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Hypercritical Advection Dominated Accretion Flow  [PDF]
G. E. Brown,C. -H. Lee,H. A. Bethe
Physics , 1999, DOI: 10.1086/309454
Abstract: In this note we study the accretion disc that arises in hypercritical accretion of $\dot M\sim 10^8 M_{\rm Edd}$ onto a neutron star while it is in common envelope evolution with a massive companion. In order to raise the temperature high enough that the disc might cool by neutrino emission, Chevalier found a small value of the $\alpha$-parameter, where the kinematic coefficient of shear viscosity is $\nu=\alpha c_s H$, with $c_s$ the velocity of sound and $H$ the disc height; namely, $\alpha\sim 10^{-6}$ was necessary for gas pressure to dominate. He also considered results with higher values of $\alpha$, pointing out that radiation pressure would then predominate. With these larger $\alpha$'s, the temperatures of the accreting material are much lower, $\lsim 0.35$ MeV. The result is that neutrino cooling during the flow is negligible, satisfying very well the advection dominating conditions. The low temperature of the accreting material means that it cannot get rid of its energy rapidly by neutrino emission, so it piles up, pushing its way through the accretion disc. An accretion shock is formed, far beyond the neutron star, at a radius $\gsim 10^8$ cm, much as in the earlier spherically symmetric calculation, but in rotation. Two-dimensional numerical simulation shows that an accretion disc is reformed inside of the accretion shock, allowing matter to accrete onto the neutron star with pressure high enough so that neutrinos can carry off the energy.
Hypercritical Accretion, Induced Gravitational Collapse, and Binary-Driven Hypernovae  [PDF]
Chris L. Fryer,Jorge A. Rueda,Remo Ruffini
Physics , 2014, DOI: 10.1088/2041-8205/793/2/L36
Abstract: The induced gravitational collapse (IGC) paradigm has been successfully applied to the explanation of the concomitance of gamma-ray bursts (GRBs) with supernovae (SNe) Ic. The progenitor is a tight binary system composed by a carbon-oxygen (CO) core and a neutron star (NS) companion. The explosion of the SN leads to hypercritical accretion onto the NS companion which reaches the critical mass, hence inducing its gravitational collapse to a black hole (BH) with consequent emission of the GRB. The first estimates of this process were based on a simplified model of the binary parameters and the Bondi-Hoyle-Lyttleton accretion rate. We present here the first full numerical simulations of the IGC phenomenon. We simulate the core-collapse and SN explosion of CO stars to obtain the density and ejection velocity of the SN ejecta. We follow the hydrodynamic evolution of the accreting material falling into the Bondi-Hoyle surface of the NS all the way up to its incorporation to the NS surface. The simulations go up to BH formation when the NS reaches the critical mass. For appropriate binary parameters the IGC occurs in short timescales (100-1000s) owing to the combined effective action of the photon trapping and the neutrino cooling near the NS surface. We also show that the IGC scenario leads to a natural explanation for why GRBs are associated only to SN Ic with totally absent or very little helium.
Hypercritical Accretion onto a Newborn Neutron Star and Magnetic Field Submergence  [PDF]
Cristian G. Bernal,Dany Page,William H. Lee
Physics , 2012, DOI: 10.1088/0004-637X/770/2/106
Abstract: We present magnetohydrodynamic numerical simulations of the late post-supernova hypercritical accretion to understand its effect on the magnetic field of the new-born neutron star. We consider as an example the case of a magnetic field loop protruding from the star's surface. The accreting matter is assumed to be non magnetized and, due to the high accretion rate, matter pressure dominates over magnetic pressure. We find that an accretion envelope develops very rapidly and once it becomes convectively stable the magnetic field is easily buried and pushed into the newly forming neutron star crust. However, for low enough accretion rates the accretion envelope remains convective for an extended period of time and only partial submergence of the magnetic field occurs due to a residual field that is maintained at the interface between the forming crust and the convective envelope. In this latter case, the outcome should be a weakly magnetized neutron star with a likely complicated field geometry. In our simulations we find the transition from total to partial submergence to occur around dotM ~ 10 M_sun/yr. Back-diffusion of the submerged magnetic field toward the surface, and the resulting growth of the dipolar component, may result in a delayed switch-on of a pulsar on time-scales of centuries to millenia.
Black hole formation via hypercritical accretion during common envelope evolution  [PDF]
Philip J. Armitage,Mario Livio
Physics , 1999, DOI: 10.1086/308548
Abstract: Neutron stars inspiralling into a stellar envelope can accrete at rates vastly exceeding the Eddington limit if the flow develops pressures high enough to allow neutrinos to radiate the released gravitational energy. It has been suggested that this hypercritical mode of accretion leads inevitably to the formation of stellar mass black holes during common envelope evolution. We study the hydrodynamics of this flow at large radii (R >> R_ns), and show that for low Mach number flows, in two dimensions, modest density gradients in the stellar envelope suffice to produce a hot, advection dominated accretion disk around the accreting object. The formation of outflows from such a disk is highly probable, and we discuss the impact of the resultant mass loss and feedback of energy into the envelope for the survival of the neutron star. Unless outflows are weaker than those inferred for well observed accreting systems, we argue that in most cases insufficient accretion occurs to force collapse to a black hole before the envelope has been ejected. This conclusions is of interest for black hole formation in general, for some models of gamma ray bursts, and for predictions of the event rate in future LIGO observations.
