Konstantin Yakunin Joint Institute for Computational Sciences Oak - - PowerPoint PPT Presentation

Konstantin Yakunin Joint Institute for Computational Sciences Oak Ridge National Laboratory Particle Physics and Astro-Cosmology Seminar, UTK

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Credit: NASA/Dana Berry, Sky Works Digital Credit: Emil Ivanov Credit: LSC Credit: LSC

The first GW signals were detected on 14 September 2015 and 26 December 2015 GW151226 Duration 1.0 s Distance 440 ± 180 MPc M1 = 14.2 and M2 = 7.5 Frequency: 35 – 450 Hz SNR = 13 (σ =5.0) GW150914 Duration 0.2 s Distance 440 ± 160 MPc M1 = 36 and M2 = 29 Frequency: 35 – 250 Hz SNR = 24 (σ =5.1)

CCSNe Observation

Formal MOU!

Credit: StudyBlue

Strongest GW signal: Rotating progenitor Non-rotating progenitor

Core Bounce PNS Instabilities Neutrino-Driven Convection SASI

Time from bounce [s]

Explosion Energy [B]

Explosion Energy versus Progenitor Mass

Explosion

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Burrows et al. 2007, Ap.J. 664, 416

• ,

=

• Bruenn et al. 2016, Ap.J. 818, 123

Richers et al. 200=17, arxiv:1701.02752

Long signal (> 1 sec), low, moderate amplitude Short signal (< 50 ms), high amplitude at bounce

Rapidly rotating progenitors Non-rotating or slowly rotating progenitors

Landscape of CCSNe

✴ Rapidly rotating progenitor ~ 1% of expected CCSNe ✴ Rotation profile is parameterized by central angular

velocity and a differential rotation Slowly Rotating

✴ Prompt convection ✴ Neutrino-driven

convection & SASI

✴ PNS convection

Rapidly Rotating

✴ Bounce/ringdown of

millisecond PNS

✴ low T/|W| instabilities

Self-Consistent Supernova Model

2D Explosion Models

500 1000 500 1000 500

• 500
• 1000

1000

B12-WH07 B15-WH07 B20-WH07 B25-WH07

Distance along symmetry axis [km] Distance from symmetry axis [km] 500 1000 500 1000 500 1000 500 1000 500 1000 500 1000 500

• 500
• 1000

1000 500

• 500
• 1000

1000 500

• 500
• 1000

1000 Distance from symmetry axis [km] Distance along symmetry axis [km]

Bruenn et al. ApJ, 818, 123 (2016)

Explosion Energy [B] B12-WH07 B15-WH07 B20-WH07 B25-WH07 0.2 0.4 0.6 0.8 1 1.2 1.4 1.6 E+ = Energy sum over positive energy zones E+

• v = E+

+ Overburden E+

• v, rec = E+
• v + Nuclear recombination

0.30 200 400 600 800 1000 1200 1400 Time After Bounce [ms] 10 15 20 25 ZAMS Progenitor Mass [M☉] 0.02 0.04 0.06 0.08 0.1 0.12

56Ni Mass [M☉]

SN 2012aw SN 2004A SN 2004dj SN 2004et SN 1993J SN 1987A SN 2005cs

Structure of GW Signal from 2D model

Prompt convection (30 ms) SASI and active accretion on PNS (228 ms) Explosion and shock expansion (780 ms) Yakunin et al. PRD, 92, 084040 (2015)

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Yakunin et al. 2015 PRD 92 084040

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Yakunin et al. 2015 PRD 92 084040

Results obtained with the CHIMERA GR multiphysics supernova code with state-of-the-art neutrino interactions.

• Simulations: signal characteristics (f, A, etc);

physical mechanism producing GW signals, bank of waveforms

• Signal Search: search algorithms based on

the most reliable parts of waveforms, proposal of detector design to observe physical properties of supernovae via GW signals

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Thanks to Marek Szczepanczyk SNR = 41 SNR = 6

5

Evolution of ground based detectors

Third generation: From 10 to 1Hz 10 x lower thermal noise 10 x times lower quantum (shot) noise

Waveform

cWB Distance (Mpc) @ 50% hrss

FC Distance (Mpc) GRB Distance (Mpc)

LB1 0.732 5 5 LB2 2.252 5 5 LB3 0.191 5 5 LB4 3.292 5 5 LB5 11.511 15 15 Piro1 0.891 5 5 Piro2 4.409 15 15 Piro3 2.445 5 5 Piro4 12.569 15 15

Waveform

cWB Distance (Mpc) @ 50% hrss

FC Distance (Mpc) GRB Distance (Mpc)

