Alessandro Chieffi

(Istituto di Astrofisica Spaziale e Fisica Cosmica & INAF)

Email: achieffi@rm.iasf.cnr.it

25 MO

1 MO

5 MO

REMEMBER that:

The interplay between the evolution of a star and the nuclear processes occurs through the RATES and NOT the cross sections:

Rlk => Xl x Xk

x screening x <v>lk

25 MO

5 MO

1 MO

PP chain

CNO cycle

CNO cycle

14N(p,)15O

p(p,e+)d

t(H-burn)= - 0.3%

t(H-burn)= - 4%M(He) => 0.91 to 0.97 MO

M(He) => 8.3 to 8.6 MO

<v>3 x 10 is NOT appreciablex 10

t(H-burn)= - 3%

MS

TORGB

HB

10 Gyr

Z=10-4

Y=0.23

Dashed => (14N(p,)15O) / 2

13 Gyr

Solid => reference

M=0.8 MO

Y=0.23

Z=10-4

MHe = 1%

Mbol(tip) = 0.055 Mag

Red – reference

Blue – 14N(p,)15O / 2

-0.04 Mag => - 0.6 Gyr

COcore

H-rich mantle

He burning shell

He (+C) intershell

H burning shell

AGB phase

R(Hshell) ~10-5 Rstar

0.7 < M / MO < 7

Neutron production

s process nucleosynthesis

Convective envelope

He shell

H shell

t(yr)

M(MO)

Convective envelope

He shell

H shell

t(yr)

M(MO)

He conv. shell

-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.)

He luminosity

M=3 MO 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

Lo

g10

(PF

)

Element

Lo

g10

(PF

)

Stable Isotopes

Reference

3 / 23 x 2

M=3 MO - Z=0.02

14Np

Reference

3 / 23 x 2

14Np

SURFACE CARBON ABUNDANCE

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

Roadmap...

1) WR stars: evolution & explosive nucleosynthesis

35

120

2) Intermediate Mass Stars: elemental yields