1. p-process in SNIa: new perspectives R. Gallino C. Travaglio
Universita’ di Torino (Italy)
Osservatorio di Teramo-INAF
C. Travaglio
Observatorio di Torino (Italy)
F. Roepke, W. Hillebrandt
MPA Munich (Germany)
Computer resources

2. p-process 164Er missing 164Er 35 p-nuclei Routes to p-nuclei
p-nuclei in the
Solar System
164Er missing
p-process
164Er

3. p-process

4. p-process B2FH+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
‘p-process’ nuclei
They suggested temperature of the order of K, and timescale of s
p-process

5. p-process Audouze & Truran (1975)
T and r optimum conditions for the synthesis of p-nuclei in SNII explosions: K
H-rich matter in postshock supernova envelope following the passage of the shock wave, and realized that required T are not acquired there
Another possible site, novae associated with binary systems. In the accreted material T and r optimum conditions can be reached. Not sufficient matter can be produced in this site
p-process

6. Arnould (1976)
Synthesis of p-nuclei during hydrostatic oxygen burning
A large enhancement of heavy elements, presumably by prior s-processing is required. Only s-seed nuclei should be enhanced and not r-process seeds (recognized to be not important seeds).
p-process

7. p-process Woosley & Howard (1978)
They found that the (p,g) chain may require physical conditions that cannot be easily realized in nature. (p,g) and (p,n) play no role.
“One must still contend with disappointingly small synthesis of species like 92Mo, 94Mo, 96Ru, 98Ru”
Alternatively, they proposed g-process. A distribution of heavy elements subjected to a ‘hot photon bath’ ((g, n), (g, p), (g, a)) will be transformed on a timescale of 1s into a distribution of nuclei close to the solar distribution of p-nuclei
T optimum conditions for the synthesis of p-nuclei in explosive events: K
p-process

8. p-process 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
86Kr(p,g) … 90Zr(p,g)91Nb(p,g)92Mo
is responsible for half of 92Mo (and important for 90Zr as well) and (p,g) reactions produce also 96Ru. The other half of 92Mo, and 94Mo, come from (g,n) reaction sequence
p-process

9. p-process Goriely et al. (2002, 2005)
He accreting WD with sub-Chandrasekhar mass
p-process 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 78Kr) with respect to Fe
p-process

10. p-process 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
p-process

11. p-process Travaglio et al. (2011,ApJ in press)
F. Roepke & W.Hillebtandt
SNIa models
R. Gallino
s-process calculations
C. Travaglio
p-process nucleosynthesis
p-process

12. p-process Type Ia models: 2D We tested different SNIa models:
(simulation done by F. Roepke)
We tested different SNIa models:
pure deflagration
delayed detonation with different strenghts
p-process

13. Tracer particles in SNIa models
p-process

14. p-process s-process in accreted mass
“Accreting white dwarfs as an alternate or additional source of s-process isotopes” (Iben, ApJ 243, 1981)
p-process

15. p-process Distribution of tracers def dc3 ddt-st dd2d
dc3 = weaker del. det.
dd2d = stronger del. det.
def = deflagration
ddt-st = standard del. det.
def
dc3
ddt-st
p-process
dd2d

16. p-process s-process seeds
Preliminary s-process tests in a close binary system during the secondary companion MS/giant accreting on a WD (Travaglio et al. ’11)
p-process

17. p-process

18. p-nuclei versus peak T (1)
p-process

19. p-nuclei versus peak T (2)
p-process

20. p-process

21. p-process Results: solar metallicity DDT-a, Z2m2, 51200 tracers
56Fe=0.58

22. Stronger delayed detonation, 56Fe=0.98
Delayed detonation standard 56Fe=0.58
Deflagration 56Fe=0.33
Weaker delayed detonation 56Fe=0.33
Stronger delayed detonation, 56Fe=0.98

23. p-process Looking deeper into p-nuclei 113In, 115Sn, 138La, (180Ta)
DDT-a, Z2m2,
51200 tracers
56Fe=0.58
113In, 115Sn, 138La, (180Ta)
152Gd, 164Er

24. p-process Looking deeper into p-nuclei
113In, 115Sn are p-only isotopes?
r-process contribution (Dillmann et al. 2008, Nemeth et al. 1994)?
138La produced by neutrino-nuclei interaction
(Woosley et al. 1990)
152Gd and 164Er large s-process contributions
75% - 80% at solar composition, with 10% of errorbar
(Arlandini et al. 1999, Kaeppeler et al. 2011)
p-process

25. p-process Long-lived p-nuclei (Dauphas et al. 2002) 92Nb/92Mo
2.8 ± 0.5 × meteorite
1.5 ± 0.6 × production in SNe
1.3 x our model
146Sm/144Sm
7.6 ± 1.3 × meteorite
1.8 ± 0.6 × production in SN
3.2 x our model
p-process

26. sp-nach
Travaglio et al. (2011)
p-process

27. 96Zr
80Kr
90Zr
86Sr
p-process
DDT-a, Z2m2,
51200 tracers
56Fe=0.58

28. 96Zr
p-process
DEF, Z2m2,
51200 tracers
56Fe=0.33

29. behave with metallicity? (Travaglio et al., in prep.)
How do p-nuclei
behave with metallicity?
(Travaglio et al., in prep.)
p-process

30. (Travaglio et al., in prep.)
Taking a fixed choice of the 13C-pocket at different Z, we may infer that the (p/56Fe)/(p/56Fe)sun ratio is always constant. This suggests a primary nature of p-process
(Travaglio et al., in prep.)
p-process

31. p-process Chemical evolution
From the hypothesis that SNIa are responsible for 2/3 of the solar 56Fe, 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 50% of the all p-nuclei.
If we take an average between DDTw-a and DDTs-a models, considering that they represent 10% of all SNIa, they account for 75% of all p-nuclei.
p-process

32. WKP
p-process at various metallicities and chemical evolution (Travaglio et al. in prep.)
Nucleosynthesis in accreted mass
(tbd)
p-process
SNIa in 3D and sub-Chandrasekhar models
(Roepke et al. at MPA)

33. p-process

34. Low Mass Stars. Evolution and Nucleosynthesis- I
Roberto Gallino
University of Torino
Dipartimento di Fisica Generale, Italy
GRADUATE SCHOOL IN ASTRONOMY XV
Monday 18th October, 2010

35. p-process

36. p-process p-process Wanajo,Janka, Kubono, ApJ 2010
Thielemann et al., 2010
Roberts,Woosley, Hoffman, ApJS 2011
p-process