Are pulsars spun up or down by SASI spiral modes?

Abstract

Pulsars may either be spun up or down by hydrodynamic instabilities during the supernova explosion of massive stars. Besides rapidly-rotating cases related to bipolar explosions, stellar rotation may affect the explosion of massive stars in the more common situations where the centrifugal force is minor. Using 2D simulations of a simplified setup in cylindrical geometry, we examine the impact of rotation on the Standing Accretion Shock Instability (SASI) and the corotation instability, also known as low-T/|W|. The influence of rotation on the saturation amplitude of these instabilities depends on the specific angular momentum in the accretion flow and the ratio of the shock to the neutron star radii. The spiral mode of SASI becomes more vigorous with faster rotation only if this ratio is large enough. A corotation instability develops at large rotation rates and impacts the dynamics more dramatically, leading to a strong one-armed spiral wave. Non-axisymmetric instabilities are able to redistribute angular momentum radially and affect the pulsar spin at birth. A systematic study of the relationship between the core rotation period of the progenitor and the initial pulsar spin is performed. Stellar rotation rates for which pulsars are spun up or down by SASI are estimated. Rapidly spinning progenitors are modestly spun down by spiral modes, less than $\sim 30\%$, when a corotation instability develops. Given the observational constraints on pulsar spin periods at birth, this suggests that rapid rotation might not play a significant hydrodynamic role in most core-collapse supernovae.

13 pages, 11 figures, accepted for publication in MNRAS. Minor changes following the referee report, figures 1 and 2 added

References in corpus (16)

• Binary interaction dominates the evolution of massive stars
• A High Order Godunov Scheme with Constrained Transport and Adaptive Mesh Refinement for Astrophysical MHD
• Delayed neutrino-driven supernova explosions aided by the standing accretion-shock instability
• Three-dimensional core-collapse supernova simulated using a 15 $M_{\odot }$ progenitor
• Instability of a stalled accretion shock: evidence for the advective-acoustic cycle
• Pulsar spins from an instability in the accretion shock of supernovae
• The Status of Multi-Dimensional Core-Collapse Supernova Models
• Semi-global simulations of the magneto-rotational instability in core collapse supernovae
• Special Relativistic Simulations of Magnetically-dominated Jets in Collapsing Massive Stars
• The Dynamics of Neutrino-Driven Supernova Explosions after Shock Revival in 2D and 3D
• Hydrodynamical Neutron Star Kicks in Three Dimensions
• Magnetic field amplification and magnetically supported explosions of collapsing, non-rotating stellar cores
• Effect of Rotation on the Stability of a Stalled Cylindrical Shock and its Consequences for Core-Collapse Supernovae
• Impacts of Rotation on Three-dimensional Hydrodynamics of Core-collapse Supernovae
• Critical Surface for Explosions of Rotational Core-Collapse Supernovae
• The intimate relation between the low T/W instability and the co-rotation point

Cited by in corpus (38)

• Hydrodynamics of core-collapse supernovae and their progenitors
• Self-consistent 3D Supernova Models From -7 Minutes to +7 Seconds: a 1-bethe Explosion of a ~19 Solar-mass Progenitor
• Rotation-supported Neutrino-driven Supernova Explosions in Three Dimensions and the Critical Luminosity Condition
• Gravitational waves from three-dimensional core-collapse supernova models: The impact of moderate progenitor rotation
• Magnetorotational Explosion of A Massive Star Supported by Neutrino Heating in General Relativistic Three Dimensional Simulations
• Core-collapse supernova simulations in one and two dimensions: comparison of codes and approximations
• Supernova Fallback as Origin of Neutron Star Spins and Spin-kick Alignment
• Impact of Neutrino Opacities on Core-Collapse Supernova Simulations
• Characteristic Time Variability of Gravitational-Wave and Neutrino Signals from Three-dimensional Simulations of Non-Rotating and Rapidly Rotating Stellar Core-Collapse
• The imprints of the last jets in core collapse supernovae
• Interplay Between Neutrino Kicks and Hydrodynamic Kicks of Neutron Stars and Black Holes
• Three-dimensional core-collapse supernovae with complex magnetic structures: II. Rotational instabilities and multi-messenger signatures
• Insights into non-axisymmetric instabilities in three-dimensional rotating supernova models with neutrino and gravitational-wave signatures
• Supplying angular momentum to the jittering jets explosion mechanism using inner convection layers
• Identifying rotation in SASI-dominated core-collapse supernovae with a neutrino gyroscope
• Reviving the stalled shock by jittering jets in core collapse supernovae: jets from the standing accretion shock instability
• Neutron star natal kick and jets in core collapse supernovae
• Imprints of the jittering jets explosion mechanism in the morphology of the supernova remnant SNR 0540-69.3
• Remnant masses of core collapse supernovae in the jittering jets explosion mechanism
• Effects of rotation and magnetic field on the revival of a stalled shock in supernova explosions
• Explaining the morphology of supernova remnant (SNR) 1987A with the jittering jets explosion mechanism
• The impact of progenitor asymmetries on the neutrino-driven convection in core-collapse supernovae
• Effect of stellar rotation on the development of post-shock instabilities during core-collapse supernovae
• Amplifying magnetic fields of a newly born neutron star by stochastic angular momentum accretion in core collapse supernovae
• The non-linear onset of neutrino-driven convection in two and three-dimensional core-collapse supernovae
• The jittering jets explosion mechanism (JJEM) in electron capture supernovae
• Standing Accretion Shock Instability in the Collapse of a Rotating Stellar Core
• Tracing the evolution of short-period binaries with super-synchronous fast rotators
• Reviving the stalled shock by jittering jets in core collapse supernovae: The key role of magnetic fields
• Possible indications for jittering jets in core collapse supernova explosion simulations
• Enhanced mass-loss rate evolution of stars with $\gtrsim 18M_{\odot }$ and missing optically-observed type II core-collapse supernovae
• Storing magnetic fields in pre-collapse cores of massive stars
• Low energy core collapse supernovae in the frame of the jittering jets explosion mechanism
• Magnetized SASI: its mechanism and possible connection to some QPOs in XRBs
• Post-explosion positive jet-feedback activity in inner ejecta of core collapse supernovae
• The rotational shear in pre-collapse cores of massive stars
• A minority view on the majority: A personal meeting summary on the explosion mechanism of supernovae
• Circular polarization of gravitational waves from magnetorotational supernovae