Neutrino-Driven Jets in Compact Object Mergers Oliver Just - PowerPoint PPT Presentation

Neutrino-Driven Jets in Compact Object Mergers Oliver Just Max-Planck-Institut für Astrophysik, Garching MICRA Workshop Stockholm, August 18 th 2015 With: H.-Th. Janka, N. Schwarz, A. Bauswein, M. Obergaulinger

Mo t i v a t i o n ➔ central engine and launch mechanism of short GRBs not safely identified yet ➔ two most likely systems: BH-tori and (H)MNS ➔ two most likely mechanisms: neutrino-annihilation and (several) magneto-rotational processes ➔ most previous studies compute annihilation rate using 1D models (Popham, DiMatteo, Liu, ...) or by post-processing individual snapshots (Ruffert, Dessart, Richers, …) ➔ other studies evolve jets without resolving the central engine (Aloy, Nagataki, Duffel, Murguia-Berthier, …) ➔ 2 necessary conditions to obtain about ~10 48 – 10 50 erg in relativistic outflow material: sufficient energy provided by nu-annihilation • sufficiently small energy loss during expansion • ➔ What is the impact of the dynamical ejecta on the jet? MICRA Workshop Stockholm August 18th, 2015

“ A L C A R ” N e u t r i n o T r a n s p o r t C o d e (OJ, Obergaulinger, Janka '15, ArXiv:1501.02999) Radiation-hydro with Boltzmann solver too expensive! Our approach (see also: O'Connor '14, Kuroda '15) : ➔ Two-moment scheme with algebraic Eddington factor ( AEF or M1 scheme ) ← e n e r g y d e n s i t y ← mo me n t u m d e n s i t y ← p r e s s u r e e v o l u t i o n e q u a t i o n s a p p r o x i ma t e a l g e b r a i c c l o s u r e r e l a t i o n s ( e . g . " M1 c l o s u r e " ) Effective save up of the two angular degrees of freedom! MICRA Workshop Stockholm August 18th, 2015

S e t u p o f B H - T o r u s Mo d e l s ( fj r s t w i t h o u t d y n a mi c a l e j e c t a ) ➔ initial configuration given by equilibrium tori with constant specific angular moment ➔ simulations performed in 2D axisymmetry ➔ multi-group neutrino transport with 10 energy groups ➔ most dominant (electron) neutrino interactions included: ✔ emission/absorption by nucleons ✔ neutrino-nucleon scattering ✔ neutrino-antineutrino annihilation ➔ Newtonian hydrodynamics with pseudo-Newtonian gravitational potential by Artemova → mimics the ISCO and BH spin ➔ angular momentum transport: Shakura & Sunyaev α-viscosity ➔ variation of mtorus, MBH, ABH, αvis ➔ similar models as used for nucleosynthesis study Just et al. '15 MNRAS 448, 541 and conceptually similar as in Fernandez '13, '14 MICRA Workshop Stockholm August 18th, 2015

Mo v i e : B H - t o r u s w i t h o u t p r o mp t e j e c t a MICRA Workshop Stockholm August 18th, 2015

N e u t r i n o e mi s s i o n p r o p e r t i e s v s . t o r u s ma s s MICRA Workshop Stockholm August 18th, 2015

N e u t r i n o e mi s s i o n p r o p e r t i e s v s . B H ma s s MICRA Workshop Stockholm August 18th, 2015

N e u t r i n o e mi s s i o n p r o p e r t i e s v s . B H s p i n MICRA Workshop Stockholm August 18th, 2015

N e u t r i n o e mi s s i o n p r o p e r t i e s v s . v i s c . p a r a me t e r MICRA Workshop Stockholm August 18th, 2015

R e l a t i v i s t i c e j e c t a e x p a n s i o n i n t o d y n a mi c a l e j e c t a ➔ we now extend Newtonian to special relativistic hydro ➔ data for dynamical ejecta mapped from SPH simulations onto 2D BH-torus grid ➔ extend EOS to low densities, include electron recombination, radioactive heating (Bauswein et. al. '13) MICRA Workshop Stockholm August 18th, 2015

Mo d e l T M1 1 4 5 1 : N S - B H r e mn a n t ➔ MOVIE ➔ dynamical ejecta are ignored since they are almost exclusively ejected in equatorial plane ➔ thermal fireball is successfully launched ➔ annihilation energy is efficiently converted to relativistic kinetic energy ➔ jet can expand almost unimpeded ➔ amount of energy sufficient at least to explain low-luminosity sGRBs MICRA Workshop Stockholm August 18th, 2015

Mo d e l T M1 1 3 5 2 0 : N S - N S r e mn a n t ➔ MOVIE ➔ dynamical ejecta are slightly equatorially dominated → favorable for jet launch ➔ jet is successfully launched, but only after significant energy input by annihilation ➔ in the jet beam , annihilation energy is efficiently converted to relativistic kinetic energy ➔ however, during expansion the jet beam dissipates almost all kinetic energy due to interaction with the cocoon and jet head ➔ amount of energy not sufficient to explain sGRBs MICRA Workshop Stockholm August 18th, 2015

Mo d e l S F H O 1 4 5 1 4 5 : N S - N S r e mn a n t ➔ MOVIE ➔ dynamical ejecta are almost spherical → not favorable for jet launch ➔ annihilation only deposits thermal energy into dynamical ejecta ➔ however, not powerful enough to launch a jet MICRA Workshop Stockholm August 18th, 2015

S u mma r y ➔ using the M1 code ALCAR we examined neutrino emission + annihilation in BH-torus systems as functions of mtorus, MBH, ABH, αvis ➔ typical annihilation energies are 10 47 – 10 49 erg and efficiencies are 10 -5 – 10 -4 , while high values favor high mtorus, low MBH, high ABH, high αvis ➔ for selected models we followed the relativistic jet expansion into the dynamical ejecta ➔ NS-BH mergers: major fraction of anni. energy may end up in relativistic ejecta → could explain at least low-luminosity sGRBs ➔ NS-NS mergers: either no jet is launched or the major fraction of anni. energy is dissipated in the dynamical ejecta → annihilation too weak ➔ for a delayed collapse in NS-NS mergers, the situation is likely even worse due to additional neutrino-driven winds ➔ results suggest that other mechanisms are needed to explain sGRBs in NS-NS mergers and high-energy sGRBs in NS-BH mergers! MICRA Workshop Stockholm August 18th, 2015

T h a n k y o u f o r y o u r a t t e n t i o n ! MICRA Workshop Stockholm August 18th, 2015

A p p e n d i x : T e s t o f N e u t r i n o S c h e me MICRA Workshop Stockholm August 18th, 2015

A p p e n d i x : J e t e x p a n s i o n i n e x t e r n a l me d i u m (Bromberg et. al. '11) MICRA Workshop Stockholm August 18th, 2015