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