Neutrino-dominated Accretion and Supernovae

By K. Kohri, Ramesh Narayan, T. Piran. 2005

180 citations recorded by the source corpus.

We suggest that part of the infalling material during the core collapse of a massive star goes into orbit around the compact core to form a hot, dense, centrifugally supported accretion disk whose evolution is strongly influenced by neutrino interactions. Under a wide range of conditions, this neutrino-dominated accretion flow will be advection dominated and will develop a substantial outflowing wind. We estimate the energy carried out in the wind and find that it exceeds 1050 ergs for a wide range of parameters and even exceeds 1051 ergs for reasonable parameter choices. We propose that the wind energy will revive a stalled shock and will help produce a successful supernova explosion. We discuss the role of the disk wind in both prompt and delayed explosions. While both scenarios are feasible, we suggest that a delayed explosion is more likely and perhaps even unavoidable. Finally, we suggest that the disk wind may be a natural site for r-process nucleosynthesis.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/53f23e136c448058a1e62e2a48db96483f2f88ae

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. B. Metzger
2. Bing Zhang
3. Pawan Kumar
4. D. Kasen
5. Ramesh Narayan
6. J. McKinney
7. E. Quataert
8. Stan Woosley

In Nuclear and High Energy Physics

1. B. Metzger
2. Bing Zhang
3. Ramesh Narayan
4. Pawan Kumar
5. J. McKinney
6. A. Tchekhovskoy
7. D. Kasen
8. J. Dexter

Citations in the corpus

• SUPERNOVA LIGHT CURVES POWERED BY FALLBACK ACCRETION (2012, background): “The resulting mass outflow rate can be estimated following Kohri et al. (2005) by assuming that the accretion rate increases as some power of radius Ṁ(r) = Ṁfb ( r rfb )s , (1) where Ṁfb and rfb are the accretion rate and radius at the outer disk edge, and 0 < s < 1.”
• General relativistic magnetohydrodynamic simulations of the jet formation and large-scale propagation from black hole accretion systems (2006, methodology): “The chosen H/R and the extent of the disk are similar to the accretion disk that is expected to form in the collapsar model (MacFadyen & Woosley 1999; Kohri & Mineshige 2002; Kohri et al. 2005).”
• The Supernova Gamma-Ray Burst Connection (2006, background): “The supernova, and the 56Ni to make it bright, are produced by a disk “wind” (MacFadyen and Woosley, 1999; MacFadyen, 2003; Kohri et al., 2005).”
• Nucleosynthesis in the Outflow from Gamma-Ray Burst Accretion Disks (2005, background): “Therefore neutrino trapping in these disks is under study by several groups, e.g. Lee et al (2004); Rosswog et al (2003); Kohri et al (2005); Janiuk et al (2005); Setiawan et al. (2004).”
• The physics of gamma-ray bursts & relativistic jets (2014, methodology): “An approximate solution to the disk structure in the NDAF and ADAF regimes can be written in the following forms using results of numerical calculations [689,691,707,708,696,698]: NDAF:”
• Mass fall-back and accretion in the central engine of gamma-ray bursts (2008, methodology): “We compute the mass in-fall rate during the collapse of the massive star, and the viscous accretion rate on to the central BH using ideas from Narayan et al. (2001) and Kohri et al. (2005).”
• A Reconnection Switch to Trigger gamma-Ray Burst Jet Dissipation (2010, methodology): “For more details, see Kohri et al. (2005).”
• Neutrino-cooled Accretion Disks around Spinning Black Holes (2006, background): “383 degenerate disks, and Kohri et al. (2005) studied the realistic mildly degenerate disks.”
• Neutrino-dominated accretion flows as the central engine of gamma-ray bursts (2017, methodology): “If we assume that the heaviest nuclei is 4He, by combing with the above equations, the bridging formula can be simplified as (Liu et al. 2007) Ye = 1 2 (1 − Xnuc) + Xnuc 1 + exp{ [1+ f (τν )]µe−Q kBT } , (32) where Xnuc is the mass fraction of free nucleons (e.g., Di Matteo et al. 2002; Kohri et al.”
• Three-dimensional GRMHD Simulations of Neutrino-cooled Accretion Disks from Neutron Star Mergers (2017, background): “…be cooled by thermal neutrino emission (Popham et al. 1999; Narayan et al. 2001; Kohri & Mineshige 2002; Di Matteo et al. 2002; Beloborodov 2003; Kohri et al. 2005; Kawanaka & Mineshige 2007; Chen & Beloborodov 2007), a process that affects the lepton number of the disk in addition to its…”
• Equation of state in relativistic magnetohydrodynamics: variable versus constant adiabatic index (2007, background): “…for a combination of protons, neutrons, electrons, positrons, and neutrinos, etc. and must include the effects of electron degeneracy, neutronization, photodisintegration, optical depth of neutrinos, etc. (Popham et al. 1999; Di Matteo et al. 2002; Kohri & Mineshige 2002; Kohri et al. 2005).”