asymmetric supernovae explosions: theory and...
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Asymmetric supernovae explosions: theory and experiment
Thierry Foglizzo CEA Saclay
X
Grefenstette+14
blue: Titanium green: Silicon red: Iron
Wongwathanarat+13
R. Hosseini-Kazeroni, B. Krueger, M. Gonzalez, F. Masset, A. Châtain, C. Royer, D. Martin, A. Kuntz
Some observational hints about the asymmetric character of ordinary supernovae
Hobbs+05
Cordes+93
Grefenstette+14
-distribution of pulsar kicks (Hobbs+05) -kick-spin angle distribution ? (Wang, Lai & Han 06, Ng & Romani 04) -polarization in the core (Leonard+06)
-nucleosynthesis inhomogeneities (Grefenstette+14)
Theoretical framework (Bethe & Wilson 85) neutrino-driven delayed explosion
electron capture p+ + e� ! n+ ⌫
modest energy in differential rotation:
GM2
ns
Rns
⇠ 2⇥ 1053erg
✓30km
Rns
◆✓M
ns
1.5Msol
◆2
Edi↵
< Erot
⇠ 2.4⇥ 1050erg
✓M
ns
1.5Msol
◆✓R
ns
10km
◆2
✓10ms
Pns
◆2
Why does the star explode ? How does the collapse turn into an explosion ?
A challenging numerical modeling: Garching, Oak Ridge, Princeton, Tokyo
Los Alamos, Basel, Chicago, CalTech, Monash
neutrino transport & interactions 3D hydrodynamics nuclear EOS general relativity
neutrinosphere shock
~150km
Fe
p+, n, e-
€
p+ + e− → n + ν e
€
n + ν e → p+ + e−
νe
2 instabilities during the phase of stalled accretion shock
Neutrino-driven convection (Herant, Benz & Colgate 92, ...)
- entropy gradient, fed by neutrino absorption - inhibited if the advection time is too short (Foglizzo et al. ’06)
SASI: Standing Accretion Shock Instability
(Blondin et al. 03 ...) - advective-acoustic cycle - large angular scale l=1,2: pulsar kick, nucleosynthesis, gravitational waves & neutrino signatures
neutrinosphere shock
~150km
Fe p+, n, e-
€
p+ + e− → n + ν e€
n + ν e → p+ + e−
νe
� ⌘Z gain
sh!BV
dr
vr< 3
Stationary Accretion Shock Instability : SASI
Blondin+03
Mechanism of SASI: advective-acoustic cycle
(Foglizzo 02, Ohnishi+06, Foglizzo+07, Scheck+08, Fernandez & Thompson 09, Guilet & Foglizzo 12)
shock ~150km
neutrinosphere €
p+ + e− → n + ν e
νe
H
He
Linear coupling between the acoustic wave and the entropy/vorticity wave
(Sato, Foglizzo & Fromang 09)
H
He
Linear coupling between the acoustic wave and the entropy/vorticity wave
(Sato, Foglizzo & Fromang 09)
8.1, 9.6 ,11.2, 15, 27Msol (Marek & Janka 08, Müller+12a,b,+13) 12, 15, 20, 25 Msol (Bruenn+13)
-depending on the progenitor, the dynamical evolution can be dominated by
-neutrino driven buoyancy (11.2Msol)
-or SASI (27Msol)
-or both (15Msol) -competition between the advection and buoyancy timescales (Foglizzo+06, Fernandez+13)
Since 2008: 2D explosions from first principles + understandable diversity
-weakish explosion energy < 1051 erg -insufficient convergence between the numerical models -no explosion in 3D yet
� ⌘Z gain
sh!BV
dr
vr< 3
The challenge of 3D modelling: SASI spiral mode, 27Msol (Hanke ‘13) no explosion ?
