A physical model of mass ejection in failed supernovae

Coughlin, Eric R.; Quataert, Eliot; Fernández, Rodrigo; Kasen, Daniel

doi:10.1093/mnras/sty667

Cited by 38 publications

(51 citation statements)

References 46 publications

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“…We note, however, that our estimates of the BH mass may be overpredicted if, for instance, a significant amount of mass is loss via neutrinos during the final collapse (Coughlin et al 2018). Also, our simulations do not account self-consistently for binary interactions between the progenitor stars, which deserves further attention (Gotberg et al 2017;Marchant et al 2019).…”

Section: Discussionmentioning

confidence: 88%

“…Stars that undergo a PISN are expected to be fully disrupted and thus to leave no remnant behind. The final BH mass may depend on the mass of neutrinos lost during the collapse, assuming they are not accreted into the BH (Coughlin et al 2018). Without a fully consistent theory for BH formation, we use this simple value based on the binding energy, which provides an upper limit on the BH mass.…”

Section: Evolution Through the Pulsesmentioning

confidence: 99%

See 1 more Smart Citation

Mind the Gap: The Location of the Lower Edge of the Pair-instability Supernova Black Hole Mass Gap

Farmer

Renzo

Mink

et al. 2019

ApJ

366

409

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Detections of gravitational waves are now starting to probe the mass distribution of stellar mass black holes (BHs). Robust predictions from stellar models are needed to interpret these. Theory predicts the existence of a gap in the BH mass distribution because of pair-instability supernovae. The maximum BH mass below the gap is the result of pulsational mass loss. We evolve massive helium stars through their late hydrodynamical phases of evolution using the open-source MESA stellar evolution code. We find that the location of the lower edge of the mass gap at 45 M  is remarkably robust against variations in the metallicity (≈3 M ), the treatment of internal mixing (≈1 M ), and stellar wind mass loss (≈4 M ), making it the most robust predictor for the final stages of the evolution of massive stars. The reason is that the onset of the instability is dictated by the near-final core mass, which in turn sets the resulting BH mass. However, varying the a g C , O 12 16 () reaction rate within its 1σ uncertainties shifts the location of the gap between 40 M  and 56 M . We provide updated analytic fits for population synthesis simulations. Our results imply that the detection of merging BHs can provide constraints on nuclear astrophysics. Furthermore, the robustness against metallicity suggests that there is a universal maximum for the location of the lower edge of the gap, which is insensitive to the formation environment and redshift for first-generation BHs. This is promising for the possibility to use the location of the gap as a "standard siren" across the universe.

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Section: Discussionmentioning

confidence: 88%

Section: Evolution Through the Pulsesmentioning

confidence: 99%

Mind the Gap: The Location of the Lower Edge of the Pair-instability Supernova Black Hole Mass Gap

Farmer

Renzo

Mink

et al. 2019

ApJ

366

409

View full text Add to dashboard Cite

show abstract

“…This mechanism has been first proposed by Nadezhin (1980), and was further investigated by Lovegrove & Woosley (2013) and Lovegrove, Woosley & Zhang (2017). More recently, Fernández et al (2018) and Coughlin et al (2018a) focused on the resulting ejection of the star's outer layers via the shock formed by the steepening of the initial pressure pulse, using both analytical arguments and numerical investigations.…”

Section: Introductionmentioning

confidence: 92%

“…The famous point explosion problem was originally solved independently by Taylor, von-Neumann, and Sedov, using a self-similarity argument (Taylor 1950;Bethe et al 1958;Sedov 1959). Conservation of energy gives the scaling of the shock radius with time, while the pressure, density, and velocity profiles within the shocked region can be found analytically through the self-similar ansatz.…”

Section: Sedov-taylor Point Explosionmentioning

confidence: 99%

Partial stellar explosions – ejected mass and minimal energy

Linial

Fuller

Sari

2021

Monthly Notices of the Royal Astronomical Society

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Many massive stars appear to undergo enhanced mass-loss during late stages of their evolution. In some cases, the ejected mass likely originates from non-terminal explosive outbursts, rather than continuous winds. Here we study the dependence of the ejecta mass, mej, on the energy budget E of an explosion deep within the star, using both analytical arguments and numerical hydrodynamics simulations. Focusing on polytropic stellar models, we find that for explosion energies smaller than the stellar binding energy, the ejected mass scales as $m_{\rm ej} \propto E^{\varepsilon _{\rm m}}$, where εm = 2.4–3.0 depending on the polytropic index. The loss of energy due to shock breakout emission near the stellar edge leads to the existence of a minimal mass-shedding explosion energy, corresponding to a minimal ejecta mass. For a wide range of progenitors, from Wolf–Rayet stars to red supergiants (RSGs), we find a similar limiting energy of $E_{\rm min} \approx 10^{46}\!-\!10^{47} \rm \, erg$, almost independent of the stellar radius. The corresponding minimal ejecta mass varies considerably across different progenitors, ranging from ${\sim } 10^{-8} \, \rm M_\odot$ in compact stars, up to ${\sim } 10^{-2} \, \rm M_\odot$ in RSGs. We discuss implications of our results for pre-supernova outbursts driven by wave heating, and complications caused by the non-constant opacity and adiabatic index of realistic stars.

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“…where r 0 = 2.4 × 10 11 cm for the YSG (green curve in this figure) and r 0 = 3 × 10 11 cm for the RSG (red curve). The dashed lines give the analytic predictions for the total energy contained behind the shock, which scales as the square of the mass lost to neutrinos (it also depends less sensitively on the stellar structure; see Coughlin et al (2018) and column 11 of Table 2 of Fernández et al (2018) for more details). This demonstrates, as we argued above, that the YSG has a larger binding energy near the base of its hydrogen envelope due to the fact that the mass interior to r 0 is larger.…”

Section: Red Supergiantmentioning

confidence: 99%

Weak Shock Propagation with Accretion. I. Self-similar Solutions and Application to Failed Supernovae

Coughlin

Quataert

2018

ApJ

Self Cite

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We present solutions for the self-similar propagation of a shock wave in a hydrostatic, adiabatic medium with a point mass gravitational field. In contrast to the well-known, Sedov-Taylor blastwave, these solutions apply to the case when the shock Mach number is of order a few, and the energy of the shocked fluid is not conserved but self-consistently modified by the binding energy of the ambient medium that is swept up by the passage of the shock. Furthermore, we show that there is one solution (for a given ambient density profile) that smoothly passes through a sonic point in the post-shock flow and results in accretion onto the central object; in analogy with the Bondi problem, we propose that these solutions are the ones that are most relevant in astrophysical environments. We apply these accreting models to failed supernovae, in which neutron star formation does not unbind the envelope, but a weak shock is still generated in the outer layers of the star from neutrino-induced mass loss. We find excellent agreement between the predictions of our self-similar, shock propagation model and numerical simulations of the collapse of a yellow supergiant; the self-similar solutions reproduce the overall scaling of the shock speed, the time and space-dependent evolution of the velocity, density, and pressure behind the shock, and the accretion rate onto the black hole. Our results have important implications for the fallback and ejection of material in failed supernovae.

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A physical model of mass ejection in failed supernovae

Cited by 38 publications

References 46 publications

Mind the Gap: The Location of the Lower Edge of the Pair-instability Supernova Black Hole Mass Gap

Mind the Gap: The Location of the Lower Edge of the Pair-instability Supernova Black Hole Mass Gap

Partial stellar explosions – ejected mass and minimal energy

Weak Shock Propagation with Accretion. I. Self-similar Solutions and Application to Failed Supernovae

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