Muller1-N20-2

0.38 1 5

Muller1-L15-3

0.47 1 1

Muller1-W15-4

0.99 N/A 1 Yak1 0.002 0.5 0.1 Yak2 0.001 0.5 0.5 Yak3 0.002 0.1 0.1 Yak4 0.004 0.5 0.5

aLIGO CCSNe Detection Distance

3G CCSNe Detection Distance

The Search for GWs from CCSNe

GW emission from core-collapse detectable

• ut to ~100kpc

Extreme post-core- collapse GW emission models detectable out to ~10-15 Mpc

[3] Gill et al. 2017

NAME TALK TITLE DATE NAME DATE TALK TITLE 03/17/2017 SN Workshop 2017 Kiranjyot Gill

CCSNe Rate within 20 Mpc

5 10 15 20 100 200 300 400 500 600 Distance (Mpc) Rate of CCSNe per Century Li 2011 Galaxy Conversion Cappellaro 1996 Galaxy Conversion

Virgo Cluster

Local Group M81 Group

[3] Gill et al. 2017

Super-K LVD IceCube Borexino

snews.bnl.gov

SNEWS: SuperNova Early Warning System

KamLAND Daya Bay HALO

Expect time of flight delay for massive neutrinos

Distance reach of detectors

SK will see ~1 event from Andromeda; HK will get a ~dozen

Neutrino Detectors

Summary of supernova neutrino detectors

G a l a c t i c s e n s i t i v i t y Extragalactic

Detector Type Location Mass (kton) Events @ 10 kpc Status

Super-K Water Japan 32 8000 Running LVD Scintillator Italy 1 300 Running KamLAND Scintillator Japan 1 300 Running Borexino Scintillator Italy 0.3 100 Running IceCube Long string South Pole (600) (106) Running Baksan Scintillator Russia 0.33 50 Running HALO Lead Canada 0.079 20 Running Daya Bay Scintillator China 0.33 100 Running NOνA Scintillator USA 15 3000 Running MicroBooNE Liquid argon USA 0.17 17 Running SNO+ Scintillator Canada 1 300 Under construction DUNE Liquid argon USA 40 3000 Future Hyper-K Water Japan 540 110,000 Future JUNO Scintillator China 20 6000 Future PINGU Long string South pole (600) (106) Future

plus reactor experiments, DM experiments...

LIGO-CCSN Collaboration

CCSNe Theory LIGO Burst Data Analysis

CCSNe Data Analysis

From 2D to 3D

512(r) x 256(θ) à 256 processors Angular resolution < 1° 540(r) x 180(θ) x 180(ɸ) à 32400 processors Angular resolution ~ 2° Efficiency of the code: 100 ms/month à 100 ms/week Ray by Ray structure 2D 3D

2D vs 3D Supernova Explosion

50 100 150 200 250 300 350 400 450 Time [ms] 50 100 150 200 250 300 350 400 450 500 550 600 650 700 750 800 C15-2D Minimum/maximum C15-1D C15-3D Mean shock radius Shock radius [km]

100 150 200 250 300 350 400 450 Time [ms] 0.1 0.2 0.3 0.4 Diagnostic energy [B] C15-3D C15-2D

a)

Lentz et al. ApJL, 807, L31 (2015) Shock Radius Explosion Energy

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Yakunin et al. 2017, arXiv:1701.07325v1

Comparisons use same time window (from 3D) and temporal resolution (from 2D). Results obtained with the CHIMERA GR multiphysics supernova code with state-of-the-art neutrino interactions.

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Yakunin et al. 2017, arXiv:1701.07325v1

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Most reliable part of signal Most reliable part of signal in frequency domain

Andresen et al. 2016

−2 2 A+[cm] 25 125 225 325 −2 2 A×,

s11.2

3/29/17 30 Dimmelmeier et al. PRD, 064056,2008 Kotake et al. PRD, 044023, 2003 Schreidegger et al. A&A, 2010 Richers et al. arxiv:1701.02752

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A possible bounce signal

Emission process Duration (ms) fpeak [Hz] Typical h at 10 kpc EGW [Mc2] Core Bounce 10 300 3x10-21 ~10-8 Prompt convection 50 200 0.3x10-21 ~10-12 SASI/ND convection 450 700 1x10-21 2x10-9 Δt/100ms Explosion >400 800 0.7x10-21 2x10-9

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• Simulations help to improve data analysis and increase chances for

detection!

• We are able to perform realistic 3D simulations and produce reliable

waveforms.

• Waveforms from 2D simulations have similar characteristics as 3D ones.

Thus, 2D simulations can be used to create a bank of waveforms. Now, even realistic 2D simulations are computationally inexpensive.

• It would be good to summarize the main characteristics of GW signals into a

table in any publication that presents new waveforms

• To produce more realistic waveforms we have to perform realistic CCSN

simulations with slow-rotating progenitor (bounce signal + neutrino-driven explosion signal)

Bruenn Marronetti Blondin Mauney Casanova Chu Endeve Hix Landfield Lentz Lingerfelt Messer Mezzacappa Roberts Yakunin

Funded by

33 3/29/17

Harris