PULSAR RECOIL BY LARGE-SCALE ANISOTROPIES IN SUPERNOVAE L. SCHECK H.-TH. JANKA, E. MÜLLER, K. KIFONIDIS, T. PLEWA
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1 PULSAR RECOIL BY LARGE-SCALE ANISOTROPIES IN SUPERNOVAE L. SCHECK H.-TH. JANKA, E. MÜLLER, K. KIFONIDIS, T. PLEWA MAX-PLANCK-INSTITUTE FOR ASTROPHYSICS, GARCHING
2 OUTLINE INTRODUCTION Observations Anisotropy Kick Mechanisms 2D SIMULATIONS Motivation Computational Setup Evolutionary phases Influence of initial conditions Influence of boundary conditions Neutron star velocities 3D SIMULATIONS Motivation First results CONCLUSIONS
3 OBSERVATIONAL EVIDENCE FOR ANISOTROPY SN1987A: non-spherical ejecta (Wang et al. 2002) Spectropolarimetry of various core collapse SN: Several % polarization => highly non-spherical ejecta Polarization increases with time, as we are looking deeper into SN (Wang et al. 2001, 2003)
4 PULSAR VELOCITIES: OBSERVATIONS mean velocities: km/sec (Lyne & Lorimer 1994) some move with more than 1000 km/s (Arzoumanian et al. 2002) Pulsars in globular clusters: small velocities Possibly bimodal distribution (Fryer et al. 1998, Arzoumanian et al. 2002) binary disruption can explain only 150 km/s...
5 PULSAR VELOCITIES: MECHANISMS anisotropic neutrino emission 3% anisotropy -> 1000 km/s required: ultrastrong magnetic fields (1016G) or speculative assumptions about neutrinos (Lai et al. 2001,Nardi & Zuluaga 2001) progenitor inhomogeneities anisotropic explosion observational evidence (SN1987A, polarization) inhom. grow during collapse, effect is controversial (Burrows & Hayes 1996, Fryer 2004) hydrodyn. instabilities can lead to large-scale anisotropies, which can produce high ns velocities (Herant 1995)
6 LARGE-SCALE ANISOTROPIES Herant (1995): l=1 situation can remain stable and lead to high pulsar velocities Chandrasekhar (1961): l=1 most unstable mode in heated fluid sphere Thompson (2000): spherical shock over hydrostatic atmosphere will develop global Rayleigh-Taylor mode, if density is sufficiently small Foglizzo (2002): 'vortical-acoustic cycle': Perturbations are generated at shock, advected downwards, generate acoustic waves near neutron star, which propagate upwards and perturb shock. Demonstrated by Blondin, Mezzacappa & DeMarino (2003), but not in a realistic SN-simulation.
7 PREVIOUS SIMULATIONS Maximum kick velocities: km/sec (e.g. Janka & Müller 1996, Burrows et al. 1995) no large-scale anisotropies (typ. angular scales <30 ) Idea: slow down onset of explosion, so that global modes have sufficient time to develop
8 SIMULATIONS: OUR APPROACH We want to simulate supernovae with slower onset of the explosion than in previous simulations We want to vary explosion energy and progenitor stars and see how this affects merging of modes and acceleration of the neutron star parameter study: We need many simulations We have to cover long timespan (1s) fast code: use simplified transport method Parametrization: replace ns interior by boundary (additional advantage: avoids problems due to incomplete knowledge of nuclear physics and neutrino interactions in dense ns interior)
9 BOUNDARY CONDITIONS inner core (1.1 MSUN) replaced by boundary condition We have to set: This determines explosion energy and timescale Choose slowly varying boundary luminosity simple: L(rib,t) = const (former simulations: exp(-t/t0)) Grid moves radially to mimic ns contraction radius of inner boundary neutrino luminosity neutrino number flux rib(t) L(rib,t) Ln(rib,t)
10 COMPUTATIONAL SETUP 2D simulations: assume axis-symmetry spherical grid, 180 angular zones, 400 radial zones hydrodynamics: Prometheus (PPM) start with post-bounce model + 0.1% perturbations rib= km rob=17000km
11 NEUTRINO TRANSPORT 1D, but independently for each angular bin Boltzmann equation + simplifying assumptions: Integration on characteristics detailed transport simulations: fit function for ceff Fermi-Dirac spectra, spectrally averaged neutrino interaction rates 100 times faster than solving boltzmann equation qualitatively similar results
12 EVOLUTIONARY PHASES I after bounce: stalled shock at about 200km negative entropy gradient leads to convection hotb bubbles grow, deform and push out shock convective structures start to merge (10-20ms) (30-100ms)
13 EVOLUTIONARY PHASES I after bounce: stalled shock at about 200km negative entropy gradient leads to convection hotb bubbles grow, deform and push out shock convective structures start to merge (10-20ms) (30-100ms)
