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Origin of the elements Which reactions Which physical conditions Which astrophysical sites

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Origin of the elements Which reactions Which physical conditions Which astrophysical sites Which quantities Yields depend on reaction rates , M , Z, treatment of convection, Mass loss , V rot , B magn , Interactions in close binaries , Explosion mechanism

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Presentation Transcript
slide1

Origin of the elements

  • Whichreactions
  • Whichphysical conditions
  • Whichastrophysical sites
  • Whichquantities
  • Yieldsdepend on
  • reactionrates,
  • M,
  • Z,
  • treatmentof convection,
  • Mass loss,
  • Vrot,
  • Bmagn,
  • Interactions in close binaries,
  • Explosion mechanism
  • Explosive nucleosynthesis
  • 1D-3D models

Evolution of stellarsystems

Part of historyhiddenin the abundances of the elements.

Nomoto et al. 2013 (ARAA)

slide2

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
  • composedfromISMenriched by one or
  • twonucleosyntheticevents 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)

slide3

STRIKING OBSERVATIONAL FACTS (EMP STARS)

1) Scatter: different according to the elements considered

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

Observations:

Cayrel et al. 2004

Spite et al 2005

Israelian et al. 2004, Centurion et al 2003

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

slide4

IN THE HALO TWO KINDS OF CHEMICALLY PECULIAR STARS

IN THE FIELD

IN GLOBULAR CLUSTERS

Gratton et al. 2004

Norris et al 97

Large scatter

STARS MADE OF

H-burningproducts

H- and He-burningproducts

slide5

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

Z=0.00001

Z=0.00050

Slow wind: YSG

enriched in

H- and He-burning

products

Slow wind: MS

Onlyenriched in

H-burning

products

slide9

Netal06

V=0, Hetal05

V=300, Hetal05

WW95

CL04

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