The Death of Massive Stars: Core-Collapse Supernovae and their - - PowerPoint PPT Presentation
The Death of Massive Stars: Core-Collapse Supernovae and their Signature in Gravitational Waves Christian David Ott cott@tapir.caltech.edu TAPIR , California Institute of Technology, Pasadena, CA, USA Niels Bohr International Academy, Niels
TAPIR, California Institute of Technology, Pasadena, CA, USA Niels Bohr International Academy, Niels Bohr Institute, Copenhagen, Denmark Center for Computation and Technology, Louisiana State University, Baton Rouge, LA, USA
cott@tapir.caltech.edu
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R 100 – 200 km
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R 100 – 200 km
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Neutrino Mechanism Magnetorotational Mechanism Acoustic Mechanism
[Colgate & White 1966, Arnett 1966, Wilson 1985, Bethe & Wilson 1985, recent: Buras et al. 2006, Kitaura et al. 2006, Marek & Janka 2009, Ott et al. 2008] [LeBlanc & Wilson ‘70, Bisnovatyi-Kogan et
recent: Burrows et al. 2007] [proposed by Burrows et al. 2006, 2007; not confirmed by other groups/codes]
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[Ott 2009, arXiv:0905.2797]
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Multi-D Dynamics
Turbulence
[Ott 2009, arXiv:0905.2797]
[Review: Ott, CQG 26, 063001 (2009)]
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from the supernova engine deep inside the star.
postshock region and in the protoneutron star (PNS).
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Shock Instability (SASI)
[Review: Ott, CQG 26, 063001 (2009)]
from the supernova engine deep inside the star.
postshock region and in the protoneutron star (PNS).
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[Review: Ott, CQG 26, 063001 (2009)]
Rotating Core Collapse and Bounce Convection & Standing Accretion Shock Instability Protoneutron Star Pulsations Nonaxisymmetric Rotational Instabilities Asymmetric Neutrino Emission Aspherical Outflows
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conservation leads to spin up & rotational deformation of inner core.
accelerations -> rapidly changing mass quadrupole moment.
GW emission in core collapse
Rotation + Gravity + Stiffening of EOS.
11 [Dimmelmeier, Ott, Marek, and Janka 2008, Ott 2009, Dimmelmeier et al. 2007ab, Ott et al. 2007]
with Ye(ρ). 6 pre-SN stellar models.
moderately differential rotation.
collapse multi-degenerate.
[Ott 2009]
WARNING: 99% of massive stars are probably slowly rotating!
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[Review: Ott, CQG 26, 063001 (2009)]
Rotating Core Collapse and Bounce Convection & Standing Accretion Shock Instability Protoneutron Star Pulsations Nonaxisymmetric Rotational Instabilities Asymmetric Neutrino Emission Aspherical Outflows
Azimuthalmodes exp(im). m=2 “bar-modes” (T/|W|)dynamical = 0.27, (T/|W|)secular 0.14.
Numbers hold roughly in GR and moderate differential rotation.
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[e.g., Chandrasekhar 1969] [Dimmelmeier et al. 2008, Ott et al. 2007, Ott et al. 2006] [e.g., Baiotti et al. 2007]
[Shibata et al. 2000, 3+1 GR NS simulations] [Ott et al. ‘07, 3+1 GR simulations]
Azimuthalmodes exp(im). m=2 “bar-modes” (T/|W|)dynamical = 0.27, (T/|W|)secular 0.14.
Numbers hold roughly in GR and moderate differential rotation.
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[e.g., Chandrasekhar 1969] [Dimmelmeier et al. 2008, Ott et al. 2007, Ott et al. 2006] [e.g., Baiotti et al. 2007]
rotational barrier.
dynamical) attainable during PNS cooling.
[Ott et al. PRL 2007 & CQG 2007, Dimmelmeier et al. 2008]
instability at low T/|W|.
m={2,3} modes mixed in
(radial & temporal variation).
Corotation instability
Resonance of unstable mode with background fluid at corotationpoint(s).
relationship to accretion and galactic disks?
15 [e.g., Centrella et al. 2001, Shibata et al. 2003, Saijo 2003, Saijo & Yoshida 2006, Ott et al. 2005, Ou & Tohline 2006]
[Ott et al. 2007, 3+1 GR simulation]
GW Emission, Model s20A2B4
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Polar Observer + Polar Observer x Equatorial Observer x Equatorial Observer +
Ott et al. 2007, PRL 3+1 GR simulation of Rotating Core Collapse
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[Ott 2009, arXiv:0905.2797]
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but greater in energy! Emission in narrow frequency band around 900—930 Hz (2 x pattern speed of the unstable mode!) models.
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[Review: Ott, CQG 26, 063001 (2009)]
Rotating Core Collapse and Bounce Convection & Standing Accretion Shock Instability Protoneutron Star Pulsations Nonaxisymmetric Rotational Instabilities Asymmetric Neutrino Emission Aspherical Outflows
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– Negative entropy gradient left by stalling shock drives prompt convection.
[e.g., Burrows & Hayes 1992]
– Growth and duration (5-50 ms) strongly dependent on seed perturbations.
