Hydrodynamics of core-collapse supernovae and their progenitors

Müller, Bernhard

doi:10.1007/s41115-020-0008-5

Cited by 161 publications

(88 citation statements)

References 480 publications

(906 reference statements)

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“…In the last decade significant progress has been made in the development of numerical codes, in particular in the treatment of multidimensional effects [12]. In the case of neutrino-driven explosions, the GW emission is primarly induced by instabilities developed at the newly formed proto-neutron star (PNS) and by the non-spherical accreting flow of hot matter over its surface [13].…”

Section: Introductionmentioning

confidence: 99%

Inference of protoneutron star properties from gravitational-wave data in core-collapse supernovae

et al. 2021

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The eventual detection of gravitational waves from core-collapse supernovae (CCSN) will help improve our current understanding of the explosion mechanism of massive stars. The stochastic nature of the late post-bounce gravitational wave signal due to the non-linear dynamics of the matter involved and the large number of degrees of freedom of the phenomenon make the source parameter inference problem very challenging. In this paper we take a step towards that goal and present a parameter estimation approach which is based on the gravitational waves associated with oscillations of proto-neutron stars (PNS). Numerical simulations of CCSN have shown that buoyancy-driven g-modes are responsible for a significant fraction of the gravitational wave signal and their time-frequency evolution is linked to the physical properties of the compact remnant through universal relations, as demonstrated in [1]. We use a set of 1D CCSN simulations to build a model that relates the evolution of the PNS properties with the frequency of the dominant g-mode, which is extracted from the gravitational-wave data using a new algorithm we have developed for our study. The model is used to infer the time evolution of a combination of the mass and the radius of the PNS. The performance of the method is estimated employing simulations of 2D CCSN waveforms covering a progenitor mass range between 11 and 40 solar masses and different equations of state. Considering signals embedded in Gaussian gravitational wave detector noise, we show that it is possible to infer PNS properties for a galactic source using Advanced LIGO and Advanced Virgo data at design sensitivities. Third generation detectors such as Einstein Telescope and Cosmic Explorer will allow to test distances of O(100 kpc).

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Section: Introductionmentioning

confidence: 99%

Inference of protoneutron star properties from gravitational-wave data in core-collapse supernovae

et al. 2021

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“…They obtain parameters 3 of ln A C19 = −2.98 ± 0.13 and n C19 = 0.74 ± 0.04. In contrast, Meakin & Arnett (2007) report ln A M07 = 0.062 ± 0.87 and n M07 = 1.05 ± 0.21 and also the results of Jones et al (2017) and Andrassy et al (2020) agree with an exponent of n ≈ 1, as pointed out by Müller (2020). Further simulations are needed to scrutinize the values of A and n, also keeping in mind that different values may exist for different stellar convection zones.…”

Section: Convective Boundary Mixingmentioning

confidence: 85%

Multidimensional low-Mach number time-implicit hydrodynamic simulations of convective helium shell burning in a massive star

