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evolv1.f
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evolv1.f
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***
SUBROUTINE evolv1(kw,mass,mt,r,lum,mc,rc,menv,renv,ospin,
& epoch,tm,tphys,tphysf,dtp,z,zpars,vkick)
c-------------------------------------------------------------c
c
c Evolves a single star.
c Mass loss is an option.
c The timestep is not constant but determined by certain criteria.
c Plots the HRD and variables as a function of time.
c
c Written by Jarrod Hurley 26/08/97 at the Institute of
c Astronomy, Cambridge.
c
c-------------------------------------------------------------c
c
c STELLAR TYPES - KW
c
c 0 - deeply or fully convective low mass MS star
c 1 - Main Sequence star
c 2 - Hertzsprung Gap
c 3 - First Giant Branch
c 4 - Core Helium Burning
c 5 - First Asymptotic Giant Branch
c 6 - Second Asymptotic Giant Branch
c 7 - Main Sequence Naked Helium star
c 8 - Hertzsprung Gap Naked Helium star
c 9 - Giant Branch Naked Helium star
c 10 - Helium White Dwarf
c 11 - Carbon/Oxygen White Dwarf
c 12 - Oxygen/Neon White Dwarf
c 13 - Neutron Star
c 14 - Black Hole
c 15 - Massless Supernova
c
c-------------------------------------------------------------c
implicit none
*
integer kw,it,ip,jp,j,kwold,rflag
integer nv
parameter(nv=50000)
*
real*8 mass,z,aj
real*8 epoch,tphys,tphys2,tmold,tbgold
real*8 mt,tm,tn,tphysf,dtp,tsave
real*8 tscls(20),lums(10),GB(10),zpars(20)
real*8 r,lum,mc,teff,rc,menv,renv,vs(3)
real*8 ospin,jspin,djt,djmb,k2,k3,vkick
parameter(k3=0.21d0)
real*8 m0,r1,lum1,mc1,rc1,menv1,renv1,k21
real*8 dt,dtm,dtr,dr,dtdr,dms,dml,mt2,rl
real*8 tol,tiny
parameter(tol=1.0d-10,tiny=1.0d-14)
real*8 ajhold,rm0,eps,alpha2
parameter(eps=1.0d-06,alpha2=0.09d0)
real*8 mlwind,vrotf
external mlwind,vrotf
logical iplot,isave
REAL*8 neta,bwind,hewind,mxns
COMMON /VALUE1/ neta,bwind,hewind,mxns
REAL*8 pts1,pts2,pts3
COMMON /POINTS/ pts1,pts2,pts3
REAL scm(50000,14),spp(20,3)
COMMON /SINGLE/ scm,spp
*
dtm = 0.d0
r = 0.d0
lum = 0.d0
mc = 0.d0
mc1 = 0.d0
rc = 0.d0
rl = 0.d0
if(ospin.le.0.d0)then
ospin = 1.0d-10
jspin = 1.0d-10
endif
k2 = 0.15d0
rflag = 0
*
* Setup variables which control the output (if it is required).
*
ip = 0
jp = 0
tsave = tphys
isave = .true.
iplot = .false.
if(dtp.le.0.d0)then
iplot = .true.
isave = .false.
tsave = tphysf
elseif(dtp.gt.tphysf)then
isave = .false.
tsave = tphysf
endif
*
do 10 , j = 1,nv
*
if(neta.gt.tiny.and.j.gt.1)then
*
* Calculate mass loss from the previous timestep.
*
dt = 1.0d+06*dtm
dms = mlwind(kw,lum,r,mt,mc,rl,z)*dt
if(kw.lt.10)then
dml = mt - mc
if(dml.lt.dms)then
dtm = (dml/dms)*dtm
dms = dml
endif
endif
else
dms = 0.d0
endif
*
* Limit to 1% mass loss.
*
if(dms.gt.0.01d0*mt)then
dtm = 0.01d0*mt*dtm/dms
dms = 0.01d0*mt
endif
*
* Calculate the rate of angular momentum loss due to magnetic braking
* and/or mass loss.
*
if(j.gt.1)then
djt = (2.d0/3.d0)*(dms/(1.0d+06*dtm))*r*r*ospin
if(mt.gt.0.35d0.and.kw.lt.10)then
djmb = 5.83d-16*menv*(r*ospin)**3/mt
djt = djt + djmb
endif
endif
*
* Update mass and time and reset epoch for a MS (and possibly a HG) star.
*
if(dms.gt.0.d0)then
mt = mt - dms
if(kw.le.2.or.kw.eq.7)then
m0 = mass
mc1 = mc
mass = mt
tmold = tm
tbgold = tscls(1)
CALL star(kw,mass,mt,tm,tn,tscls,lums,GB,zpars)
if(kw.eq.2)then
if(GB(9).lt.mc1.or.m0.gt.zpars(3))then
mass = m0
else
epoch = tm + (tscls(1) - tm)*(ajhold-tmold)/
& (tbgold - tmold)
epoch = tphys - epoch
endif
else
epoch = tphys - ajhold*tm/tmold
endif
endif
endif
tphys2 = tphys
tphys = tphys + dtm
*
* Find the landmark luminosities and timescales as well as setting
* the GB parameters.
