1. The synthesis of 26 Al, 60 Fe and 44 Ti in massive stars and their current inventory in our Galaxy Alessandro Chieffi Istituto Nazionale di AstroFisica (Istituto di Astrofisica e Planetologia Spaziale) & Centre for Stellar and Planetary Astrophysics – Monash University - Australia Email: alessandro.chieffi@iaps.inaf.it In collaboration with Marco Limongi Dust in EuroGENESIS environments: from primitive, massive stars to novae Perugia (Italy), November 11-14, 2012

2. Na22 2.6 Yr 2.842 MeV Ti44 63 Yr 0.268 MeV Sc44 3.9 h 3.653 MeV Ni56 5.9 d 2.135 MeV Co56 77 d 4.566 MeV Co57 271 d 0.836 MeV

5. Between 1979 and 2001 several experiments were carried out: Kretschmer et al. AA 412,47 (2003) HEAO3 SMM GRIS CGRO R. DIEHL Clemson 2005 Astronomy with Radioactivities V

6. On the basis of just the integrated flux towards the galactic center, the various 26 Al sources are: Type II Supernovae WR stars Novae Intermediate mass stars Confined in the spiral arms of our Galaxy Confined within the disk of our Galaxy 10<M<30 30<M<120 1-3<M<7

7. Kretschmer et al. AA 412,47 (2003) Plüschke et al. AIP Conf. Proc. 510 ed. M.L. McConnell & J.M. Ryan p 35-39 (2000)) 1.809 MeV All Sky Map CGRO

8. The 53 GhZ free-free all-sky map marks the regions of ionized matter. A strong ionizing flux (l<912 A) is necessary to mantain matter ionized (otherwise it would recombine in 1 Myr) Only stars more massive than, say, 15 M O do produce a strong ionizing flux hence The correlation between the 53 GhZ free-free and the 1.809 MeV maps implies that they share the same spatial distribution and therefore that 26 Al and ionizing photons are produced by the same stars Knodelseder (1999 - ApJ 510, 915) found also that the scaling between the two fluxes is CONSTANT towards all longitudes and equal to: i.e. 26 Al mainly produced by stars more massive than 15 M O Y 26 Al = 10 -4 M O per O7 V (Log(Q o )=49.05) R GxL = 1.25 10 -11  1.8MeV /  <912A

9. RHESSI and INTEGRAL launched in 2002 INTErnational Gamma-Ray Astrophysics Laboratory Reuven Ramaty High Energy Solar Spectroscopic Imager 60 Fe/ 26 Al RHESSI 0.17± 0.05 INTEGRAL 0.14± 0.03 Diehl et al. (2006 – Nature 439,5) R. DIEHL Clemson 2005 Astronomy with Radioactivities V R. DIEHL Clemson 2005 Astronomy with Radioactivities V

10. Summary of the observational facts: 1) 26 Al is very probably produced by stars having M>15 M O 2) There are roughly 1.25 10 -11  1.8MeV per ionizing photon at all longitudes 3) The 60 Fe/ 26 Al flux ratio is of the order of 0.14 ± 0.05 towards the Galactic center 4) Roughly 2.8 M O of 26 Al are present in the Galaxy (± 30%)

11. The theoretical interpretation is based on our database of evolutions of massive stars: Limongi and Chieffi (2006 – ApJ 647, 483) FRANEC (release 5.050419) O.R.F.E.O. Online Repository for the Franec Evolutionary Output WEBPAGE: http://orfeo.iasf-roma.inaf.it WARNING: though the ground and the metastable 26 Al states are properly taken into account, for simplicity in the following I’ll simply refer to the total 26 Al

12. 26 Al production: 1) H convective core H rich mantle Central H burning 2) C (Ne/C) conv. shell (when the star is in shell Si burning) 3) Explosive Ne burning He burning shell C convective shell CO core Si burning shell He core Fe Shock wave

13. 26 Al 25 Mg 24 Mg 28 Si 26 Mg 27 Al 29 Si P N 26 Al production in central H burning The 25 Mg is the initial one (usually scaled solar) H rich mantle Central H burning

