changa/html/starlifetime_8h_source.html

#ifndef STARTIME_H_INCLUDED

#define STARTIME_H_INCLUDED

/*

  Uses Raiteri, Villata, and Navarro (A&A, 315, 105, 1996) fit to

  Padova group stellar models to find stellar lifetimes as a

  function of mass, M,and metallicity, Z.


  log t = a0(Z) + a1(Z)*log(M) + a2(Z)*(log(M))**2


  where t is stellar lifetime in years, M is stellar mass

  in solar masses, and Z, defined as the total mass fracion in

  elements heavier than He, is in the range 0.0004-0.05.

  Coefficients are given as follows:


  a0(Z) = 10.13 + 0.07547*log(Z) - 0.008084*(log(Z))**2


  a1(Z) = -4.424 + 0.7939*log(Z) - 0.1187*(log(Z))**2


  a2(Z) = 1.262 + 0.3385*log(Z) - 0.1187*(log(Z))**2


  zmin, zmax = minimum and maximum metallicity in stellar lifetimes equation

  zsol = solar metal abundance

  xoxsol = solar oxygen abundance */


class Padova {

    double a00, a01, a02;

    double a10, a11, a12;

    double a20, a21, a22;

    mutable double a0, a1, a2;

    double zmin, zmax, zsol, xoxsol;

    void CoefInit (double dMetals) const;

 public:

 Padova() : a00(10.13), a01(0.07547), a02(-0.008084),

      a10(-4.424),a11(-0.7939), a12(-0.1187),

      a20(1.262),a21(0.3385),a22(0.05417),

      a0(0.0), a1(0.0), a2(0.0),

      zmin(7e-5), zmax(3e-2), zsol(0.02), xoxsol(9e-3) {}


    double Lifetime(double dStarMass, double dMetals) const;

    double StarMass(double dStarLtime, double dMetals) const;

    void pup(PUP::er& p) {

    p | a00;

    p | a01;

    p | a02;

    p | a10;

    p | a11;

    p | a12;

    p | a20;

    p | a21;

    p | a22;

    p | a0;

    p | a1;

    p | a2;

    p | zmin;

    p | zmax;

    p | zsol;

    p | xoxsol;

    }

    };


#endif