– Negative lepton gradient drives PNS convection. [e.g., Dessart et al. 2005] – Physical scale: 10-50 km. Duration: 1 s.
[e.g., Herant et al. 1994, Burrows et al. 1995, Blondin et al. 2003, Buras et al. 2006, Burrows et al. 2006, Marek & Janka 2009]
– Neutrino heating -> negative entropy gradient behind shock. – Advective-acoustic cycle -> low-mode standing accretion shock instability. – Physical scale: 50-300 km. Duration: until explosion or BH formation.
[Burrows et al. 2006]
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stochastic nature (governed by turbulent flow/non-linear dynamics).
to small radii.
[Murphy, Ott & Burrows 2009 (in prep.); Marek et al. 2009, Müller et al. 2004, Kotakeet al. 2007, 2009]
simulations with the code Bethe-Hydro.
[Murphy & Burrows 2008]
parametrized neutrino luminosity and heating.
SN dynamics in nonrotating 12, 15, 20, and 40 MSUN stars.
[Woosley & Heger 2007]
[Murphy, Ott & Burrows 2009]
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[Murphy, Ott and Burrows 2009 (in prep.)]
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[Murphy, Ott & Burrows 2009 (in prep.)]
required and longer time to explosion -> stronger GW emission.
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[Review: Ott, CQG 26, 063001 (2009)]
Rotating Core Collapse and Bounce Convection & Standing Accretion Shock Instability Protoneutron Star Pulsations Nonaxisymmetric Rotational Instabilities Asymmetric Neutrino Emission Aspherical Outflows
2009/07/02
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turbulence excite lowest-order (l=1) g-mode in the PNS. f 300 Hz.
[Burrows, Livne, Dessart, Ott, Murphy 2006, 2007b/c, Ott et al. 2006]
500 ms —1 s after bounce.
that steepen into shocks; deposit energy in the stalled shock.
(2) possible parametric instability, limiting mode amplitudes. [Weinberg & Quatert’08]
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s25.0 from Burrows et al. 2007 Core Bounce Convection & SASI early g-modes late-time PNS g-modes
prompt convection.
and -driven.
l=2 components emit GWs.
saturate at low level.
[Weinberg & Quatert 2008]
[Ott 2009, Ott et al. 2006]
(s)
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[Ott 2009, Ott et al. 2006, Burrows et al. 2007]
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[Review: Ott, CQG 26, 063001 (2009)]
Rotating Core Collapse and Bounce Convection & Standing Accretion Shock Instability Protoneutron Star Pulsations Nonaxisymmetric Rotational Instabilities Asymmetric Neutrino Emission Aspherical Outflows
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[Epstein 1978, Burrows & Hayes 1996, Janka & Müller 1997, Müller et al. 2004, Ott 2009, Kotake et al. 2007, 2009]
will emit GWs. Asymmetric neutrino radiation:
[Ott et al. 2008]
GW “Memory”
[Dessart et al. 2006, Ott 2009 Accretion-Induced Collapse
Large h, low frequency
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[Review: Ott, CQG 26, 063001 (2009)]
Rotating Core Collapse and Bounce Convection & Standing Accretion Shock Instability Protoneutron Star Pulsations Nonaxisymmetric Rotational Instabilities Asymmetric Neutrino Emission Aspherical Outflows
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[Burrows & Hayes 1996, Fryer et al. 2004; in the MHD context: Kotake et al. 2004, Obergaulinger et al. 2005, 2006]
be large, leading to density perturbations O(10%). [Bazan & Arnett ‘97, Meakin et al. ‘06].
GW burst (with memory!) from mass motions and neutrinos.
need large parameter study.
[Burrows & Hayes 1996]
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Neutrino Mechanism Magnetorotational Mechanism Acoustic Mechanism
[Ott 2009, arXiv:0905.2797 and CQG Topical Review, Ott 2009]
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Neutrino Mechanism Magnetorotational Mechanism Acoustic Mechanism
Dominant Multi-D Dynamics and GW Emission Process(es)
Convection and SASI.
[Ott 2009, arXiv:0905.2797 and CQG Topical Review, Ott 2009]
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Neutrino Mechanism Magnetorotational Mechanism Acoustic Mechanism
Convection and SASI. Rotating core collapse & bounce, PNS rotational instabilities.
[Ott 2009, arXiv:0905.2797 and CQG Topical Review, Ott 2009]
Dominant Multi-D Dynamics and GW Emission Process(es)
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Neutrino Mechanism Magnetorotational Mechanism Acoustic Mechanism
Convection and SASI. Rotating core collapse & bounce, PNS rotational instabilities. PNS pulsations.
[Ott 2009, arXiv:0905.2797 and CQG Topical Review, Ott 2009]
Dominant Multi-D Dynamics and GW Emission Process(es)
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Neutrino Mechanism Magnetorotational Mechanism Acoustic Mechanism
Convection and SASI. Rotating core collapse & bounce, PNS rotational instabilities. PNS pulsations.
