Neutrino Signature from Multi-D Supernova Models

Transcription

1 Neutrino Signature from Multi-D Supernova Models David Radice 1,2 A. Burrows, J. C. Dolence, S. Seadrow, M. A. Skinner, D. Vartanyan, J. Wallace 1 Research Associate, Princeton University 2 Schmidt Fellow, Institute for Advanced Study νeclipse 2017

2 Core-Collapse Supernovae Cassiopeia-A ~ (50 yr) -1 per galaxy few every second in the observable universe Peak luminosity ~10 10 solar erg EM radiation erg kinetic energy erg neutrinos Problem: how do they explode? Neutrinos could tell us!

3 Numerical Modeling General relativistic gravity Hydrodynamics Nuclear equation of state Neutrino radiation transport First 1D simulations Colgate & White 1966 First 1D full-physics simulations only early 2000s From Dolence, Burrows, et al No single multi-d code has everything!

4 Fornax A new CCSN code Spherical dendritic grid Multi-dimensional M1 neutrino O(v/c) transport Newtonian with effective GR potential 1D, 2D, and 3D Dolence, Skinner, et al., in prep 2017

5 Current Efforts in Princeton* Explosion mechanism: crucial physical dependencies [Burrows, Vartanyan,, DR 2016 Vartanyan et al., in prep 2017] Low-mass progenitors: electron-capture vs regular CCSNe [DR, Burrows, et al. 2017] Neutrino detection: shock-breakout burst [Wallace, Burrows, and Dolence 2016] Neutrino detection: explosion signatures [Seadrow et al., in prep 2017] Stay tuned for 3D results! * and collaborators at LANL, LLNL

6 Massive Star Explosions Vartanyan et al., in prep 2017

7 Many-Body Effects 1 V d d = G2 F E ga(3 2 cos )(n n + n p )S A + (1 + cos )n n S V. From Horowitz et al. 2017

8 Many-Body Effects s9.0-ls220 DR, Burrows, et al 2017

9 Many-Body Effects s9.0-ls220 DR, Burrows, et al 2017

10 Many-Body Effects s9.0-ls220 DR, Burrows, et al 2017

11 Many-Body Effects s9.0-ls220 DR, Burrows, et al 2017

12 Many-Body Effects s9.0-ls220 DR, Burrows, et al 2017

13 Protoneutron Star Convection From Buras et al 2006 See also Dessart, Burrows et al. 2006

14 Protoneutron Star Convection PNS unstable to Ledoux convection Modest impact on neutrino luminosities in the first 250 ms (especially heavy-lepton neutrinos) What happens over longer times? Check with progenitors exploding in self-consistent 1D simulations From Buras et al 2006 See also Dessart, Burrows et al. 2006

15 Protoneutron Star Convection DR, Burrows, et al 2017

16 Shock Breakout Signal Wallace, Burrows, and Dolence 2016

17 Shock Breakout Signal The Astrophysical Journal, 817:182 (24pp), 2016 February 1 4pp), 2016 February 1 Hyper-K Wallace, Figure Burrows, 6. Example and Dolence realization 2016 of detection rates in the no-oscillation case with

18 Shock Breakout Signal The Astrophysical Journal, 817:182 (24pp), 2016 February 1 Figure 16. Similar to Figure 14, but using the neutrino oscillations expecte Wallace, Burrows, and Dolence 2016

19 Figure 14. For Hyper-K (left) and Super-K (right), the expected light curve for SNe at 4, 7, and 10 kpc, inc Wallace, the NH. Burrows, Detections and of Dolence neutrinos2016 of all flavors are taken into account, with IBDs and NC scattering off of o 4 Shock Breakout Signal The Astrophysical Journal, 817:182 (24pp), 2016 February 1

20 Shock Breakout: Detectability Figure 21. Same as Figure 18, but for DUNE in the IH case. For DUNE, signals have been subtrac Figure 22. Similar to Figure 11, but for Ln n e,max (left), t max (middle), and t rise,1/2 (right), in the no-oscillation case. In a not plotted beyond 1 kpc, and the data are shown as a single point rather than a line connecting multiple points. Breakout burst can provide accurate timing of core bounce Most Likely Value and Perce Model Employing the LSEO Wallace, Burrows, and Dolence 2016

21 Shock Breakout: Luminosity The Astrophysical Journal, 817:182 (24pp), 2016 February 1 Figure 21. Same as Figure 18, but for DUN Wallace, Burro Figure 11. The 95% uncertainty in measuring Ln n e,max as a function of distance for various detectors for the 15 M e LSEOS model, in the no-oscillation case. For each detector, the lines represent the span needed to include 95% of the Ln n e,max s calculated from the set of sampled observations. When the uncertainty values for a specific detector get either too large or too small relative to the model value, we stop plotting the uncertainty at that distance and greater distances. The uncertainty values for Super-K and JUNO were cut off at 7 kpc if the previous criteria were not met at 7 kpc because of the small number of events for an SN beyond that distance. no-oscillation case, can determine t max to within model value out to a distance of 7 kpc. Table 1 that the value of t max most likely to be measured the PDF of t max in our analysis) is displaced fro t max through many of the SN distances under However, this offset of the most likely measured v fraction of the error expected in a measureme Hyper-K for reasonable SN distances ( 7 kpc) important. DUNE can measure t max to an accur out to 7 kpc in the no-oscillation case. Again distance the measurement has a possibility of bein accurate with increasing model progenitor ma accurate for the Shen EOS. JUNO and Super-K oscillation case, cannot make a measurement wi the model value for an SN at distances greater tha all distances and models, in the no-oscillation c Figure 22. willsimilar be thetomost Figure likely 11, but to for accurately Ln n e,max (left), measure t max (mi t ma not plottedwe beyond have1 defined kpc, andt max the in datasuch are shown a wayas that a single it is distinguishing between progenitor models and E accurate measurement of t max in multiple detec useful in triangulating the position of the SN. Peak luminosity measurement only for nearby supernovae Wallace, Burrows, and Dolence Detector Performance for Measurin

22 Neutrino Light-Curves n luminosities [10 51 erg s 1 ] D 2D 11.0 Baseline r = 10, 000 km 0.5 L nµ n e n e n µ 0 n rms energies [MeV] Retarded time after bounce [s] DR, Burrows, et al 2017

23 Neutrino Light-Curves Time after bounce [s] Seadrow et al., in prep 2017

24 Neutrino Light-Curves Time after bounce [s] Seadrow et al., in prep 2017

25 Conclusions Detailed knowledge of neutrino-matter interaction fundamental to understand explosion mechanism Neutrinos from the next galactic supernova: a unique probe of the central engine Open issues: need accurate 3D models, oscillations

26 Conclusions Detailed knowledge of neutrino-matter interaction fundamental to understand explosion mechanism Neutrinos from the next galactic supernova: a unique probe of the central engine Open issues: need accurate 3D models, oscillations Thank you!