our broad-band monitoring revealed a hard X-ray spectral component at E ≥ 10 keV, in addition to luminous and highly variable soft X-rays, with properties unprecedented among astronomical transients. An abrupt change in the X-ray decay rate and variability appears to accompany the change in optical spectral properties. AT 2018cow showed bright radio emission consistent with the interaction of a blastwave with v sh ∼ 0.1 c with a dense environment (Ṁ ∼ 10 −3 − 10 −4 M yr −1 for v w = 1000 km s −1 ). While these properties exclude 56 Ni-powered transients, our multi-wavelength analysis instead indicates that AT 2018cow harbored a "central engine", either a compact object (magnetar or black hole) or an embedded internal shock produced by interaction with a compact, dense circumstellar medium. The engine released ∼ 10 50 − 10 51.5 erg over ∼ 10 3 − 10 5 s and resides within lowmass fast-moving material with equatorial-polar density asymmetry (M ej,fast 0.3 M ). Successful SNe from low-mass H-rich stars (like electron-capture SNe) or failed explosions from blue supergiants satisfy these constraints. Intermediate-mass black-holes are disfavored by the large environmental density probed by the radio observations.

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“…Some studies (e.g. Nadezhin 1980;Lovegrove & Woosley 2013;Sukhbold et al 2016;Fernández et al 2018) stress that is quite unlikely that the H envelope collapses entirely, even during a direct collapse, because it is loosely bound. In the following, we consider the two extreme cases in which f H = 0 (the H envelope is completely lost) and f H = 0.9 (90 % of the H envelope collapses).…”

Section: Compactness Modelmentioning

confidence: 99%

Impact of the Rotation and Compactness of Progenitors on the Mass of Black Holes

Mapelli

Spera

Montanari³

et al. 2020

ApJ

147

117

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We investigate the impact of stellar rotation on the formation of black holes (BHs), by means of our population-synthesis code sevn. Rotation affects the mass function of BHs in several ways. In massive metal-poor stars, fast rotation reduces the minimum zero-age main sequence (ZAMS) mass for a star to undergo pair instability and pulsational pair instability. Moreover, stellar winds are enhanced by rotation, peeling-off the entire hydrogen envelope. As a consequence of these two effects, the maximum BH mass we expect from the collapse a rotating metal-poor star is only ∼ 45 M , while the maximum mass of a BH born from a non-rotating star is ∼ 60 M . Furthermore, stellar rotation reduces the minimum ZAMS mass for a star to collapse into a BH from ∼ 18 − 25 M to ∼ 13 − 18 M . Finally, we have investigated the impact of different core-collapse supernova (CCSN) prescriptions on our results. While the threshold value of compactness for direct collapse and the fallback efficiency strongly affect the minimum ZAMS mass for a star to collapse into a BH, the fraction of hydrogen envelope that can be accreted onto the final BH is the most important ingredient to determine the maximum BH mass. Our results confirm that the interplay between stellar rotation, CCSNe and pair instability plays a major role in shaping the BH mass spectrum.

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Mass ejection in failed supernovae: variation with stellar progenitor

Cited by 115 publications

References 84 publications

Weak Shock Propagation with Accretion. II. Stability of Self-similar Solutions to Radial Perturbations

Weak Shock Propagation with Accretion. II. Stability of Self-similar Solutions to Radial Perturbations

An Embedded X-Ray Source Shines through the Aspherical AT 2018cow: Revealing the Inner Workings of the Most Luminous Fast-evolving Optical Transients

Impact of the Rotation and Compactness of Progenitors on the Mass of Black Holes

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