the “bermuda triangle”ecsne and/or aic of one wds postulated to explain many observations,...
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THE “BERMUDA TRIANGLE”EVOLUTION AND FATE OF 8 – 12 SOLAR-MASS STARS
SAMUEL JONESHEIDELBERG INSTITUTE FOR THEORETICAL STUDIES
MON 14 MAR 2016
18th RINGBERG WORKSHOP
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● Statistical significance: ~50% of all massive stars (or more? See Jennings+ 2012)
● Mass range in which multiple stellar fates are realised: ONe WDs, ECSNe and CCSNe
WH
Y S
TU
DY
8-1
2 M
☉
STA
RS?
Jones+ 2013Woosley & Heger 2015
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ECSNe and/or AIC of ONe WDs postulated to explain many observations, including:
● Production of Ag and Pd (e.g. Hansen+ 2012)
● Site for r-process (e.g. Cescutti+ 2014, but also Wanajo+ 2011)
● “bimodal” NS mass distribution (e.g. Schwab+ 2010)
● Bimodal BeX orbital eccentricity (e.g. Knigge+ 2011)
● Low L transients (e.g. Thompson+ 2009)
ELECTRON-CAPTURESUPERNOVAE?
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Image Credit: NASA, ESA, J. Hester, A. Loll (ASU) Image credit: NASA/Andrew Fruchter (STScI)
WHAT HAPPENS TO 8-10SOLAR-MASS STARS?
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Image Credit: NASA, ESA, J. Hester, A. Loll (ASU)
WHAT ARE ELECTRON-CAPTURESUPERNOVAE?
Image credit: NASA/CXC/SAO
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SUPER-AGB STARSImage credit: Alexander Heger
Nuclear burning is curtailed due to combined effects of neutrino losses and degeneracy, leaving an ONe core
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Lugaro+ (2012)
SUPER-AGB STARTwo (three) general classical scenarios:
1. The H envelope is ejected, producing a planetary nebula and an ONe white dwarf
2. The core grows due to accumulation of ash from the burning shells, eventually exceeding the effective Chandrasekhar limit and collapsing to a neutron star
3. An ONe WD is formed, but later accretes from a binary companion and collapses to a neutron star
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At about 3e9 g/cc, 24Mg begins to capture electrons, inducing a contraction
But it is 20Ne + 2e-, activated at about 1010 g/cc that releases enough energy to ignite an oxygen deflagration wave in the centre
The energy release from burning competes with electron capture on the ash; in the classical picture the electron captures win and the star's core collapses
Miyaji+ (1980); Nomoto (1984,1987)
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OUTSTANDING PROBLEMS
● The mass loss rates and core growth rates for these stars are not well known (e.g. Poelarends+ 2008)
● Hydrodynamic instabilities triggered by iron opacities (e.g. Lau+ 2012) or energy deposition by H ingestion in to He-burning convection zones (Jones+ 2015) may lead to ejection of the envelope before the core reaches critical mass
● Sensitive to nuclear physics input and mixing processes; the deflagration ignition density is critical
● In 1D simulations of the O deflagration, neutron stars, WDs and thermonuclear SNe were all possible outcomes (Isern+ 1991, Canal+ 1992)
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OUTSTANDING PROBLEMS
● In 1D simulations of the O deflagration, neutron stars, WDs and thermonuclear SNe were all possible outcomes (Isern+ 1991, Canal+ 1992)
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O DEFLAGRATIONMULTI-DIMENSIONAL SIMULATIONSin collaboration with: F. Röpke, R. Pakmor, I. Seitenzahl, S. Ohlmann & P. Edelmann
LEAFS code (Reinecke+ 1999, Röpke & Hillebrandt 2005, Röpke 2005, 2006)
Isothermal ONe core/WD in HSE with central densities 109.9, 109.95, 1010.3 g / cc
Centrally-confined ignition: 300 'bubbles' within 50 km sphere, < 5 x 10-4 M☉ inside initial flame
Laminar flame speeds from Timmes+ (1992); turbulent from Schmidt+ (2006)
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NUCLEAR REACTIONSDELEPTONISATION OF NSE ASH
NKK: Nabi & Klapdor-Kleingrothaus
LMP: Langanke & Martinez-Pinedo (2001)
ODA: Oda+ (1994)
FFN: Fuller, Fowler & Newman (1985)
ANA: Analytical rates; Gamow-Teller strength B = 4.6 (Arcones+ 2010)
SJ, FKR, RP, IRS, STO, PVFE arXiv:1602.05771
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Scale: 1500 kmTime: 0.7 s
56NiO
DEF
LAG
RA
TIO
N3D
4π
: 512
3
THER
MO
NU
CLE
AR
EX
PLO
SIO
N?