Horst

Hirschi

Edelmann

et al. 2021

A&A

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Context.A realistic parametrization of convection and convective boundary mixing in conventional stellar evolution codes is still the subject of ongoing research. To improve the current situation, multidimensional hydrodynamic simulations are used to study convection in stellar interiors. Such simulations are numerically challenging, especially for flows at low Mach numbers which are typical for convection during early evolutionary stages. Aims. We explore the benefits of using a low-Mach hydrodynamic flux solver and demonstrate its usability for simulations in the astrophysical context. Simulations of convection for a realistic stellar profile are analyzed regarding the properties of convective boundary mixing. Methods. The time-implicit Seven-League Hydro (SLH) code was used to perform multidimensional simulations of convective helium shell burning based on a 25 M⊙ star model. The results obtained with the low-Mach AUSM + -up solver were compared to results when using its non low-Mach variant AUSM + B -up. We applied well-balancing of the gravitational source term to maintain the initial hydrostatic background stratification. The computational grids have resolutions ranging from 180 × 90 2 to 810 × 540 2 cells and the nuclear energy release was boosted by factors of 3 × 10 3 , 1 × 10 4 , and 3 × 10 4 to study the dependence of the results on these parameters. Results. The boosted energy input results in convection at Mach numbers in the range of 10 −3 to 10 −2 . Standard mixing-length theory (MLT) predicts convective velocities of about 1.6 × 10 −4 if no boosting is applied. The simulations with AUSM + -up show a Kolmogorov-like inertial range in the kinetic energy spectrum that extends further toward smaller scales compared with its non low-Mach variant. The kinetic energy dissipation of the AUSM + -up solver already converges at a lower resolution compared to AUSM + B -up. The extracted entrainment rates at the boundaries of the convection zone are well represented by the bulk Richardson entrainment law and the corresponding fitting parameters are in agreement with published results for carbon shell burning. However, our study needs to be validated by simulations at higher resolution. Further, we find that a general increase in the entropy in the convection zone may significantly contribute to the measured entrainment of the top boundary. Conclusion.This study demonstrates the successful application of the AUSM + -up solver to a realistic astrophysical setup. Compressible simulations of convection in early phases at nominal stellar luminosity will benefit from its low-Mach capabilities. Similar to other studies, our extrapolated entrainment rate for the helium-burning shell would lead to an unrealistic growth of the convection zone if it is applied over the lifetime of the zone. Studies at nominal stellar luminosities and different phases of the same convection zone are needed to detect a possible evolution of the entrainment rate and the impact of radiation on convective boundary mixing.

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“…Conversely, literature values for A vary from A ≈ 1 (Meakin & Arnett 2007) to A ≈ 0.05 (Cristini et al 2019). See Müller (2020) and references therein for examples of entrainment law parameters derived from 3D simulation results. The fact that A and n are not the same between setups suggests that the entrainment law in its current form does not encompass every aspect of the growth of the convective region in these simulations.…”

Section: Dependence Of Entrainment On the Entrainment Law Parametersmentioning

confidence: 99%

“…1 in Brott et al 2011) and asteroseismic frequencies (Aerts et al 2018). E-mail: l.j.a.scott@keele.ac.uk Both 3D hydrodynamics simulations and observations can be compared to 1D models incorporating CBM and other mixing processes, such as waves (Meakin & Arnett 2007;Jones et al 2017;Edelmann et al 2019;Müller 2020;Pratt et al 2020). Incorporating 3D hydrodynamics results, such as convective regions that grow as a result of entrainment, into 1D models also allows them to be studied on evolutionary time-scales.…”

Section: Introductionmentioning

confidence: 99%

Convective core entrainment in 1D main-sequence stellar models

Scott

Hirschi

Georgy

et al. 2021

Monthly Notices of the Royal Astronomical Society

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3D hydrodynamics models of deep stellar convection exhibit turbulent entrainment at the convective-radiative boundary which follows the entrainment law, varying with boundary penetrability. We implement the entrainment law in the 1D Geneva stellar evolution code. We then calculate models between 1.5 and 60 M⊙ at solar metallicity (Z = 0.014) and compare them to previous generations of models and observations on the main sequence. The boundary penetrability, quantified by the bulk Richardson number, RiB, varies with mass and to a smaller extent with time. The variation of RiB with mass is due to the mass dependence of typical convective velocities in the core and hence the luminosity of the star. The chemical gradient above the convective core dominates the variation of RiB with time. An entrainment law method can therefore explain the apparent mass dependence of convective boundary mixing through RiB. New models including entrainment can better reproduce the mass dependence of the main sequence width using entrainment law parameters A ∼ 2 × 10−4 and n = 1. We compare these empirically constrained values to the results of 3D hydrodynamics simulations and discuss implications.

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Hydrodynamics of core-collapse supernovae and their progenitors

Cited by 161 publications

References 480 publications

Inference of protoneutron star properties from gravitational-wave data in core-collapse supernovae

Inference of protoneutron star properties from gravitational-wave data in core-collapse supernovae

Multidimensional low-Mach number time-implicit hydrodynamic simulations of convective helium shell burning in a massive star

Convective core entrainment in 1D main-sequence stellar models

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