14 EVOLUTIONARY PHASES II explosion starts, shock accelerates rapidly ( ms) in most cases only one downflow remains neutrino-driven wind forms neutron star for higher explosion energies, downflow is blown away (t<1s) (>400ms)
15 EVOLUTIONARY PHASES II explosion starts, shock accelerates rapidly ( ms) in most cases only one downflow remains neutrino-driven wind forms neutron star for higher explosion energies, downflow is blown away (t<1s) (>400ms)
16 2D MOVIES Eexp = 0.4 foe Eexp = 1.2 foe
17 PROGENITORS different progenitor stars (15 solar masses): WPE15 (Woosley, Pinto, Ensman, 1988) LSC15 (Limongi, Straniero, Chieffi, 2000) S15b7s2 [+rotation] (Woosley, Weaver, 1995) high accretion rate delayes explosion, more massive ns steep entropy gradient: faster onset of convection all progenitors produce highly anisotropic explosions
18 ROTATION Rotating version of s15s7b2 model (Buras et al. 2003): Piron core=12s, PPNS=10..20ms (similar to Heger et al. 2003) convection is affected by centrifugal forces (Hoiland) downflows form at both poles (l=2) highly anisotropic evolution is possible on avg. somewhat more isotropic than nonrot. models
19 INITIAL PERTURBATIONS morphology depends strongly on initial perturbations influence of boundary conditions is weaker (Mns vns) / (Mej < vej >)
20 NEUTRON STAR VELOCITY axis-symmetry: motion only along axis direction in most of our simulations: neutron star can not move at all! indirectly: momentum balance vnsmns = PNS = -PGAS high velocities! vrecord HOLDER = 800 km/s after 1s and still high accelerations: arecord HOLDER(1sec) = 550 km/s2
21 ACCELERATION MECHANISM direction: towards downflow, away from ejecta dominating force: gravitational pull of anisotropic ejecta additional, weaker forces, when downflow is still present: downflow, wind, neutrinos important as prediction for observations!
22 ACCELERATION MECHANISM direction: towards downflow, away from ejecta dominating force: gravitational pull of anisotropic ejecta additional, weaker forces, when downflow is still present: downflow, wind, neutrinos important as prediction for observations!
23 ACCELERATION MECHANISM direction: towards downflow, away from ejecta dominating force: gravitational pull of anisotropic ejecta additional, weaker forces, when downflow is still present: downflow, wind, neutrinos important as prediction for observations!
24 ACCELERATION COMPONENTS gravity dominates momentum transfer due to downflows also important recoil caused by outflows is weaker neutrinos: <5% in most cases (estimate)
25 ACCELERATION COMPONENTS gravity dominates momentum transfer due to downflows also important recoil caused by outflows is weaker neutrinos: <5% in most cases (estimate)
26 NS VELOCITY DISTRIBUTION high velocities possible for all explosion energies high variation of velocities for fixed energy still high accelerations after one second
27 NS VELOCITY DISTRIBUTION weak variation of vnsmax with explosion energy: vns = Pej / Mns
28 2D vs. 3D 2D limitations: downflow at equator or moving over equator => small acceleration in 2D is merging of modes in 3D as efficient as in 2D?
29 3D SIMULATIONS 400 x 45 x 120 zones 3 angular resolution 150 ms cut out 15 cones at poles to avoid numerical problems l=1 mode develops! next simulation is on the way...
30 3D SIMULATIONS 400 x 45 x 120 zones 3 angular resolution 300 ms cut out 15 cones at poles to avoid numerical problems l=1 mode develops! next simulation is on the way...
31 3D SIMULATIONS 400 x 45 x 120 zones 3 angular resolution 1000 ms cut out 15 cones at poles to avoid numerical problems l=1 mode develops! next simulation is on the way...
32 3D MOVIES 0-0.4s 0.9s s 0.5-1s
33 CONCLUSIONS We have performed a large sample of 2D supernova simulations for different 15M progenitor stars (including a rotating one). The simulations cover the first second after bounce. For slow a onset of the explosion, hydrodynamical instabilities can evolve to global modes, simultanously leading to anisotropic explosions and high pulsar velocities. We found neutron star velocities of up to 800km/s and still high accelerations after one second. The main acceleration mechanism is the gravitational pull due to the anisotropic ejecta distribution. The neutron star velocity is antiparallel to the explosion direction. First 3D results are promising...
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