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Y2 Isochrones

The old page of Y2 can be accessed as well.

 

  • You can try out the Y2 version 3 !

  • Download the isochrone sets of Y2 version 3
    When downloaded, ungzipped and untared, an interpolation program together with the isochrones can be found.
    This is for interpolation in Y, [a/Fe], Z, and age.
  • Download the evolution track sets of Y2 version 3
    This gzipped tared file contains both of the base set and the wider Y set as well as an interpolation program.

     

  • The first announcement of the 3rd version has been; Yi, S. K., Kim, Y. -C., Demarque, P., Lee, Y. W., Han, S.-I. and Kim, D. G. `The Y2 Isochrones getting an extra dimension' (2008) The Art of Modelling Stars in the 21st Century, IAU Symposium 252, held 6-11 April 2008 at Sanya, China, 413 -- 416

     

  • The HB tracks (Han, S.-I. et al. 2009) will be on-line soon.

     

  • We acknowledge the significant contribution of C. Na, S. -I. Han, and D. G. Kim, to this 3rd version.

     

  • The 3rd version Y2 is consisted of 2 sets. The base set is for Y = dY/dZ * Z + Yp where dY/dZ = 1.5, 2.0, 2.5, and 3.0, with Yp=0.23
    Thus, the range of Y is narrower in lower Z. The extra set for wider range of Y is for Y = dY/dZ * Z + Yp where Yp = 0.23, 0.28, 0.33, 0.38, and 0.43, with dY/dZ=2.0

     

    The coverage of the base set The coverage of the extra set for wider range of Y
    Z [a/Fe]=0.0, [a/Fe]=0.3, [a/Fe]=0.6
    dY/dZ=1.5 dY/dZ=2.0 dY/dZ=2.5 dY/dZ=3.0
    0.00001 O O O O
    0.0001 O O O O
    0.0004 O O O O
    0.001 O O O O
    0.004 O O O O
    0.007 O O O O
    0.01 O O O O
    0.02 O O O O
    0.04 O O O O
    0.06   O O O
    0.08   O O O
    Z [a/Fe]=0.3
    Yp=0.23 Yp=0.28 Yp=0.33 Yp=0.38 Yp=0.43
    0.00001 O O O O O
    0.0001 O O O O O
    0.0004 O O O O O
    0.001 O O O O O
    0.004 O O O O O
    0.007 O O O O O
    0.01 O O O O O
    0.02 O O O O O
    0.04 O        
    0.06 O        
    0.08 O        
    Y = dY/dZ * Z + Yp, for Yp=0.23 Y = dY/dZ * Z + Yp, for dY/dZ=2.0

     

  • Summary of the input physics
    Grevesse and Noels Solar mixture
    OPAL EOS
    OPAL Rosseland mean Opacities and Ferguson Low temperature opacities
    Bahcall and Pinsonneault Energy generation rates
    Itoh et al. Neutrino loss rate
    Convective core overshoot ~0.2Hp
    Thoul et al. Helium diffusion
    Eddington grey Atmosphere

     

  • The EEP mapping scheme (Kim, D. G., 2005, MS thesis, Yonsei University)
    EEP mapping
    The 9 Primary EEPs are identified first, and then the secondary EEPs are set in between, in equal spacing.