View
3
Download
0
Category
Preview:
Citation preview
Supernovae as Nature’s Particle Physics ExperimentsShuai Zha1, Shing Chi Leung1,2, Lap Ming Lin1 & Ming-chung Chu1
1Department of Physics, The Chinese University of Hong Kong, Hong Kong2Kavli IPMU (WPI), UTIAS, The University of Tokyo, Japan
QCS2017, Yukawa Institute, Kyoto University, Feb 20-22, 2017
1
2
Hong Kong
The Chinese University of Hong Kong
3
Supernovae as Nature’s Particle Physics Experiments
- Type IA (SNIa) and Core-collapse supernovae (CCSNe)
- Equations of State (EOS)
- Hydrodynamic Simulation
- Results: - Dark matter admixed SNIa- Quark phase in core-collapse SN: gravitational-wave and
neutrino signals
- Summary
4
Type IA Supernovae
- progenitor: C-O white dwarf accreting to Chandrasekhar limit ~1.4 Mʘ
- But: 1. sub-luminous SNIa found2. small admixture of fermionic dark matter can significantly lower the Chandrasekhar massS.-C. Leung et al., PRD 87, 123506 (2013).
S.-C. Leung, M.-C. Chu, L.-M. Lin, ApJ 812, 110 (2015).
- Our work: effects of fermionic dark matter admixture on SNIa. Can perculiar SNIa signal dark matter admixture?
- Thermonuclear runaway of the reaction 14 12C →3 56Ni. 56Ni powers the light curves by its decay energy 56Ni → 56Co → 56Fe - believed to be standard candles
Also: see S.C. Leung’s poster on dark matter admixed Accretion Induced Collapse
5
Core-collapse supernovae
http://www.mpa-garching.mpg.de/112431/hl201504
Credit: Tobias Melson, Hans-Thomas JankaT. Melson, H.-T. Janka, & A. Marek, ApJ Letts 801, L24 (2015).
- Stars with mass > 10 Mʘ Fe core collapse Type II supernova, neutron star or black hole
- Important for spreading heavy elements
- Some of the most energetic events; may affect galaxy and/or dark matter halo evolution
- Prompt shock stalls (photodisintegration, neutrino emission)
- Convection enhances neutrino energy deposition revives shock
- need multi-dimensional hydro with realistic neutrino transport
S. E. Woosley et al., Rev. Mod. Phys. 74, 1015 (2002).)
6
Core-collapse supernova as a route to quark star?
K. Nakazato et al., PRD 77, 103006 (2008); PRD 81, 083009 (2010); A&A 558, A50 (2013). I. Sagert et al., PRL 102, 081101 (2009); T. Fischer et al., ApJS 194, 39 (2011).
- Hybrid EOS with quark phase (HShen + Bag Model)- General relativistic radiation hydrodynamics + Boltzmann neutrino
transport AGILE-BOLTZTRAN- Spherical symmetry- Quark phase transition at low enough density (B = 90 MeVfm-3)
second collapse and delayed shock (100’s ms)- Core: Quark/hybrid star for 15 Mʘ; black hole for 40 Mʘ- Second neutrino burst
M. Takahara and K. Sato, ApJ. 335, 301 (1988); N. A. Gentile et al., ApJ. 414, 701 (1993).
Our work: extend to 2D (3D?) important for explosion hydro, rotating collapse, gravitational-wave signals. Aim: correlated Gravitation-wave and neutrino signals signals for quark stars
7
- Hybrid EOS: HShen + MIT Bag Model (Bag constant = B), Gibbs construction of the mixed phase
Hybrid Equation of State (EOS)
K. Nakazato et al., PRD 77, 103006 (2008).
- Quark phase softer EOS
T = 100 MeV
T = 5 MeV
T = 50 MeV
Baryon no. density nB (fm-3)Q
uark
frac
tion
f Qua
rk
B1/4 = 165 MeV
Pres
sure
P(d
yne/
cm2 )
Baryon no. density nB (fm-3)
H. Shen et al., Nucl. Phys. A 637, 435 (1998); H. Shen et al., Prog. Theor. Phys. 100, 1013 (1998).
8
Hydrodynamics
EULER EQUATIONS (2D)5th order WENO 3rd order Runge-Kutta
Particle TracerNucleosynthesis
Opacity databaseRadiative transfer
Flame-capturing schemeLevel-set method (default)Point-set method
Nuclear reaction19 isotope networkAlpha-chain network(Timmes)
Deflagration physicsDetonation physics
HShen EOS , , ,P T A ZHshen + MIT Bag EOS (B)
Neutrino transport IDSA
SC Leung et al., MNRAS 454, 1238 (2015).
