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Ultra-high Energy Neutrinos and Slow Jets of Core Collapse Supernovae

Ultra-high Energy Neutrinos and Slow Jets of Core Collapse Supernovae. Atsushi Watanabe (Harish-Chandra Research Institute). In collaboration with Raj Gandhi (HRI) Abhijit Samanta (HRI). 8 th Jan, 2009 @ NuHoRIzons, HRI, Allahabad. Cosmic neutrinos.

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Ultra-high Energy Neutrinos and Slow Jets of Core Collapse Supernovae

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  1. Ultra-high Energy Neutrinos and Slow Jets of Core Collapse Supernovae Atsushi Watanabe (Harish-Chandra Research Institute) In collaboration withRaj Gandhi (HRI) Abhijit Samanta (HRI) 8th Jan, 2009 @ NuHoRIzons, HRI, Allahabad

  2. Cosmic neutrinos ● Neutrinos are keys to go beyond the standard model • Masses, Mixings, CP violation • Flavor ratio on the earth ● Neutrinos can carry important information of astrophysical objects ● Cosmic ray sources

  3. What are its implications in high-energy neutrino observation ? Contents of talk ● The neutrino flux from charmed meson is important at high-energy range [Enberg, Reno, Sarcevic, 08’]

  4. Contents of talk • Active Galactic Nuclei (AGN) • Gamma Ray Burst (GRB) • Core collapse supernovae (Slow jets) [Halzen, 07’]

  5. Slow jet model of core collapse supernovae [Razzaque, Mesaros, Waxman, 05’] • Jetted SN hypothesis Supernovae ⇔ GRB Core collapse of massive stars resulting in a relativistic fireball jet which breaks through the stellar envelope is a widely discussed scenario for gamma ray burst production. Much more frequent than GRB

  6. Diffuse flux is small But point sources near our galaxy are feasible Slow jet model of core collapse supernovae SN rate in these is ～ 0.1 per year

  7. M82 3.2 Mpc +69° -25° 2.5 Mpc NGC253 Slow jet model of core collapse supernovae SN rate in these is ～ 0.1 per year Beam effect: 1/5

  8. Charmed mesons • Short lived - “prompt” The probability that pion and kaon interact with environment increase with increasing energy. Even a small fraction of short-lived particle Can give the dominant contribution at high energy. [Thunman, Ingelman, Gondolo, 95’]

  9. The jet co-moving frame and the earth frame Flux in jet-comving frame Flux in the earth frame Summing over fluences from all SNe (Star formation rate, jet fraction …) [Enberg, Reno, Sarcevic, 08’] We have chosen RMW pion flux as a basis to fix the flux scale Diffuse flux in the earth frame

  10. D-ERS pion-RMW Results (diffuse flux from D decay)

  11. Point sources (up-going muon events) D-ERS pion-RMW

  12. Point sources (down-going muon events) D-ERS D-ERS(electron)

  13. Summary and outlook • We have explored the slow jet supernovae model with charmed-meson neutrino flux. • It is found that the event rate is low for diffuse flux. • But the neutrinos form the point sources near our galaxy can be received by KM3 scale detector. ・ The event rate for the Glashow resonance is small.

  14. Summary and outlook ・Tau events ? “Double bang events” [Learned, Pakvasa, 94’] ・Other sources ( AGN, GRB …)

  15. Appendix Assuming that the jet duration is a few second, these agree well except the high-energy tail.

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