LVCSupernovaWorkshopSearchesPanel Mezzacappa V2 · 00.2 0.40.6 0.8 1 1.2 Time from bounce [s] 0 0.2...

8
Stellar Core Bounce ProtoNeutron Star (PNS) Instabilities PostShock Region NeutrinoDriven Convection Induced Standing Accretion Shock Instability (SASI) Induced 0 0.2 0.4 0.6 0.8 1 1.2 Time from bounce [s] 0 0.2 0.4 0.6 0.8 Explosion Energy [B] W-H 12 solar mass progenitor W-H 15 solar mass progenitor W-H 20 solar mass progenitor W-H 25 solar mass progenitor Explosion Energy versus Progenitor Mass Wossley-Heger 12, 15, 20, 25 Solar Mass Nonrotating Progenitors; 256 x 256 Spatial Resolution Explosion 3/29/2017 1 Kei Kotake will give an extensive overview as part of the Status of Core Collapse Supernova Modeling Panel.

Transcript of LVCSupernovaWorkshopSearchesPanel Mezzacappa V2 · 00.2 0.40.6 0.8 1 1.2 Time from bounce [s] 0 0.2...

Page 1: LVCSupernovaWorkshopSearchesPanel Mezzacappa V2 · 00.2 0.40.6 0.8 1 1.2 Time from bounce [s] 0 0.2 0.4 0.6 0.8 Explosion Energy [B] W-H 12 solar mass progenitor W-H 15 solar mass

Stellar Core Bounce Proto‐Neutron Star(PNS) Instabilities

Post‐ShockRegion

Neutrino‐DrivenConvection Induced

Standing AccretionShock Instability (SASI)

Induced

0 0.2 0.4 0.6 0.8 1 1.2Time from bounce [s]

0

0.2

0.4

0.6

0.8

Expl

osio

n En

ergy

[B]

W-H 12 solar mass progenitorW-H 15 solar mass progenitorW-H 20 solar mass progenitorW-H 25 solar mass progenitor

Explosion Energy versus Progenitor MassWossley-Heger 12, 15, 20, 25 Solar Mass Nonrotating Progenitors; 256 x 256 Spatial Resolution

Explosion

3/29/2017 1Kei Kotake will give an extensive overview as part of the 

Status of Core Collapse Supernova Modeling Panel.

Page 2: LVCSupernovaWorkshopSearchesPanel Mezzacappa V2 · 00.2 0.40.6 0.8 1 1.2 Time from bounce [s] 0 0.2 0.4 0.6 0.8 Explosion Energy [B] W-H 12 solar mass progenitor W-H 15 solar mass

3/29/2017 2

r = 10 km

f m = 0.1f maxm

f m = 0

�= 1010 g/ cm3

Standing accret ion shock

A A1

A2B

C

PNS

Sources of Gravitational Radiation

(1) PNS convection in region A.

(2) Acoustic waves in the PNS initiated by PNS convection.

(3) Deceleration of infalling convective plumes.

(4) Excitation of PNS g‐modes by these down flows (2D) or by PNS convection (3D).

• Andresen et al. 2017 arXiv:1607.05199

• Marek, Janka, and Mueller, A&A 496, 475 (2009)• Murphy, Ott, and Burrows Ap.J. 707 1173 (2009)• Mueller, Janka, and Marek Ap.J. 766, 43 (2013)

The late‐time, high‐frequency GW is given by the g‐modefrequency in B (A2) for the 2D (3D) case.

g‐Mode Frequency (Brunt‐Vaisala Frequency)

(5) SASI‐Induced Modulation (Low Frequency)

Page 3: LVCSupernovaWorkshopSearchesPanel Mezzacappa V2 · 00.2 0.40.6 0.8 1 1.2 Time from bounce [s] 0 0.2 0.4 0.6 0.8 Explosion Energy [B] W-H 12 solar mass progenitor W-H 15 solar mass

3/29/2017 3Yakunin et al. 2015 PRD 92 084040 

Quasi‐Spherical Collapse=> Bounce Signal Absent

Page 4: LVCSupernovaWorkshopSearchesPanel Mezzacappa V2 · 00.2 0.40.6 0.8 1 1.2 Time from bounce [s] 0 0.2 0.4 0.6 0.8 Explosion Energy [B] W-H 12 solar mass progenitor W-H 15 solar mass

Prompt ConvectionAcoustic Waves

Quiescent Phase

Neutrino‐Driven Convection/SASI Induced g‐Modes

Deceleration of Convective Plumes(Stochastic)

Correlated

3/29/2017 4Mueller, Janka, and Marek Ap.J. 766, 43 (2013)

Page 5: LVCSupernovaWorkshopSearchesPanel Mezzacappa V2 · 00.2 0.40.6 0.8 1 1.2 Time from bounce [s] 0 0.2 0.4 0.6 0.8 Explosion Energy [B] W-H 12 solar mass progenitor W-H 15 solar mass

3/29/2017 5Yakunin et al. 2015 PRD 92 084040 

Cessation of accretion corresponds to cessation of high‐frequency component of GW amplitude.

Page 6: LVCSupernovaWorkshopSearchesPanel Mezzacappa V2 · 00.2 0.40.6 0.8 1 1.2 Time from bounce [s] 0 0.2 0.4 0.6 0.8 Explosion Energy [B] W-H 12 solar mass progenitor W-H 15 solar mass

3/29/2017 6

Yakunin et al. 2015 PRD 92 084040 

Distinguish convection‐ and SASI‐dominated models by ratio of high‐ to low‐frequency power?• Andresen et al. 2017 arXiv:1607.05199

Page 7: LVCSupernovaWorkshopSearchesPanel Mezzacappa V2 · 00.2 0.40.6 0.8 1 1.2 Time from bounce [s] 0 0.2 0.4 0.6 0.8 Explosion Energy [B] W-H 12 solar mass progenitor W-H 15 solar mass

3/29/2017 7

Comparisons use same time window (from 3D) and temporal resolution (from 2D).Yakunin et al. 2017, arXiv:1701.07325v1  

See also Andresen et al. 2017 arXiv:1607.05199.

Page 8: LVCSupernovaWorkshopSearchesPanel Mezzacappa V2 · 00.2 0.40.6 0.8 1 1.2 Time from bounce [s] 0 0.2 0.4 0.6 0.8 Explosion Energy [B] W-H 12 solar mass progenitor W-H 15 solar mass

3/29/2017 8

Collapse

Bounce

Ring Down

Kuroda, Takiwaki, and Kotake PRD 89 044011 (2014)

What happens at late times?