14. 26 Al production in the C (Ne/C) convective shell 26 Al 25 Mg 24 Mg 28 Si 26 Mg 27 Al 29 Si P N X M preserved produced 22 Ne, 12 C 26 Al C profile CO core He core Fe DESTRUCTION: 12 C( 12 C,  ) 20 Ne 12 C( 12 C,p) 23 Na( ,p) 26 Mg (CNO) INI  14 N( ,  ) 18 F(  + ) 18 O( ,  ) 22 Ne( ,n) 25 Mg

15. 26 Al production in C (Ne/C) convective shell

16. 26 Al production by the explosive Ne burning 26 Al 25 Mg 24 Mg 28 Si 26 Mg 27 Al 29 Si P N 23 Na (n,p) The synthesis of 26 Al occurs in the region where the peak temperature drops to T peak  2.2 10 9 K CO core He core Fe Shock wave T1T1 T2T2 r1r1 r2r2 Fe core ignition

17. Total 26 Al yield as a function of the initial mass H-burnC(C/Ne) shellExplosive Ne burn. Semi secondary origin Primary origin

18. Diehl et al. (2006 – Nature 439,5)

19. The galactic R GxL The galactic 26 Al By adopting: m up’ =11M O – M top = 120M O a Galactic Lyman continuum Luminosity Q GAL = 3.5 10 53 photons/s

20. The galactic 26 Al By adopting: m up’ =11M O – M SN I I =35M O – M top = 120M O a Galactic Lyman continuum Luminosity Q GAL = 3.5 10 53 photons/s Steady state

21.  2 Velorum Binary system containing the closest WR(11) star Main data taken from Schaerer et al. (1997) and Oberlack et al. (2000) Distance: 258 pc - WC8 (9 M O ) - O8.5III (29 M O ) 26 Al(Upper limit) => 6.3 10 -5 (+2.1-1.4) M O

22.  2 Velorum Binary system containing the closest WR(11) star Main data taken from Schaerer et al. (1997) and Oberlack et al. (2000) Distance: 258 pc - WC8 (9 M O ) - O8.5III (29 M O ) 26 Al(Upper limit) => 6.3 10 -5 (+2.1-1.4) M O

23. 60 Fe 57 Fe 56 Fe 60 Ni 58 Fe 59 Co 61 Ni 59 Fe 44 d P N 60 Fe production: 1) basics 58 Ni 62 Ni Central He burning T < 3.5 10 8 K 22 Ne( ,n) 25 Mg  < 10 7 n/cm 3 Central C burning Main n donor  = few 10 7 n/cm 3 Shell He burning T > 4 10 8 K  => 6 10 10 to 10 12 n/cm 3  crit = 10 10 n/cm 3  crit = 3 10 11 n/cm 3 Shell C burning T > 1.3 10 9 K  => 6 10 11 to 2 10 12 n/cm 3 Shell Ne burning T > 1.8 10 9 K  => 6 10 11 to 2 10 12 n/cm 3 T < 10 9 K

24. 60 Fe production: 2) the He and C convective shells X M preserved produced 22 Ne, 12 C 60 Fe He/C

25. 60 Fe production: 3) the Ne explosive contribution

26. The total 60 Fe production M < 60 M O Mainly produced by the C convective shell M > 60 M O Mainly produced by the C convective shell (Ledoux criterion) M > 60 M O Mainly produced by the He convective shell (Schwarz. criterion)

27. The galactic 60 Fe/ 26 Al flux ratio The 60 Fe/ 26 Al flux ratio is of the order of 0.14 ± 0.03 towards the Galactic center

29. Summary & Conclusions Observational:  26 Al is very probably produced by stars having M>15 M O  There are roughly 1.25 10 -11 n(  1.8MeV )/ (ionizing photon) at all longitudes  The 60 Fe/ 26 Al flux ratio is of the order of 0.14 ± 0.05 towards the Galactic center  Roughly 2.8 M O of 26 Al are present in the Galaxy (± 30%) Theoretical:  26 Al is mainly produced by the Ne explosive burning.  60 Fe is mainly produced by the C convective shell.  The observed (and quite constant) average number of  1.8MeV per ionizing photon (R GxL ) is rather well reproduced by our models.  The observed 60 Fe/ 26 Al flux ratio towards the center of our Galaxy is well reproduced if the Langer (1989) mass loss rate in the WNE,WCO is adopted.  Our predictions for  2 Velorum are in agreement with the quoted upper limit and hence the longstanding discrepancy between the data and the predictions is removed.