[Ott 2009, arXiv:0905.2797 and CQG Topical Review, Ott 2009]
Dominant Multi-D Dynamics and GW Emission Process(es)
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– Milky Way, Andromeda (M31), Triangulum (M33) + 30 small galaxies/satellite galaxies (incl. SMC & LMC).
Compiled from long list of references, e.g. Cappellaro et al., den Bergh & Tammann.
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Core-collapse SNe within 5 Mpc since the beginning of LIGO operations:
M82 Chandra/HST/Spitzer composite. M31 (Andromeda) Spitzer.
Ando et al. 2005
[Ott 2009]
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– Neutrino mechanism – Magnetorotational mechanism – Acoustic Mechanism
appears mutually exclusive.
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emission mechanisms need more/better modeling.
mode unlikely to see strongest bursts beyond local group!
for detection, 100 for doing real (nuclear/astro)physics.
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[Murphy, Ott & Burrows 2009 (in prep.)]
[Meakin & Arnett 2007]
emission comes from SASI downflow plume that is decelerated at the PNS surface.
behavior in linear limit.
SASI plume Brunt-Väisälä: N2 > 0: stable, N2 < 0: unstable Overshooting
Boundary to stable layer
Buoyancy acceleration
integration of buoyancy acceleration and analytic model for turning point:
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[Murphy, Ott & Burrows 2009 (in prep.)]
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[Ott 2009, see also Marek et al. 2009]
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multi-D nature.
– Nature: AIC, O/Ne, or Iron core. – Structure, rotational configuration. – Precollapse asphericities.
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[Burrows et al. 2006, 2007b/c, Ott et al. 2006]
Azimuthalmodes exp(im). m=2 “bar-modes” (T/|W|)dynamical = 0.27, (T/|W|)secular 0.14.
and moderate differential rotation.
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[Dimmelmeier et al. 2008, Ott et al. 2007, Ott et al. 2006] [e.g., Baiotti et al. 2007]
[Ott et al. 2009 in prep.]
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Core collapse between 02/15 and 03/05.
LIGO H2 and GEO600 in Astrowatch mode.
a core-collapse SN at 4 Mpc.
Thanks: Erik Katsavounidis& Michael Landry
[Ott 2008]
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[Ott 2009, Marek et al. 2009, Kotake et al. 2007, 2009, Ott et al. 2006, Müller et al. 2004, Janka & Müller 1997]
[Ott 2009]
(Brunt-VäisälaFrequency)
Based on subtle imbalance between neutrino heating and cooling in the postshock region.
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[Thompson et al. 2003, Rampp & Janka 2002, Liebendörfer et al. 2002,2005]
Problem: Fails to explode massive stars in spherical symmetry.
[Wilson 1985, Bethe & Wilson 1985; recent reviews: Kotakeet al. 2006, Janka et al. 2007]
Breaking of spherical symmetry is a key ingredient of the supernova mechanism!
[Ott 2009]
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[e.g., Burrows et al. 2007, Dessart et al. 2008, Shibata et al. 2006, Kotake et al. 2004, Yamada & Sawai 2004,]
VULCAN 2D R-MHD code, Livne et al. 2007, Burrows et al. 2007.
P0 < 4-6 s
10 B = 1052 erg
fields up to equipartition:
instability (MRI)
may be GRB precursor.
56 Betelgeuse as seen by the HST, Distance: 200 pc Betelgeuse as seen by the HST, Distance: 200 pc
MZAMS ≥ 8—10 MSUN
Photo-dissociation and e- capture
MZAMS ≥ 8—10 MSUN
Photo-dissociation and e- capture
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Inner core bounce,
neutrinos and dissociation: Shock stalls.
EGrav= 300 [B]ethe (3 x 1053 erg) EExplosion = 1 B ENeutrinos = 99% EGrav≈ 15% MSUNc2
SN Energetics
58 3D GR simulation Ott 2006, rendition by R. Kähler, Zuse Institute, Berlin
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Protoneutron star (PNS) core pulsations, Burrows et al. 2006, 2007; Ott et al. 2006
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[e.g., Blondin et al. 2003,2006; Foglizzo et al. 2006, Scheck et al. 2006, 2007, Burrows et al. 2006, 2007 ] Advective-acoustic cycle drives shock instability. Seen in simulations by all groups!
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few x 1053 erg (100 B)
1 B
0.3 – 1.5 s after bounce.
PNS mass 1.8 – 2.5 MSUN.
No direct BH formation in pop I/II stars!
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– Milky Way, Andromeda (M31), Triangulum (M33) + 30 small galaxies/satellite galaxies (incl. SMC & LMC).
Compiled from long list of references, e.g. Cappellaro et al., den Bergh & Tammann.
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[Dimmelmeier et al. 2008, Dimmelmeier et al. 2007, Ottet al. 2007, Ott 2006]
hot microphysical EOS & deleptonization during collapse.
inner core mass, inner core angular momentum, and (to some extent) nuclear EOS.
no “multiple centrifugal bounce”.
cores (precollapse P0 < 8 s) “detectable” throughout the Milky Way.
Cores stay axisymmetric through bounce and early postbounce phase.