New Frontiers in Nuclear and Particle Astrophysics: Time varying quarks MHD Jets Neutrino Mass Hierarchy G. J. Mathews – UND OMEG5-I Nov. 18, 2011 NAOJ, Mitaka, Tokyo

R-PROCESS NUCLEOSYNTHESIS IN THE MHD+NEUTRINO-PAIR HEATED COLLAPSAR JET

Neutrino-Heated Relativistic MHD Jet Tracer particles undergo high entropy r-process

R-Process in the jet

Why is Y e so low then so high? Neutronized accretion- disk material

Later in the Jet e + p  n + e + e + n  p + e - Y e ~ [1 + (  e/  e ) 2 ] -1 _ Absorbed/ Lower Temperature

Analogous to neutrino driven SN wind High Density Environment e + n  p + e -

Evidence for an inverted neutrino hierarchy from neutrino nucleosynthesis in core collapse supernovae, meteorites and new measurements of the θ 13 neutrino mixing angle G. J. Mathews,T. Kajino, W. Aoki,W. Fujiya, J. B. Pitts, 2011, Submitted

Neutrinos Can Change Flavor => Neutrinos have mass and mix

Neutrino Flavor vs Mass Eigenstates

Mass Hierarchy?

T2K Collaboration

Neutrino Nucleosynthesis in Core Collapse Supernovae ν ν ν ν ν

Neutrinos in Supernovae Neutrino Luminosity ~10 53 erg/sec Woosley, Wilson, GJM, Hoffman, Meyers (1994)

Neutrino Energies are high enough to induce nucleon emission reactions

The ν-Process Woosley, Hartmann, Hoffman, Haxton (1990) Cross Section is very small ~ cm 2, Only rare isotopes are affected: 7 Li, 11 B, 19 F, 138 La, 180 Ta

Neutrino reactions to produce 7 Li and 11 B 7 Li, 7 Be 11 B

Where do the neutrino reactions occur?

7 Li and 11 B are produced in the He/C Shell

Neutrinos interact as they pass through the outer layers

As Neutrinos Pass through the Supernova they can Oscillate

Resonance Density => neutrinos convert in O shell

Transition probabilities Normal Inverted Strong ν μτ => ν e mixing in O shell

Effects of mixing Mixing in O shell affects neutrino spectrum in outer He/C shell => 7 Li, 11 B affected – ( 138 La, 180 Ta unaffected) Normal hierarchy - Inverted hierarchy -

Sensitivity of 7 Li/ 11 /B ratio to θ 13 requirement

What is the lower limit to sin 2 (θ 13 )? T2K

Problem Isotopic Li/B exceedingly difficult to measure in a SN remnant Even if measured, would be difficult to distinguish the ν-process contribution from surface contamination Need a sample direct from ejected He/C shell

Murchison Meteorite Ca-Al rich Inclusions Primitive Solar System Material

SiC grains

Nyugen (2005) X grains ~1% of SiC grains

Composition of SiC grains SiC X grains exhibit 12 C/ 13 C > Solar, 14 N/ 15 N < Solar, Enhanced 28 Si, Decay of 26 Al (t 1/2 = 7x10 5 yr) and 44 Ti (t 1/2 = 60 yr) => origin in Core Collapse Supernovae

Out of 1000 SiC grains from a 30 g sample of the Murchison CM2 chondrite, 7 X grains show resolvable anomalies in Li and/or B. => 7 Li/ 11 B > upper limit

Preference for inverted hierarchy 2 σ 3 σ

Baysian Analysis Let O be the observed isotopic ratio hierarch, I be the theory that the mass hierarchy is inverted, and N be that the mass hierarchy is normal P(I|O) = P(I) P(O|I) / P(O) = P(I) P(O|I) / { P(I) P(O|I) + [1-P(I)] P(O|N) } = (P(I) * 1/60) / { P(I) * 1/60 + [1-P(I)] * 1/190 }. P(I|O) ≈ 3 P(I) / [1 + 2 P(I)}. If it were a 50/50 probability for inverted hierarchy before, then 75% probability that the hierarchy is inverted afterward. If no oscillations an equal possibility, then If you were 33% sure before, you'd be 60% sure afterwards

Conclusions SiC X grains enriched in ν-process material have the potential to solve the neutrino mass hierarchy problem for finite θ 13. An analysis of only 7 grains indicates that the inverted hierarchy is preferred over normal hierarchy by 75/25. An analysis of even a few more grains could provide a detection of ν-process 7 Li and substantially improve these limits.

Neutrino Flavor vs Mass Eigenstates

Composition of SiC grains SiC X grains exhibit 12 C/ 13 C > Solar, 14 N/ 15 N < Solar, enhanced 28 Si, Decay of 26 Al (t 1/2 = 7x10 5 yr) and 44 Ti (t 1/2 = 60 yr) => origin in Core Collapse Supernovae Mainstream SiC grains have – 12 C/ 13 C or ~Solar => origin in AGB stars (Hoppe et al. 1994).