30. M( 44 Ti)=1.6 10 -4 M O M( 44 Ti)= 3 10 -5 M O Cas A as seen by IBIS – ISGRI aboard INTEGRAL at 25 - 40 KeV Observed: Predicted: Distance 3 Kpc -- 335 yr old -- M ini 30 M O M end 16 M O 3 lines : 67.9 KeV, 78.4 KeV, 1.157 MeV  ( 44 Ti ) = 59.8 yr

31. 44 Ti Not produced in a normal freeze out Critical phase Produced in the  -rich freeze-out of zones exposed to the complete explosive Si burning ( 3   C( ,  ) 16 O( ,  )...NSE )  cooling <<  build up  cooling >>  build up

32. 42 Ca 43 Ca 44 Ca 46 Ca 48 Ca 40 Ca 45 Sc 48 Ti 47 Ti 46 Ti 44 Ti 49 Ti 50 Ti 50 V 51 V 50 Cr 52 Cr 53 Cr 54 Cr 55 Mn 44 Ti Produced in the  -rich freeze-out of zones exposed to the complete explosive Si burning 40 Ca( ,  ) 44 Ti 43 Sc(p,  ) 44 Ti 41 Ca(  n) 44 Ti 44 Sc(p,n) 44 Ti 44 Ti( ,p) 47 V

34. 26 Al 25 Mg 24 Mg 28 Si 26 Mg 27 Al 29 Si P N 26 Al production in central H burning: 1) basics

35. 26 Al production by the explosive Ne burning: 1) basics 26 Al 25 Mg 24 Mg 28 Si 26 Mg 27 Al 29 Si P N 23 Na (n,p) 26 Al(n,p) CA88 26 Al(n,a) NACRE

36. 26 Al production in central H burning: 3) uncertainties 2) the 25 Mg(p,  ) 26 Al cross section 3) the convective core size 1) the initial 25 Mg abundance many...., but we tested the following:

37. 26 Al production in central H burning: 3) uncertainties 1) the initial 25 Mg abundance 60 M O STD 6.94 10 -5 25 Mg INI *2 1.39 10 -4 2) the 25 Mg(p,  ) 26 Al cross section 3) the convective core size (0.3 Hp ) 60 M O STD 6.94 10 -5 M O 0.5 H P 5.98 10 -5 M O 120 M O STD 2.82 10 -4 M O 0.5 H P 3.50 10 -4 M O

38. 26 Al production by the explosive Ne burning: 4) uncertainties 26 Al 25 Mg 24 Mg 28 Si 26 Mg 27 Al 29 Si P N 23 Na 26 Mg( ,n) 29 Si 24 Mg(n,  ) 25 Mg 25 Mg( ,n) 28 Si 16 O(n,  ) 17 O 21 Ne( ,n) 24 Mg 20 Ne(n,  ) 21 Ne 28 Al(p,n) 28 Si 26 Al(n,p) 26 Mg 29 Si( ,n) 32 S 26 Al(n,  ) 23 Na 20 Ne( ,p) 23 Na 26 Mg(p,  ) 27 Al 24 Mg( ,p) 27 Al 20 Ne(p,  ) 21 Na 27 Al( ,p) 30 Si 24 Mg(p,  ) 25 Al 23 Na( ,p) 26 Mg 28 Al(p,n) 28 Si 27 Al(p,  ) 28 Si 25 Mg(p,  ) 26 Al 30 Si(p,  ) 31 P (n,p) 20 Ne( ,  ) 16 O 20 Ne( ,  ) 24 Mg 20 Ne( ,p) 23 Na 24 Mg( ,p) 27 Al test25 M O totalexplosive60M O totalexplosive Reference8.61 10 -5 25.2 10 -5 26 Al(n,p) x 2 26 Al(n,  ) x 2 6.63 10 -5 -23%-39%19.8 10 -5 -21%-50% 24 Mg(n,  ) x 2 11.5 10 -5 +33%+57%33 10 -5 +31%+60% 25 Mg(p,  ) x 2 11.7 10 -5 +33%+57%