Viscosity and Rotation in Core-Collapse Supernovae

By T. Thompson, E. Quataert, Adam Burrows. 2004

187 citations recorded by the source corpus.

We construct models of core-collapse supernovae in one spatial dimension, including rotation, angular momentum transport, and viscous dissipation employing an α-prescription. We compare the evolution of a fiducial 11 M☉ nonrotating progenitor with its evolution when including a wide range of imposed initial rotation profiles (1.25 s < P0 < 8 s, where P0 is the initial, approximately solid-body, rotation period of the iron core). This range of P0 covers the region of parameter space from where rotation begins to modify the dynamics (P0 ~ 8 s) to where angular velocities at collapse approach Keplerian (P0 ~ 1 s). Under the assumption of strict angular momentum conservation, all models in this range leave behind neutron stars with spin periods ≲10 ms, shorter than those of most radio pulsars but similar to those expected theoretically for magnetars at birth. A fraction of the gravitational binding energy of collapse is stored in the free energy of differential rotation. This energy source may be tapped by viscous processes, providing a mechanism for energy deposition that is not strongly coupled to the mass accretion rate through the stalled supernova shock. This effect yields qualitatively new dynamics in models of supernovae. We explore several potential mechanisms for viscosity in the core-collapse environment: neutrino viscosity, turbulent viscosity caused by the magnetorotational instability (MRI), and turbulent viscosity by entropy- and composition gradient-driven convection. We argue that the MRI is the most effective. We find for rotation periods in the range P0 ≲ 5 s and a range of viscous stresses that the postbounce dynamics is significantly affected by the inclusion of this extra energy deposition mechanism; in several cases we obtain strong supernova explosions.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/af309dc0c12b336d40266fac4727b772ef557132

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Citations in the corpus

Magnetized relativistic jets and long-duration GRBs from magnetar spin-down during core-collapse supernovae (2009, background): “…in the few hundred milliseconds after a successful explosion is discussed in detail in a number of papers (Burrows, Hayes & Fryxell 1995; Janka & Mueller 1995; Thompson et al. 2005; Scheck et al. 2006; Arcones, Janka & Scheck 2007; see, in particular, figs 9 and 11 of Thompson et al. 2005 and fig.”
Non-spherical core collapse supernovae - II. The late-time evolution of globally anisotropic neutrino-driven explosions and their implications for SN 1987 A (2005, background): “Also magneto-rotational instabilities were suggested to aid the explosion by creating viscous heating behind the shock in addition to the still dominant energy input there by neutrinos (Thompson et al. 2005).”
Semi-global simulations of the magneto-rotational instability in core collapse supernovae (2008, background): “…energy into the post-shock stellar matter the MRI might thus be important for the currently favored neutrino-driven core collapse supernova explosion mechanism (e.g. Thompson et al. 2005; Janka et al. 2007), although possibly only for rapidly and strongly differentially rotating progenitors.”
Neutrino-dominated Accretion and Supernovae (2005, background): “Related ideas have been discussed by MacFadyen (2003) and Thompson et al. (2005).”
THE LANDSCAPE OF THE NEUTRINO MECHANISM OF CORE-COLLAPSE SUPERNOVAE: NEUTRON STAR AND BLACK HOLE MASS FUNCTIONS, EXPLOSION ENERGIES, AND NICKEL YIELDS (2014, background): “Similarly, there are other new and potentially interesting heating mechanisms such as magnetic dissipation (Thompson et al. 2005), damping of Alfvenic waves, and magnetic fields, possibly combined with rotation (e.g. Iwakami et al. 2014; Nakamura et al. 2014a; Sawai et al. 2013; Sawai & Yamada…”
NEW TWO-DIMENSIONAL MODELS OF SUPERNOVA EXPLOSIONS BY THE NEUTRINO-HEATING MECHANISM: EVIDENCE FOR DIFFERENT INSTABILITY REGIMES IN COLLAPSING STELLAR CORES (2012, background): “This could, for example, provide an explanation for the late explosions of a 15M⊙ star of Marek & Janka (2009) and Müller et al. (2012), which are associated with strong shock oscillations.”
Two-Dimensional Multiangle, Multigroup Neutrino Radiation-Hydrodynamic Simulations of Postbounce Supernova Cores (2008, background): “This results in a greater neutrino energy deposition efficiency behind the shock and, thus, creates more favorable conditions for explosion (Burrows & Goshy 1993; Janka 2001; Thompson et al. 2005; Marek & Janka 2007).”
Colloquium: Perspectives on core-collapse supernova theory (2012, background): “A useful approximate condition for explosion is when the characteristic neutrino heating time in the gain region (τH) exceeds the advection time (τadv) through it (Thompson et al. 2005; Janka 2001).”
Simulations of Magnetically Driven Supernova and Hypernova Explosions in the Context of Rapid Rotation (2007, background): “…et al. 2003; Yamada & Sawai 2004; Kotake et al. 2004; Mizuno et al. 2004; Takiwaki et al. 2004; Akiyama & Wheeler 2005; Ohnishi et al. 2006; Sawai et al. 2005; Thompson et al. 2005; Proga 2005;Wilson et al. 2005;Moiseenko et al. 2006; Matt et al. 2006; Masada et al. 2007; Shibata et al. 2006).”
BLACK HOLE FORMATION IN FAILING CORE-COLLAPSE SUPERNOVAE (2010, methodology): “This is common practice in stellar evolution codes (e.g., Heger et al. 2000) an hs also been applied to Newtonian 1D stellar collapse calculations (Akiyama et al. 2003; Thompson et al. 2005).”
Two-dimensional hydrodynamic core-collapse supernova simulations with spectral neutrino transport - I. Numerical method and results for a 15 solar mass star (2005, background): “Further, Thompson et al. (2005) have recently shown that neutrino viscocity, which is connected with the non-diagonal elements of the Eddington tensors, is of minor importance.”