The Dynamics of Neutrino-Driven Supernova Explosions after Shock Revival in 2D and 3D

Abstract

We study the growth of the explosion energy after shock revival in neutrino-driven explosions in two and three dimensions (2D/3D) using multi-group neutrino hydrodynamics simulations of an $11.2M_{\odot }$ star. The 3D model shows a faster and steadier growth of the explosion energy and already shows signs of subsiding accretion after one second. By contrast, the growth of the explosion energy in 2D is unsteady, and accretion lasts for several seconds as confirmed by additional long-time simulations of stars of similar masses. Appreciable explosion energies can still be reached, albeit at the expense of rather high neutron star masses. In 2D, the binding energy at the gain radius is larger because the strong excitation of downward-propagating g-modes removes energy from the freshly accreted material in the downflows. Consequently, the mass outflow rate is considerably lower in 2D than in 3D. This is only partially compensated by additional heating by outward-propagating acoustic waves in 2D. Moreover, the mass outflow rate in 2D is reduced because much of the neutrino energy deposition occurs in downflows or bubbles confined by secondary shocks without driving outflows. Episodic constriction of outflows and vertical mixing of colder shocked material and hot, neutrino-heated ejecta due to Rayleigh-Taylor instability further hamper the growth of the explosion energy in 2D. Further simulations will be necessary to determine whether these effects are generic over a wider range of supernova progenitors.

25 pages, 24 figures, accepted for publication in MNRAS. Minor revisions, wrong panel in Figure 4 corrected

References in corpus (18)

• Delayed neutrino-driven supernova explosions aided by the standing accretion-shock instability
• Three-Dimensional Simulations of Core-Collapse Supernovae: From Shock Revival to Shock Breakout
• Instability of a stalled accretion shock: evidence for the advective-acoustic cycle
• The Role of Turbulence in Neutrino-Driven Core-Collapse Supernova Explosions
• Neutrino-driven supernova of a low-mass iron-core progenitor boosted by three-dimensional turbulent convection
• Criteria for Core-Collapse Supernova Explosions by the Neutrino Mechanism
• Equation-of-State Dependent Features in Shock-Oscillation Modulated Neutrino and Gravitational-Wave Signals from Supernovae
• Features of the Acoustic Mechanism of Core-Collapse Supernova Explosions
• Gravitational Waves from Core Collapse Supernovae
• Neutrino emission characteristics and detection opportunities based on three-dimensional supernova simulations
• Improved constrained scheme for the Einstein equations: An approach to the uniqueness issue
• On The Intrinsic Diversity of Type II-Plateau Supernovae
• Interplay of Neutrino Opacities in Core-collapse Supernova Simulations
• Magnetic field amplification and magnetically supported explosions of collapsing, non-rotating stellar cores
• An axis-free overset grid in spherical polar coordinates for simulating 3D self-gravitating flows
• Impacts of Rotation on Three-dimensional Hydrodynamics of Core-collapse Supernovae
• Nonlinear Saturation of g-modes in Proto-Neutron Stars: Quieting the Acoustic Engine
• Does energy of type IIP supernovae depends on stellar mass?

Cited by in corpus (8)

• The Status of Multi-Dimensional Core-Collapse Supernova Models
• Neutron star kicks by the gravitational tug-boat mechanism in asymmetric supernova explosions: progenitor and explosion dependence
• Three-Dimensional Supernova Explosion Simulations of 9-, 10-, 11-, 12-, and 13-M${}_{\odot }$ Stars
• Rotation-supported Neutrino-driven Supernova Explosions in Three Dimensions and the Critical Luminosity Condition
• Spectropolarimetry of superluminous supernovae: insight into their geometry
• The $\nu$-process with fully time-dependent supernova neutrino emission spectra
• A Critical Assessment of Turbulence Models for 1D Core-Collapse Supernova Simulations
• APSARA: A multi-dimensional unsplit fourth-order explicit Eulerian hydrodynamics code for arbitrary curvilinear grids