Pre-bounce neutrino physicsElectron-captureNeutrino heating
Helmholtz EOS
9
Isotropic Diffusion Source Approximation
M. Liebendörfer et al., ApJ 698, 1174(2009).
Diffusion source: coupling between trapped and streaming neutrinos
10
Detailed comparisons with results in literature 1D shock-tube tests 2D hydrodynamics tests Standard PTD model Standard DDT model
Pure turbulent deflagration model
Delayed detonation transition model
Code test
RESULTS – DARK MATTER ADMIXED SNIA Weaker explosion Less turbulent Weaker hydrodynamics instabilities Lower amount of 56Ni
Higher MDM(0 0.03 Msun)
No DM
MDM = 0.03 Mʘ
11
SUB-LUMINOUS SNIA
Lower 56Ni = Lower peak luminosity A wide range in peak luminosity Using peak luminosity to guess MDM
More DM
12
Results – Core-collapse SNe (Preliminary)
13
- 2nd collapse occurs ~ 0.4 s (tb2) after the first one, producing a very strong shock.
- 2nd collapse occurs for B1/4 = 165 MeV
B1/4 = 165 MeV
B1/4 = 145 MeV (α = 0.7)
tb2t – tb (s)
(g
/cc)
2nd collapse for B1/4 = 165 MeV
tb2
tb2+ 4.3 ms
tb2+4.4ms
tb2+4.7ms
r (km)
v/c
414.4ms414.3ms400.0ms
Progenitor: M = 12 Mʘ (S. E. Woosley et al., Rev. Mod. Phys. 74, 1015 (2002).)
Stalled accretion shock from first collapse
14
r (km)
v/c
Prompt shock
10 100 1000
(g/c
c)
Quark star
Proto-neutron star
Core
5 10 15 20r (km)
B1/4 = 165 MeV
B1/4 = 165 MeV
Results – Quark Phase (Preliminary)
15
Neutrino signals
L (e
rg/s)
t – tb (s)<
E>(M
eV)
t – tb (s)
- 2nd neutrino burst is about as strong as the first one.
e
e
e
e
B1/4 = 165 MeV
16
Gravitational-wave signals
- Generated rotating progenitor (1.5 s rotation period)- Calculated from quadrupole formula.- G-wave signals more or less similar for different EOS’s for the first collapse.
x10-22
-10 -5 0 5 10
t – tb (ms)
17
Gravitational-wave signals
B1/4 = 165 MeV
B1/4 = 145 MeV
HShenHshen +b145Hshen +b165
t – tb (ms) t – tb2 (ms)-10 -5 0 5 10
After 2nd collapsex10-22 x10-21
- Gravitational-wave signal from 2nd collapse is even stronger (3x) than from the first one for B1/4 = 165 MeV, with shorter period.
18
Summary
- Core-collapse Supernovae simulated with and without quark phase transition (preliminary)
- 2D hydro + WENO shock capturing + IDSA neutrino transport
- Quark phase transition second collapse, generating strong shock, if B large enough (B1/4 = 165 MeV, but NS mass is only 1.5 Mʘ)
- A mechanism for CCSNe?
- Clear Neutrino and Gravitational-wave signals- Worth more detailed study
- Dark matter admixed SNIa: Weaker explosion, lower amount of 56Ni → sub-luminous SNIa
Supernovae as Nature’s Particle Physics ExperimentsShuai Zha1, Shing Chi Leung1,2, Lap Ming Lin1 & Ming-chung Chu1
1Department of Physics, The Chinese University of Hong Kong, Hong Kong2Kavli IPMU (WPI), UTIAS, The University of Tokyo, Japan
QCS2017, Yukawa Institute, Kyoto University, Feb 20-22, 2017
19
Recommended