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Scale: 2500 kmTime: 1.3 s
56NiO
DEF
LAG
RA
TIO
N3D
4π
: 512
3
THER
MO
NU
CLE
AR
EX
PLO
SIO
N?
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Scale: 400,000 kmTime: 60 sO
DEF
LAG
RA
TIO
N3D
4π
: 512
3
THER
MO
NU
CLE
AR
EX
PLO
SIO
N?
56Ni
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ρign = 109.9 g cm-3
THERMONUCLEAR EXPLOSION?
SJ, FKR, RP, IRS, STO, PVFE arXiv:1602.05771
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ρign = 1010.3 g cm-3
CORE COLLAPSE
SJ, FKR, RP, IRS, STO, PVFE arXiv:1602.05771
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DIAGNOSTICS
Bound ONeFe remnants
Remarkably similar result to Isern+ (1991)
Core collapse
SJ, FKR, RP, IRS, STO, PVFE arXiv:1602.05771
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M80: Miyaji+ (1980)
N87: Nomoto (1987)
M87: Miyaji & Nomoto (1987)
I91: Isern+ (1991)
C92: Canal+ (1992)
H93: Hashimoto+ (1993)
G96: Gutierrez+ (1996)
T13: Takahashi+ (2013)
S15: Schwab+ (2015)
IGNITION DENSITYSENSITIVITY TO MIXING PROCESSES
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SJ, RA, SS, AD, PW, FH (2016 in prep)
MIXING IN STARSIDEALISED 3D SIMULATIONS TO INFORM 1D MODELS
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SJ, RA, SS, AD, PW, FH (2016 in prep)
MIXING IN STARSIDEALISED 3D SIMULATIONS WITH PPMstar
In collaboration with: Paul Woodward, Falk Herwig, Stou Sandalski, Robert Andrassy, Austin Davis
7683 and 15363 simulations in 4π geometry
O shell burning in 25 solar-mass star at Zini=0.02
2 fluids (μconv = 1.848, μstab = 1.802)
Constant volume heating
Ideal gas EoS
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O-S
HEL
L B
UR
NIN
GSJ
, RA
, SS,
AD
, PW
, FH
(201
6 in
pre
p)
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O-S
HEL
L B
UR
NIN
GSJ
, RA
, SS,
AD
, PW
, FH
(201
6 in
pre
p)
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O-SHELL BURNING
SJ, RA, SS, AD, PW, FH (2016 in prep)
Entrainment rate = 1.33 x 10-6 M☉ s-1
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O-SHELL BURNING1D MIXING MODEL
SJ, RA, SS, AD, PW, FH (2016 in prep)
See also: talk by R. Hirschi
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SUMMARYECSNe and AIC of ONe Wds postulated to explain many astrophysical observations, including:● Abunudance anti-correlations● Site for r-process● “bimodal” NS mass distribution● Bimodal BeX orbital
eccentricity● Low L transientsIn recent 2-3 years we have improved:● Nuclear physics input● Progenitor models● Deflagration simulationsNext: pre-ignition mixing
Temporally and spatially averaged mixing properties of 3D hydrodynamic O-shell burning simulations can be well approximated in 1D codes when:● the local MLT mixing length is
limited to the distance to the convective boundary
● Exponential-diffusive CBM is employed, with an e-folding length of ~0.025HP