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README_SSE
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README_SSE
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************************************************************************
Information on the SSE package.
Created by Jarrod Hurley at the Institute of Astronomy, Cambridge, UK
in collaboration with Onno Pols and Christopher Tout.
12th February 2000.
More information can be found in the paper:
"Comprehensive analytic formulae for stellar evolution as a function
of mass and metallicity"
Hurley J.R., Pols O.R., Tout C.A., 2000, MNRAS, 315, 543.
This reference should be used for any publications that utilise the
SSE package.
Any queries that are not answered by referring to the paper can be addressed
to: jhurley@astro.swin.edu.au
************************************************************************
Mass range: 0.1 -> 100 Msun
Metallicity Range: 0.0001 -> 0.03 (0.02 is solar)
************************************************************************
The SSE package contains the following FORTRAN files:
sse.f - Main routine. Evolves one star and creates data files.
const_bse.h - parameter file
deltat.f - determines stellar evolution update timestep
evolv1.f - routine that controls the evolution of each star
evolve.in - input file for sse.f
hrdiag.f - subroutine to decide which evolution stage the star is
currently at and then the appropriate luminosity, radius
and core mass are calculated
kick.f - generates supernova kick
mlwind.f - subroutine which contains the preferred mass loss prescription
mrenv.f - calculates envelope parameters
ran3.f - random number generator
star.f - subroutine which derives the landmark timescales and
luminosities that divide the various evolution stages.
zcnsts.f - subroutine which sets all the constants of the formulae which
depend on metallicity so that there is no Z dependence
elsewhere
zdata.h - data file which contains all the coefficient values
zfuncs.f - contains all the formulae as a collection of separate functions
and
Makefile - f77 compiler. Use command "make sse"
************************************************************************
The main routine sse.f contains comments that should (hopefully?)
make everything self-explanatory. It is simply an example to show how
EVOLV1 should be used.
In the case of EVOLV1 being called in a loop over many stars
be careful to initialise each new star, i.e.
mt = mass
kw = 1
tphys = 0.0
epoch = 0.0
ospin = 0.0
However, the routine ZCNSTS only needs to be called each time you change
metallicity.
Note that the epoch is required because the physical time and the
age of the star are not always the same.
For example, when a star becomes a WD, at say time tWD, its' effective age
becomes zero because the WD evolution formulae start from t=0.0. Therefore
we set epoch = tWD and from then on the age of the star is age = t - epoch.
The same happens when the star becomes a naked helium star, NS or BH. The
epoch parameter is also very useful in binary evolution when a star needs
to be rejuvenated or aged as a result of mass transfer.
You may not want to use sse.f at all and instead, for example, prefer to use
EVOLV1 directly as the main routine.
Also, you may want to utilise the individual subroutines in different ways.
For example, if instead of actually evolving the stars all you want
is an estimate of evolution timescales then, given the mass of a star
(and mt=mass, kw=1), a call to STAR will return the array TSCLS
which contains the necessary information.
PROBLEMS: if the program stops with a 'FATAL ERROR' then more information
should be contained in the fort.99 file. When you have
identified the initial conditions that produce the error then
please contact me and I may help to fix the bug - assuming it
can be reproduced!
************************************************************************
Definitions of the various data arrays are contained in the header of the
subroutine where they are filled. A summary is also given here:
* ---------------------------------------------------------------------
MASS Initial stellar mass in solar units
AJ Current age in Myr
MT Current mass in solar units (used for R)
TM Main sequence lifetime
TN Nuclear burning lifetime assuming no further mass loss
TSCLS Evolution timescales for different stages
LUMS Landmark luminosities
GB Giant branch parameters
ZPARS Parameters for distinguishing various mass intervals
R Stellar radius in solar units
KW Evolution type (0 - 15).
MC Core mass in solar units
* ------------------------------------------------------------
KW
0 - deeply or fully convective low mass MS star
1 - Main Sequence star
2 - Hertzsprung Gap
3 - First Giant Branch
4 - Core Helium Burning
5 - First Asymptotic Giant Branch
6 - Second Asymptotic Giant Branch
7 - Main Sequence Naked Helium star
8 - Hertzsprung Gap Naked Helium star
9 - Giant Branch Naked Helium star
10 - Helium White Dwarf
11 - Carbon/Oxygen White Dwarf
12 - Oxygen/Neon White Dwarf
13 - Neutron Star
14 - Black Hole
15 - Massless Supernova
* ------------------------------------------------------------
TSCLS (all timescales are in Myr units)
1; BGB 2; He ignition 3; He burning
4; Giant t(inf1) 5; Giant t(inf2) 6; Giant t(Mx)
7; FAGB t(inf1) 8; FAGB t(inf2) 9; FAGB t(Mx)
10; SAGB t(inf1) 11; SAGB t(inf2) 12; SAGB t(Mx)
13; TP 14; t(Mcmax)
* ------------------------------------------------------------
LUMS (all luminosities are in solar units)
1; ZAMS 2; End MS 3; BGB
4; He ignition 5; He burning 6; L(Mx)
7; BAGB 8; TP
* ------------------------------------------------------------
GB = giant branch parameters
1; effective A(H) 2; A(H,He) 3; B
4; D 5; p 6; q
7; Mx 8; A(He) 9; Mc,BGB
* ------------------------------------------------------------
ZPARS
1; M below which hook doesn't appear on MS, Mhook.
2; M above which He ignition occurs non-degenerately, Mhef.
3; M above which He ignition occurs on the HG, Mfgb.
4; M below which C/O ignition doesn't occur, Mup.
5; M above which C ignites in the centre, Mec.
6; value of log D for M<= zpars(3)
7; value of x for Rgb propto M^(-x)
8; value of x for tMS = MAX(tHOOK,x*tBGB)
9; constant for McHeIf when computing Mc,BGB, mchefl.
10; constant for McHeIf when computing Mc,HeI, mchefl.
11; hydrogen abundance.
12; helium abundance.
13; constant x in rmin = rgb*x**y used by LM CHeB.
14; z**0.4 to be used for WD L formula.
* ------------------------------------------------------------
Good luck!
************************************************************************