Simulations of Magnetically Driven Supernova and Hypernova Explosions in the Context of Rapid Rotation

By Adam Burrows, L. Dessart, E. Livne, Christian D. Ott, J. Murphy. 2007

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We present here the first 2D rotating, multigroup, radiation magnetohydrodynamics (RMHD) simulations of supernova core collapse, bounce, and explosion. In the context of rapid rotation, we focus on the dynamical effects of magnetic stresses and the creation and propagation of MHD jets. We find that a quasi-steady state can be quickly established after bounce, during which a well-collimated MHD jet is maintained by continuous pumping of power from the differentially rotating core. If the initial spin period of the progenitor core is ≲2 s, the free energy reservoir in the secularly evolving proto-neutron star is adequate to power a supernova explosion and may be enough for a hypernova. The jets are well collimated by the infalling material and magnetic hoop stresses and maintain a small opening angle. We see evidence of sausage instabilities in the emerging jet stream. Neutrino heating is subdominant in the rapidly rotating models we explore but can contribute 10%-25% to the final explosion energy. Our simulations suggest that even in the case of modest or slow rotation, a supernova explosion might be followed by a secondary, weak MHD jet explosion, which, because of its weakness, may to date have gone unnoticed in supernova debris. Furthermore, we suggest that the generation of a nonrelativistic MHD precursor jet during the early proto-neutron star/supernova phase is implicit in both the collapsar and "millisecond magnetar" models of GRBs. The multidimensional, multigroup, rapidly rotating RMHD simulations we describe here are a start along the path toward more realistic simulations of the possible role of magnetic fields in some of nature's most dramatic events.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/3d9ec3b80a15c1881ef48b65c8756c3146c41750

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Citations in the corpus

Pulsational Pair-instability Supernovae (2016, background): “…studies of MHD core collapse (LeBlanc & Wilson 1970; Meier et al. 1976; Müller & Hillebrandt 1979; Akiyama et al. 2003; Ardeljan et al. 2005; Burrows et al. 2007; Dessart et al. 2008; Takiakai & Kotake 2011; Mösta et al. 2014, 2015) universally show jets or strong bipolar outflows…”
MAGNETOROTATIONALLY DRIVEN SUPERNOVAE AS THE ORIGIN OF EARLY GALAXY r-PROCESS ELEMENTS? (2012, background): “…the up to now microphysically most complete two-dimensional axisymmetric study of MHD-CCSN with multi-group flux-limited diffusion neutrino transport performed by Burrows et al. (2007) has shown, that neutrino heating contributes only 10%−−25% to the explosion energy and is therefore subdominant.”
On the nature of supernovae Ib and Ic (2012, background): “…asymmetry of the shock in an explosion through the neutrino mechanism (Scheck et al. 2006; Marek & Janka 2009) or the magnetorotational mechanism (LeBlanc & Wilson 1970; Bisnovatyi-Kogan, Popov & Samokhin 1976; Khokhlov et al. 1999; Maeda et al. 2002; Burrows et al. 2007; Dessart et al. 2008).”
The Proto-Magnetar Model for Gamma-Ray Bursts (2010, background): “Only recently, however, have simulations begun to capture the combined effects of MHD and neutrino heating (e.g. Burrows et al. 2007).”
Simulations of ultrarelativistic magnetodynamic jets from gamma‐ray burst engines (2008, background): “Burrows et al. (2007) find that a relativistic jet in the collapsar scenario may be preceded by a non-relativistic precursor jet that might clear the way for the second, relativistic jet.”
Colloquium: Perspectives on core-collapse supernova theory (2012, background): “For overall perspectives, I point to Bethe (1988;1990), Janka (2001,2012), Janka et al. (2007), Burrows et al. (1995,2007ab), Herant et al. (1994), Kotake, Sato, & Takahashi (2006), Kotake et al. (2012ab), Burrows (2000), and Mezzacappa (2005).”
A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMICS CODE FOR CORE-COLLAPSE SUPERNOVAE. II. RELATIVISTIC EXPLOSION MODELS OF CORE-COLLAPSE SUPERNOVAE (2012, background): “…2006, 2009), while the former Arizona group did not obtain neutrino-driven explosions at all with their 2D MGFLD code Vulcan (Livne et al. 2004, 2007) but found acoustic explosions powered by sound waves created by violent dipolar oscillations of the protoneutron star (Burrows et al. 2006, 2007b).”
A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMIC CODE FOR CORE-COLLAPSE SUPERNOVAE. I. METHOD AND CODE TESTS IN SPHERICAL SYMMETRY (2010, background): “…1996; Buras et al. 2006b, 2006a; Bruenn et al. 2006) and the standing accretion-shock instability (SASI; Blondin et al. 2003), or by some alternative mechanism, such as MHD effects (e.g., Burrows et al. 2007 and references therein), or energy deposition by acoustic waves (Burrows et al. 2006b).”
BLACK HOLE FORMATION IN FAILING CORE-COLLAPSE SUPERNOVAE (2010, background): “Left out of this picture are potential magnetohydrodynamics contributions t the explosion mechanism and energetics (cf. Burrows et al. 2007b).”
Evolution and fate of very massive stars (2013, background): “They find that fast rotating stars with an initial mass below about 200 M retain enough angular momentum in their cores in order to produce a collapsar ( j > jKerr, lso; Woosley 1993) or a magnetar (see e.g. Wheeler et al. 2000; Burrows et al. 2007; Dessart, O’Connor & Ott 2012c).”
Semi-global simulations of the magneto-rotational instability in core collapse supernovae (2008, background): “…to now, there exist only global simulations of MHD core collapse supernovae, which evolve the entire core of a massive star through gravitational collapse, bounce, and explosion (e.g., Kotake et al. 2004; Yamada & Sawai 2004; Takiwaki et al. 2004; Obergaulinger et al. 2006b,a; Burrows et al. 2007).”
MAGNETOROTATIONAL CORE-COLLAPSE SUPERNOVAE IN THREE DIMENSIONS (2014, background): “4s; Ott et al. 2006; Burrows et al. 2007) and an efficient process to rapidly amplify the likely weak 1 TAPIR, Mailcode 350-17, California Institute of Technology, Pasadena, CA 91125, USA, pmoesta@tapir.caltech.edu 2 Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU WPI),…”
Superluminous supernovae: 56Ni power versus magnetar radiation (2012, background): “Today, highly energetic magneto-rotational explosion are expected to be the most suitable means to produce super-luminos SNe (Burrows et al. 2007).”
DIMENSION AS A KEY TO THE NEUTRINO MECHANISM OF CORE-COLLAPSE SUPERNOVA EXPLOSIONS (2010, methodology): “Two-dimensional models also enable accretion in one quadrant to power explosion in another (Burrows et al. 2007b), something impossible in 1D and one reason neutrino-driven explosions in 1D are generally thwarted.”
NEUTRINO SIGNATURES AND THE NEUTRINO-DRIVEN WIND IN BINARY NEUTRON STAR MERGERS (2008, methodology): “…(Rosswog & Price 2007) and taken a few milliseconds after coalescence, we perform two-dimensional (axisymmetric) multi-group fluxlimited-diffusion (MGFLD) radiation hydrodynamics simulations using the code VULCAN/2D (Livne et al. 2004; Dessart et al. 2006a; Burrows et al. 2007b; Ott et al. 2008).”
Two-Dimensional Multiangle, Multigroup Neutrino Radiation-Hydrodynamic Simulations of Postbounce Supernova Cores (2008, methodology): “The module implementing 2D transport in the MGFLD approximation, evolving the zeroth moment of the radiation field, is discussed in Burrows et al. (2007c).”