in SNIa with multi-d models: their role in Galactic chemical evolution C. Travaglio INAF Observatory of Turin (Italy) R. Gallino University of Turin (Italy) F. Rӧpke, W. Hillebrandt Uni-Würzburg, MPA Munich (Germany) Computer resources
The team F. Roepke & W.Hillebtandt SNIa models R. Gallino s-process seeds C. Travaglio nucleosynthesis Travaglio et al. 2011, ApJ 739,93
in SNIa: historical overview B2FH+Cameron (1957) Howard, Meyer, Woosley (1991) Travaglio, Rӧpke, Gallino, Hillebrandt (2011) Goriely et al. (2002, 2005) Kusakabe, Iwamoto, Nomoto (2011)
B 2 FH+Cameron (1957) H-rich layers of SNII (p,g) and (g,n) reactions operating on preexisting s- and r-seed nuclei Cameron called them excluded isotopes Because of the dominant role of played by proton reactions, named these nuclei They suggested temperature of the order of 2.5 10 9 K, and timescale of 10-100 s
Howard, Meyer & Woosley (1991) A new site for the gamma-process: Type Ia supernovae. CO-WD that explodes by deflagration or detonation. They investigate chains to produce the light-p, and found that 86 Kr(p,g) 90 Zr(p,g) 91 Nb(p,g) 92 Mo is responsible for half of 92 Mo (and important for 90 Zr as well) and (p,g) reactions produce also 96 Ru. The other half of 92 Mo, and 94 Mo, come from (g,n) reaction sequence
Goriely et al. (2002, 2005) He accreting WD with sub- Chandrasekhar mass are produced in the accreting He-layers Tested different initial abundances of s-nuclei, up to 100xsolar They found that most of the p- nuclei are coproduced at level close to solar, but underproduced (except 78 Kr) with respect to Fe
Kusakabe,Iwamoto & Nomoto (2011) They used as SNIa model the W7 (Nomoto et al. 84), pure deflagration They also examine the impact of different s-seed distributions
s-process in accreted mass Accreting white dwarfs as an alternate or additional source of s-process isotopes (Iben, ApJ 243, 1981)
p-nuclei versus peak T
Results: solar metallicity (Travaglio et al. 2011) DDT-a, Z2m2, 51200 tracers 56 Fe=0.58 M
Looking deeper into p 113 In, 115 Sn, 138 La, 152 Gd 164 Er, 180 Ta DDT-a, Z2m2, 51200 tracers 56 Fe=0.58 M
Looking deeper into p-nuclei 113 In, 115 Sn are p-only isotopes? r-process contribution (Dillmann et al. 2008, Nemeth et al. 1994)? 138 La produced by neutrino (Woosley et al. 1990) 152 Gd and 164 Er large s-process contribution at solar composition (Arlandini et al. 1999, Kaeppeler et al. 2011) 180 Ta at least 50% contribution from s-process at solar composition (Mohr et al. 2007)
Comparing rates: Basel and JINA
Looking deeper into p: 94 Mo mistery 95 Mo(ɣ,n) 94 Mo 94 Mo(ɣ,n) 93 Mo
94 Mo mistery: one possibility to solve it
New improvements to solve 94 Mo mistery A New Proposal to the High Intensity Gamma-Ray Source (HIγS2) PAC-12 (Duke University, North Carolina, USA) Cross Section Measurements for 94 Mo(γ,n) 93 Mo Key Photonuclear Reaction for Understanding the Origin of p-nuclei A. Banu (Spokesperson), B. Glassman, D. Votaw James Madison University, Department of Physics and Astronomy, Harrisonburg, VA 22801, USA C. Travaglio INAF Astrophysical Observatory Turin, Italy B2FH Association Turin, Italy
s-seeds behaviour with metallicity (Travaglio et al. 2013, in prep)
We obtain an important p- contribution (of 60%) to 144 Sm and 196 Hg using the 208 Pb s- enhanced seed. Also 168 Yb, 174 Hf, and 190 Pt get a substantial contribution (about 25% 30%) this way. No important contribution derives on the light p-nuclei Results: p-products at different metallicities (Travaglio et al. 2013, in prep.)
Chemical evolution (Travaglio et al. 2011) From the hypothesis that SNIa are responsible for 2/3 of the solar 56 Fe, and assuming that our DDT-a model represents the typical SNIa with a frequency of 70% (Li et al. 2010), we conclude that they can be responsible for about at least 50% of the all p- nuclei.
Chemical evolution (chemical evolution code from Travaglio et al. 04)
in SNIa with 3D models (Seitenzahl et al. 2013, MNRAS, 429, 1156) Travaglio et al. 2013: in preparation. Production of p-nuclei at different metallicities and the role of SNIa in p- process Galactic chemical evolution