Exclusive Diffraction at HERA Henri Kowalski DESY Ringberg October 2005
How Turbulence Enables the Explosion of Core-Collapse ... · Quintin Mabanta & Jeremiah Murphy...
Transcript of How Turbulence Enables the Explosion of Core-Collapse ... · Quintin Mabanta & Jeremiah Murphy...
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How Turbulence Enables the
Explosion of Core-Collapse Supernova
Quintin Mabanta & Jeremiah Murphy
Ringberg Workshop
July 25th, 2017
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1-D simulations do not explode,
yet multi-D do
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Simulations suggested, but did not prove,
that turbulence is the dominant
factor that aids explosion
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We develop a self-consistent turbulence
model and show that it reduces the
critical conditions for explosion
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The semi-analytic nature also allows us to
explain how it enables explosion
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Outline
● Background
➢ Why turbulence is important
➢ “Critical Curve”
● Methodology
➢ Reynolds decomposition
➢ Turbulence Models
➢ Isolating Turbulent Terms
➢ Source of Energy for Turbulent Dissipation
● Results and Future Work
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The fundamental question is: how does the stalled
shock revive into an blastwave?
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Reviving the Shock
● Bethe and Wilson (1985) hypothesized that neutrino heating alone
revitalized the shock
● As the core heats up, a few processes are involved
○ Nuclear Dissociation○ Electron Capture○ Positron Capture
● Energy is converted to neutrinos
○ p + e- → n + νe
○ n + e+ → p + v
e
● Lightbulb Model
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1-Dimensional hydrodynamic and neutrino transport simulations
have been unsuccessful in creating realistic supernovae...
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Multi-D succeeds where 1-D fails
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How does turbulence aid explosion?
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● People suspect that turbulence is a key contributor to
successful supernova explosions (Murphy & Burrows 2008;
Marek & Janka 2009; Murphy & Meakin 2011; Hanke+ 2012;
Murphy+ 2013; Couch & Ott 2015; Melson+ 2015; Radice+
2016; etc.)
● Though there is some progress, these are guesses and
suppositions. No one had yet shown how turbulence aids
explosion
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Simulations are important, but they’re often
complex and computationally expensive, making it
difficult to thoroughly investigate the various
effects
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We use another approach, which is to build upon
and develop a semi-analytic theory, which enables a
deeper understanding of the mechanisms at play
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The Big Picture
Murphy & Dolence (2017)
My Parameters
● M
NS
: 1.5 M
☉
● R
NS
: 65 km
● Tν: 4 MeV
● Let Ṁ vary
● Find critical Lν
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Original Critical Curve
Burrows & Goshy (1993)
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Some Inspiration
Murphy & Burrows (2008)
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Outline
● Background
➢ Why turbulence is important
➢ “Critical Curve”
● Methodology
➢ Reynolds decomposition
➢ Turbulence Models
➢ Isolating Turbulent Terms
➢ Source of Energy for Turbulent Dissipation
● Results and Future Work
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Let’s augment this critical condition analysis to
include turbulence in a self-consistent way
With Reynolds decomposition, we can explore how
turbulence reduces the critical curve
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Start With Continuity Equations
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Equations With Turbulence
● By Reynolds decomposing our equations we can peer into the various
components involved in creating a successful supernova explosion
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L
e
= 4πr
2ρ<e′v′>
R = v′rr
2
+ v′θθ2
+ v′ϕϕ2
ε
= ν [∇2
<R> − 2(∇v′)·(∇v′ )]
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By introducing these new terms, we now have more
unknowns than equations
Must develop a model for the turbulent dissipation
(εk
), the Reynolds stress (R), and turbulent
luminosity (L
e
)
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Two Sources of Turbulence
Standing Accretion Shock
Instability (SASI)
Neutrino Driven
Convection
Murphy+ (2013) Müller+ (2012)
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To correctly incorporate these effects we need
a non-linear model for turbulence
A non-linear model exists for convection but not yet for the SASI
(work in progress by Erica Bloor)
For now, Neutrino Driven Convection is the only model
we have to probe for the intricacies turbulent dynamics
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Making some constraints...
● From Murphy & Dolence
(2013), we can impose a few
conditions on the turbulent
kinetic energy and turbulent
luminosity. Namely:
➢ W
B
= E
k
➢ Lντ = E
K
+ L
e
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The radial Reynolds stress is in rough equipartition
with both of the tangential components
Rϕϕ + R
θθ
~ R
rr
The transverse components are roughly balanced
Rϕϕ ~ R
θθ
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Following Kolmogorov’s hypothesis, we can also
approximate the turbulent dissipation to be:
εk
= v′3ℒ -1
= R
3/2ℒ -1
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We need some sort of local description
Based upon simulations, we have
a profile for these terms
We use the global conditions
to set the scales
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Some Assumptions...
● E
k
~ Ɛk
M
g
● We take the lengthscale of convection to
be the entire length of the gain region
● Use a hypertangent prescription of
the Turbulent Luminosity
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Outline
● Background
➢ Why turbulence is important
➢ “Critical Curve”
● Methodology
➢ Reynolds decomposition
➢ Turbulence Models
➢ Isolating Turbulent Terms
➢ Source of Energy for Turbulent Dissipation
● Results and Future Work
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Altered Density and Temperature Profiles
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How Turbulence Affects the Profile
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How Turbulence Affects the Critical Curve
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So what is the source of the energy
for turbulent dissipation?
Is there double counting of the neutrino energy?
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Conversion of Convective Kinetic Energy to Heat
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Summary
● Simulations suggest that multidimensional effects ease explosion
● Burrows & Goshy (1993) constructed a critical curve which divided the
boundary between which steady-state solutions do or do not exist
● We include turbulence self-consistently in a critical conditions analysis
(Reynolds decomposition)
● Investigate how turbulence reduces the critical condition
● All turbulent effects play a role in this reduction, but we find turbulent
dissipation to be the dominant effect
● We implore simulators check our assumptions and check the values of R,
εk
, and L
e
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Looking Forward
● Implement a more rigorous neutrino transport model (two-moment
closure, ray-by-ray, Boltzmann transport)
● Verify and validate our model with 3-D simulations
● Incorporate SASI..?
● Probe how sensitive the critical curve is to other detailed physics (e.g.
General Relativity, Equation of State, absorption cross-section, etc.)
Thanks!