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Alessandro Chieffi (Istituto di Astrofisica Spaziale e Fisica Cosmica & INAF)

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Presentation on theme: "Alessandro Chieffi (Istituto di Astrofisica Spaziale e Fisica Cosmica & INAF)"— Presentation transcript:

1 Alessandro Chieffi (Istituto di Astrofisica Spaziale e Fisica Cosmica & INAF) Email: achieffi@rm.iasf.cnr.it

2 25 M O 1 M O 5 M O

3 REMEMBER that: The interplay between the evolution of a star and the nuclear processes occurs through the RATES and NOT the cross sections: R lk => X l x X k x screening x lk

4 25 M O 5 M O 1 M O PP chain CNO cycle 14 N(p, ) 15 O p(p,e + )d t(H-burn)= - 0.3% t(H-burn)= - 4% M(He) => 0.91 to 0.97 M O M(He) => 8.3 to 8.6 M O 3 x 10 is NOT appreciable x 10 t(H-burn)= - 3%

5 MS TO RGB HB

6 10 Gyr Z=10 -4 Y=0.23 Dashed => ( 14 N(p, ) 15 O) / 2 13 Gyr Solid => reference

7 M=0.8 M O Y=0.23 Z=10 -4 M He = 1% M bol (tip) = 0.055 Mag Red – reference Blue – 14 N(p, ) 15 O / 2 -0.04 Mag => - 0.6 Gyr

8 CO core H-rich mantle He burning shell He (+C) intershell H burning shell AGB phase R(H shell ) ~10 -5 R star 0.7 < M / M O < 7 Neutron production s process nucleosynthesis

9 Convective envelope He shell H shell t(yr) M(M O )

10 Convective envelope He shell H shell t(yr) M(M O ) He conv. shell

11 -3 8.1 6.5 -1 8.5 7.5 Base conv. env. H burn. shell He burn. shell Log(Surf. C abund.) Log(Tmax He shell) Log(T base conv. Env.)

12 He luminosity

13 M=3 M O Z=0.02 Y=0.284 Neutron captures on: Fe Kr84 – Rb – Sr – Y – Zr92 Xe132 – Cs – Ba – La – Ce – Pr – Nd144 Hg202 – Tl – Pb – Bi209 Network: H to Si (full) + 92 nuclei

14 Log 10 (PF) Element

15 Log 10 (PF) Stable Isotopes

16 Reference 3 / 2 3 x 2 M=3 M O - Z=0.02 14 Np

17 Reference 3 / 2 3 x 2 14 Np SURFACE CARBON ABUNDANCE

18 The mother of all rates: 12 C(, ) 16 O

19 Roadmap... 1) WR stars: evolution & explosive nucleosynthesis 35 120 2) Intermediate Mass Stars: elemental yields

20


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