Origin of the elements

Which reactions Which physical conditions Which astrophysical sites Which quantities

Yields depend onreaction rates,

M, Z,

treatment of convection,Mass loss,

Vrot, Bmagn,

Interactions in close binaries, Explosion mechanism

Explosive nucleosynthesis

1D-3D models

Nomoto et al. 2013 (ARAA)

Evolution of stellar systems

Part of history hidden in the abundances of the elements.

How to constrain the yields?

INDVIDUAL STARS

Check of in situ processes (WR) Composition of the ejecta of Supernovae Asteroseismology Unaltered surface composition of stars composed from ISM enriched by one or two nucleosynthetic events or a restricted mass range of stars like EMP halo stars, CEMP stars General properties of stars

COLLECTIVE EFFECTS

ISM abundances (in primordial galaxies)

Nomoto et al. 2013 (ARAA)

STRIKING OBSERVATIONAL FACTS (EMP STARS)

1) Scatter: different according to the elements considered

Cayrel et al. 2004

2) No sign of Pair Instability Supernovae

3) Important amount of primary nitrogen

4) More carbon, less oxygen produced at low Z ?

5) CEMP, CRUMP (no, r, s, r and s)

6) The O-Na, Mg-Al anticorrelation in globular cluster stars

7) Helium-rich stars in globular clusters

Israelian et al. 2004, Centurion et al 2003

Spite et al 2005 Norris et al 1997

Mc William et al 95; Barbuy et al. 96; Christlieb et al. 04; Frebel et al. 05; Plez & Cohen 05

Gratton et al 2004; Piotto et al 2005

Observations:

IN THE FIELD IN GLOBULAR CLUSTERS

IN THE HALO TWO KINDS OF CHEMICALLY PECULIAR STARS

STARS MADE OF

H- and He-burning productsH-burning products

Norris et al 97Gratton et al. 2004

Large scatter

SAME MASS: 60 Msol, SAME Vini=800 km s-1

Z=0.00050 Z=0.00001

Slow wind: MSOnly enriched in

H-burningproducts

Slow wind: YSGenriched in

H- and He-burningproducts

WW95

CL04

Netal06

V=0, Hetal05

V=300, Hetal05