Angular Momentum Role in the Hypercritical Accretion of Binary-Driven Hypernovae  [PDF]
L. Becerra,F. Cipolletta,C. L. Fryer,Jorge A. Rueda,R. Ruffini
Physics , 2015, DOI: 10.1088/0004-637X/812/2/100
Abstract: The induced gravitational collapse (IGC) paradigm explains a class of energetic, $E_{\rm iso}\gtrsim 10^{52}$~erg, long-duration gamma-ray bursts (GRBs) associated with Ic supernovae, recently named binary-driven hypernovae (BdHNe). The progenitor is a tight binary system formed of a carbon-oxygen (CO) core and a neutron star companion. The supernova ejecta of the exploding CO core triggers a hypercritical accretion process onto the neutron star, which reaches in a few seconds the critical mass, and gravitationally collapses to a black hole emitting a GRB. In our previous simulations of this process we adopted a spherically symmetric approximation to compute the features of the hypercritical accretion process. We here present the first estimates of the angular momentum transported by the supernova ejecta, $L_{\rm acc}$, and perform numerical simulations of the angular momentum transfer to the neutron star during the hyperaccretion process in full general relativity. We show that the neutron star: i) reaches in a few seconds either mass-shedding limit or the secular axisymmetric instability depending on its initial mass; ii) reaches a maximum dimensionless angular momentum value, $[c J/(G M^2)]_{\rm max}\approx 0.7$; iii) can support less angular momentum than the one transported by supernova ejecta, $L_{\rm acc} > J_{\rm NS,max}$, hence there is an angular momentum excess which necessarily leads to jetted emission.
Characterizing the time variability in magnetized neutrino--cooled accretion disks: signatures of the gamma-ray burst central engine  [PDF]
Augusto Carballido,William H. Lee
Physics , 2010, DOI: 10.1088/2041-8205/727/2/L41
Abstract: The central engine of Gamma Ray Bursts is hidden from direct probing with photons mainly due to the high densities involved. Inferences on their properties are thus made from their cosmological setting, energetics, low-energy counterparts and variability. If GRBs are powered by hypercritical accretion onto compact objects, on small spatial scales the flow will exhibit fluctuations, which could in principle be reflected in the power output of the central engine and ultimately in the high energy prompt emission. Here we address this issue by characterizing the variability in neutrino cooled accretion flows through local shearing box simulations with magnetic fields, and then convolving them on a global scale with large scale dynamical simulations of accretion disks. The resulting signature is characteristic, and sensitive to the details of the cooling mechanism, providing in principle a discriminant for GRB central engine properties.
Time-dependent Hypercritical Accretion onto Black Holes  [PDF]
Luca Zampieri
Physics , 1996,
Abstract: Results are presented from a time-dependent, numerical investigation of super-Eddington spherical accretion onto black holes with different initial conditions. We have studied the stability of stationary solutions, the non-linear evolution of shocked models and the time-dependent accretion from an expanding medium.
The need for hypercritical accretion in massive black-hole binaries with large Kerr parameters  [PDF]
Enrique Moreno Mendez
Physics , 2010, DOI: 10.1111/j.1365-2966.2010.18121.x
Abstract: Recent measurements of the Kerr parameters of the black holes in M33 X-7 and LMC X-1 yield a*=0.84\pm0.05 and a*=0.90^{+.04}_{-.09} respectively. We study massive binary evolution scenarios that can reproduce such high values for the Kerr parameters. We first discuss a model with Case C mass transfer leading to a common envelope and tidal synchronization of the primary before it collapses into a black hole. We also study a Case M evolution model (which involves tidally-locked, rotationally-mixed, chemically-homogeneous stars in a close binary). Our analysis suggests that, regardless of the specific scenario, the observed Kerr parameters for the black holes in M33 X-7 and LMC X-1 had to be obtained through hypercritical mass accretion.
Vacuum Breakdown near a Black Hole Charged by Hypercritical Accretion  [PDF]
A. Treves,R. Turolla
Physics , 1998, DOI: 10.1086/307159
Abstract: We consider a black hole accreting spherically from the surrounding medium. If accretion produces a luminosity close to the Eddington limit the hole acquires a net charge so that electrons and ions can fall with the same velocity. The condition for the electrostatic field to be large enough to break the vacuum near the hole horizon translates into an upper limit for the hole mass, $M\sim 6.6\times 10^{20} {\rm g}.$ The astrophysical conditions under which this phaenomenon can take place are rather extreme, but in principle they could be met by a mini black hole residing at the center of a star.
Hypercritical accretion onto a magnetized neutron star surface: a numerical approach
Bernal, C. G.;Lee, W. H.;Page, Dany;
Revista mexicana de astronomía y astrofísica , 2010,
Abstract: the properties of a new-born neutron star, produced in a core-collapse supernova, can be strongly affected by the possible late fallback which occurs several hours after the explosion. this accretion occurs in the regime dominated by neutrino cooling, explored initially in this context by chevalier (1989). here we revisit this approach in a 1d spherically symmetric model and carry out numerical simulations in 2d in an accretion column onto a neutron star, considering detailed microphysics, neutrino cooling and the presence of magnetic fields in ideal mhd. we compare our numerical results with the analytic solutions and explore how the purely hydrodynamical as well as the mhd solutions differ from them, and begin to explore how this may affect the appearance of the remnant as a typical radio pulsar.
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