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

8th Jan, 2009 @ NuHoRIzons, HRI, Allahabad

Atsushi Watanabe(Harish-Chandra Research Institute)

In collaboration with Raj Gandhi (HRI) Abhijit Samanta (HRI)

Cosmic neutrinos Cosmic neutrinos

• Masses, Mixings, CP violation• Flavor ratio on the earth

● Neutrinos are keys to go beyond the standard model

● Neutrinos can carry important information of astrophysical objects

● Cosmic ray sources

Contents of talkContents of talk

● The neutrino flux from charmed meson is important at high-energy range

[Enberg, Reno, Sarcevic, 08’]

What are its implications in high-energy neutrino observation ?

Contents of talkContents of talk

• Active Galactic Nuclei (AGN)• Gamma Ray Burst (GRB)• Core collapse supernovae (Slow jets)

[Halzen, 07’]

Slow jet model of core collapse supernovaeSlow 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 jetwhich breaks through the stellar envelope is a widely discussed scenario for gamma ray burst production.

Much more frequent than GRB

Slow jet model of core collapse supernovaeSlow jet model of core collapse supernovae

• Diffuse flux is small• But point sources near

our galaxy are feasible

SN rate in these is ～ 0.1 per year

M82

NGC253

3.2 Mpc

2.5 Mpc

-25°

+69°

Slow jet model of core collapse supernovaeSlow jet model of core collapse supernovae

SN rate in these is ～ 0.1 per yearBeam effect: 1/5

Charmed mesonsCharmed 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’]

The jet co-moving frame and the earth frameThe jet co-moving frame and the earth frame

[Enberg, Reno, Sarcevic, 08’]

Flux in jet-comving frame

Flux in the earth frame

Diffuse flux in the earth frame

We have chosen RMW pion flux as a basis to fix the flux scale

Summing over fluencesfrom all SNe(Star formation rate, jet fraction …)

pion-RMW

Results (diffuse flux from D decay)Results (diffuse flux from D decay)

D-ERS

Point sources (up-going muon events)Point sources (up-going muon events)

pion-RMW

D-ERS

Point sources (down-going muon events)Point sources (down-going muon events)

D-ERS

D-ERS(electron)

Summary and outlookSummary 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.

Summary and outlookSummary and outlook

・ Tau events ?

・ Other sources ( AGN, GRB …)

“Double bang events”

[Learned, Pakvasa, 94’]

AppendixAppendix

Assuming that the jet durationis a few second, these agree wellexcept the high-energy tail.