PRACE 150 million hours
16.000 processors 4.5 months/model
time evolution: 500ms diameter: 300km
From a shallow water experiment to supernova theory
- explosion energy, neutrino signal, grav. waves, nucleosynthesis, - Pulsar kick and spin
Complex comprehensive simulations
SWASI experiment Build intuition Fast exploration of the parameter space: accretion rate, Mach number, shock radius, angular momentum
Predictions of SN and pulsars
properties
progenitor structure + nuclear EOS + neutrino transport & interactions + GR + multi-D hydro
Multi-D hydro 3D stationary accretion, neutrino heating, SASI+convection
- 2D shallow water with viscous drag, then inviscid
© MPA/Janka
- 2D cylindrical SASI ideal gas neutrino cooling
© Blondin & Mezzacappa
© Hosseini Kazeroni
© Masset, Gonzalez
© Grefenstette
Dynamics of water in the fountain
diameter 40cm
3s/oscillation
Dynamics of the gas in the supernova core
diameter 400km 0.03s/oscillation
1 000 000 x bigger 100 x faster
SWASI Shallow Water Analogue of a Shock Instability
acoustic waves shock wave pressure
surface waves hydraulic jump depth
Formal similarity between SASI and SWASI
accretion of gas (on a cylinder) density , velocity , sound speed
inviscid shallow water accretion depth , velocity , wave speed
- Inviscid shallow water: analogue to an isentropic gas γ=2 ( intermediate between "isothermal" and "γ=2 without entropy" )
isothermal
adiabatic
expected scaling
shock radius 200 km → 20 cm oscillation period 30 ms → 3 s
Blondin & Mezzacappa 07
3D spherical γ=4/3
2D cylindrical γ=2 isentropic
a shallow water experiment with a circular hydraulic jump
Comparison to the 2D shallow water model
No free parameter: - laminar viscous drag measured in the stationary flow - inner boundary: free spillover
Foglizzo, Masset, Guilet, Durand PRL (2012)
SWASI: simple as a garden experiment
May 2010
June 2010
October 2010
November 2010 November 2013
The “supernova fountain” at the Palais de la Découverte, Paris 17 decembre 2013-16 february 2014
S N 2 N S !Supernovae explosions, from stellar core-collapse
to neutron stars and black holes
12 researchers 138 presentations
2059 visitors
Thierry Foglizzo Julien Faure
Rémi Hosseini-Kazeroni Noël Martin
Jérôme Novak Micaela Oertel Patrick Blottiau
Elias Khan Jérôme Guilet Bruno Peres
Michael Urban Jérôme Margueron
-injection radius: 33cm -NS radius: 4-8 cm -flow rate: Q = 0-4L/s -injection slit: h = 0.5-2mm -rotation period: 10-500s
Froude number Reynolds number
Re = 650
✓h
1mm
◆ 32✓Fr
4
◆✓20cm
r
◆
Fr = 4.9
✓Q
L/s
◆✓h
mm
◆� 32
April 2014
A new prototype built at CEA in 2014
Rotating progenitor: accreted angular momentum changes its sign as SASI grows
fountain rotation period: 246s injection slit: 0.55mm flow rate: 1.17L/s
Blondin & Mezzacappa 07
The consequences of SASI on the birth conditions of neutron stars!
- pulsar kicks (Scheck+04, 06, Nordhaus+10, 11,
Wongwathanarat+10, 13) - pulsar spin ? (Blondin & Mezzacappa 07, Yamasaki & Foglizzo 08, Iwakami+09, Rantsiou+11 Guilet & Fernandez 14)
Hobbs et al. 05
Unexpected robust spiral shock driven at the corotation radius when the inner rotation rate reaches 20% Kepler
analogue to the instability of a neutron star rotating differentially (Shibata+02,03, Saijo+03,06, Watts+05, Corvino+10)
flow rate: 0.3L/s, slit size: 1.6mm
instability mechanism dominated by the corotation trapping of acoustic waves (Papaloizou & Pringle 84, Goldreich & Narayan 85)
Saijo & Yoshida 2006
velocity
density
Increasing the rotation rate above the centrifugal limit (TK=15s):
shallow water analogue of the m=1 instability of a centrifugal shock
fountain rotation period: 12.7s (i.e. 0.84 TK) injection slit: 0.9mm flow rate: 0.7L/s
Instability of a centrifugal shock
Instability mechanism: corotation trapping of acoustic waves (Papaloizou & Pringle 1984, Goldreich & Narayan 1985)
Molteni et al. 1999
density
toward larger scales
educative experiment
outdoor fountain ?
aquatic parc ??
Conclusions
Hydrodynamical instabilities are a key ingredient to supernova theory - enable the explosion by locally increasing neutrino capture - pulsar kick up to 1000km/s - pulsar spin up to 10 Hz
SWASI: first experimental view on core collapse supernovae - complementary to perturbative tools and numerical modeling - makes asymmetric explosions more intuitive and attractive to students
First results from the new prototypes - Palais de la Découverte, Paris at Fall 2014 - increasing the rotation rate:
T>150s: spiral SASI with a counter-spinning neutron star T~30-60s: neutron star destabilized by differential rotation
Towards a better modeling of the experiment: - interplay of SWASI and turbulence ? - experiment scaling to a larger size ?
Guitar Nebula: 1.4Msol@1600km/s Cordes et al. ‘93