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Gravitational SIGNATURE of Core-Collapse Supernovae

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Presentation on theme: "Gravitational SIGNATURE of Core-Collapse Supernovae"— Presentation transcript:

1 Gravitational SIGNATURE of Core-Collapse Supernovae
Konstantin Yakunin (Florida Atlantic University) In collaboration with S. Bruenn (FAU), P. Marronetti (FAU), A. Mezzacappa (ORNL-UTK) and the CHIMERA Team (ORNL-FAU-NCSU) GWPAW, Millowakee November 13, 2018

2 Funded by Blondin Warren Bruenn Dirk Marronetti Fuller Yakunin
Budiardja Cardall Endeve Hix Lentz Messer Mezzacappa Parete-Koon Funded by Collaborators Solvers: D’Azevedo Data Management: Barreto, Canon, Klasky, Podhorszki Networking: Beck, Moore, Rao Visualization: Ahern, Daniel, Ma, Meredith, Pugmire, Toedte Cray Center of Excellence: Levesque, Wichmann GWPAW, Millowakee November 13, 2018

3 How is the SN shock revived?
Known, Potentially Important Ingredients Gravity Neutrino Heating Convection Shock Instability Nuclear Burning Rotation Magnetic Fields Need 3D models with all of the above, treated with sufficient realism. GWPAW, Millowakee November 13, 2018

4 CHIMERA Bruenn et al., Journ. Phys. Conf. Ser., 180, (2009) “RbR-Plus” MGFLD Neutrino Transport O(v/c), GR time dilation and redshift, GR aberration (in flux limiter) 2D PPM Hydrodynamics adaptive radial grid Lattimer-Swesty EOS Cooperstein et al. for low densities Nuclear (Alpha) Network 14 alpha nuclei between helium and zinc 2D Effective Gravitational Potential Marek et al. A&A, 445, 273 (2006) GR time dilation, effective gravitational potential, “Ray-by-Ray-Plus” Approximation Radial transport allowed. Lateral transport suppressed. Buras et al. A&A, 447, 1049 (2003) GWPAW, Millowakee November 13, 2018

5 15 M Progenitor collapse in 2D
GWPAW, Millowakee November 13, 2018

6 GWPAW, Millowakee November 13, 2018

7 Murphy, Ott, and Burrows, Ap.J. 707, 1173 (2009)
CHIMERA simulation for 15 M progenitor GWPAW, Millowakee November 13, 2018

8 Effective GR potential & LS EoS
Gravitational WAVE Murphy, Ott, and Burrows (2009) CHIMERA Newtonian potential & Shen EoS Effective GR potential & LS EoS GWPAW, Millowakee November 13, 2018

9 Gravitational WAVE Marek and Janka (2009) CHIMERA simulation
GWPAW, Millowakee November 13, 2018

10 Gravitational Wave extraction
Neutrinos Epstein-Müller approximation R - distance from the source to the observer θ, φ - direction angles of neutrino emission in observer’s frame dLν/dΩ - direction dependent neutrino luminosity GWPAW, Millowakee November 13, 2018

11 GW from Neutrino emission
GWPAW, Millowakee November 13, 2018

12 TracER PARTICLE METHOD
Heger 15 model: 5000 particles = 40 per row X 125 rows Post-bounce time = 0 ms Post-bounce time = 5 ms Post-bounce time = 157 ms GWPAW, Millowakee November 13, 2018

13 TRAcER ANALYSIS Low frequency component of early signal (tb<100 ms) produced by deflection of infalling matter through the shock GWPAW, Millowakee November 13, 2018

14 Detectability by ADV. ligo
CHIMERA simulation for 15 M progenitor GWPAW, Millowakee November 13, 2018

15 Conclusions 2D simulations of core-collapse SN show sustained explosions for a range of non-rotating progenitors There is qualitative agreement between several groups on the main characteristics of the GW signals from 2D Core Collapse Supernovae simulations Galactic event detection by AdvLIGO will provide unique insights of the collapse dynamics and proto-neutron star structure 3D simulations are necessary for the complete realistic GW waveforms GWPAW, Millowakee November 13, 2018

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