Presentation is loading. Please wait.

Presentation is loading. Please wait.

Observing Supernova Neutrinos to Late Times

Similar presentations


Presentation on theme: "Observing Supernova Neutrinos to Late Times"β€” Presentation transcript:

1 Observing Supernova Neutrinos to Late Times
Shirley Li The Ohio State University Collaborators: Luke Roberts, John Beacom TeVPA, August 2017

2 ? Timescale of a SN Detectable! 2/11 Shirley Li (OSU)
Figure credit: R.J. Hall 2/11

3 First input -- simulation
Luke Roberts Blondin et al., 2003 Shirley Li (OSU) 3/11

4 4/11

5 Late-time neutrinos are interesting!
Neutrino luminosity NS! 1/t behavior Transparency time Connects SN and NS Preliminary Late-time neutrinos are interesting! Shirley Li (OSU) 5/11

6 Late-time neutrinos are robust!
Neutrino energy Moderate mixing effect Preliminary Late-time neutrinos are robust! Shirley Li (OSU) 6/11

7 𝜈 𝑒 signal rate in Super-K
𝜈 𝑒 +𝑝→ 𝑒 + +𝑛 Inputs: 10 kpc SN 22.5 kton 3.5 MeV threshold Preliminary Plenty of events in Super-K! Shirley Li (OSU) 7/11

8 Other flavors Shirley Li (OSU) 8/11

9 Alternative outcome -- BH
Different mechanisms for BH formation Preliminary BH may form at late times Shirley Li (OSU) 9/11

10 Detecting BH formation
Detection significance of BH formation Preliminary We can detect BH formation at late times Shirley Li (OSU) 10/11

11 Conclusions Shirley Li (OSU) 11/11

12 Thank you!

13 Back up

14 Easily reconstruct neutrino spectrum
𝜈 𝑒 energy spectrum 𝜈 𝑒 +𝑝→ 𝑒 + +𝑛 𝐸 𝑒 + = 𝐸 𝜈 𝑒 βˆ’ 1.3 MeV --- known detection threshold Preliminary Easily reconstruct neutrino spectrum Shirley Li (OSU)

15 Plenty of events to late time in DUNE!
𝜈 𝑒 signal rate in DUNE 𝜈 𝑒 +40Arβ†’ 𝑒 βˆ’ +40 K βˆ— Inputs: 10 kpc SN 40 kton 5 MeV threshold Preliminary Plenty of events to late time in DUNE! Shirley Li (OSU)

16 Detection threshold needs to reach ~ 5 MeV
𝜈 𝑒 energy spectrum 𝜈 𝑒 +40Arβ†’ 𝑒 βˆ’ +40 K βˆ— 𝐸 𝑒 = 𝐸 𝜈 𝑒 βˆ’ 5.8 MeV --- unknown detection threshold Preliminary Detection threshold needs to reach ~ 5 MeV Shirley Li (OSU)

17 Non-negligible events at late time
𝜈 π‘₯ signal rate 𝜈 π‘₯ +𝑝→ 𝜈 π‘₯ +𝑝 Inputs: 10 kpc SN 22.5 kton 0.1, 0.2 MeV threshold Preliminary Non-negligible events at late time Shirley Li (OSU)

18 Detection threshold is crucial
𝜈 π‘₯ energy spectrum 𝜈 π‘₯ +𝑝→ 𝜈 π‘₯ +𝑝 𝐸 det β‰ͺ 𝐸 𝜈 π‘₯ --- unknown detection threshold Preliminary Detection threshold is crucial Shirley Li (OSU)


Download ppt "Observing Supernova Neutrinos to Late Times"

Similar presentations


Ads by Google