*
aj = tphys - epoch
CALL star(kw,mass,mt,tm,tn,tscls,lums,GB,zpars)
*
* Find the current radius, luminosity, core mass and stellar type
* given the initial mass, current mass, metallicity and age
*
kwold = kw
CALL hrdiag(mass,aj,mt,tm,tn,tscls,lums,GB,zpars,
& r,lum,kw,mc,rc,menv,renv,k2)
*
* If mass loss has occurred and no type change then check that we
* have indeed limited the radius change to 10%.
*
if(kw.eq.kwold.and.dms.gt.0.d0.and.rflag.ne.0)then
mt2 = mt + dms
dml = dms/dtm
it = 0
20 dr = r - rm0
if(ABS(dr).gt.0.1d0*rm0)then
it = it + 1
if(it.eq.20.and.kw.eq.4) goto 30
if(it.gt.30)then
WRITE(99,*)' DANGER1! ',it,kw,mass,dr,rm0
WRITE(*,*)' STOP: EVOLV1 FATAL ERROR '
CALL exit(0)
STOP
endif
dtdr = dtm/ABS(dr)
dtm = alpha2*MAX(rm0,r)*dtdr
if(it.ge.20) dtm = 0.5d0*dtm
if(dtm.lt.1.0d-07*aj) goto 30
dms = dtm*dml
mt = mt2 - dms
if(kw.le.2.or.kw.eq.7)then
mass = mt
CALL star(kw,mass,mt,tm,tn,tscls,lums,GB,zpars)
if(kw.eq.2)then
if(GB(9).lt.mc1.or.m0.gt.zpars(3))then
mass = m0
else
epoch = tm + (tscls(1) - tm)*(ajhold-tmold)/
& (tbgold - tmold)
epoch = tphys2 - epoch
endif
else
epoch = tphys2 - ajhold*tm/tmold
endif
endif
tphys = tphys2 + dtm
aj = tphys - epoch
mc = mc1
CALL star(kw,mass,mt,tm,tn,tscls,lums,GB,zpars)
CALL hrdiag(mass,aj,mt,tm,tn,tscls,lums,GB,zpars,
& r,lum,kw,mc,rc,menv,renv,k2)
goto 20
endif
30 continue
endif
*
* Initialize or adjust the spin of the star.
*
if(j.eq.1)then
if(tphys.lt.tiny.and.ospin.lt.0.001d0)then
ospin = 45.35d0*vrotf(mt)/r
endif
jspin = ospin*(k2*r*r*(mt-mc)+k3*rc*rc*mc)
else
jspin = MAX(1.0d-10,jspin - djt*1.0d+06*dtm)
ospin = jspin/(k2*r*r*(mt-mc)+k3*rc*rc*mc)
endif
*
* Test for changes in evolution type.
*
if(j.eq.1.or.kw.ne.kwold)then
*
* Force new NS or BH to have a one second period.
*
if(kw.eq.13.or.kw.eq.14)then
ospin = 2.0d+08
jspin = k3*rc*rc*mc*ospin
CALL kick(kw,mass,mt,0.d0,0.d0,-1.d0,0.d0,vs)
vkick = dsqrt(vs(1)*vs(1)+vs(2)*vs(2)+vs(3)*vs(3))
endif
jp = jp + 1
spp(jp,1) = tphys
spp(jp,2) = float(kw)
if(kw.eq.15)then
spp(jp,3) = mass
goto 90
else
spp(jp,3) = mt
endif
endif
*
* Record values for plotting and reset epoch.
*
epoch = tphys - aj
if((isave.and.tphys.ge.tsave).or.iplot)then
ip = ip + 1
scm(ip,1) = tphys
scm(ip,2) = float(kw)
scm(ip,3) = mass
scm(ip,4) = mt
scm(ip,5) = log10(lum)
scm(ip,6) = log10(r)
teff = 1000.d0*((1130.d0*lum/(r**2.d0))**(1.d0/4.d0))
scm(ip,7) = log10(teff)
scm(ip,8) = mc
scm(ip,9) = rc
scm(ip,10) = menv
scm(ip,11) = renv
scm(ip,12) = epoch
scm(ip,13) = ospin
if(isave) tsave = tsave + dtp
if(tphysf.lt.tiny)then
ip = ip + 1
do 35 , it = 1,13
scm(ip,it) = scm(ip-1,it)
35 continue
endif
endif
*
if(tphys.ge.tphysf)then
jp = jp + 1
spp(jp,1) = tphys
spp(jp,2) = float(kw)
spp(jp,3) = mt
goto 90
endif
*
* Record radius and current age.
*
rm0 = r
ajhold = aj
if(kw.ne.kwold) kwold = kw
CALL deltat(kw,aj,tm,tn,tscls,dtm,dtr)
*
* Check for type change.
*
it = 0
m0 = mass
if((dtr-dtm).le.tol.and.kw.le.9)then
*
* Check final radius for too large a jump.
*
aj = MAX(aj,aj*(1.d0-eps)+dtr)
mc1 = mc
CALL hrdiag(mass,aj,mt,tm,tn,tscls,lums,GB,zpars,
& r1,lum1,kw,mc1,rc1,menv1,renv1,k21)
dr = r1 - rm0
if(ABS(dr).gt.0.1d0*rm0)then
dtm = dtr - ajhold*eps
dtdr = dtm/ABS(dr)
dtm = alpha2*MAX(r1,rm0)*dtdr
goto 40
else
dtm = dtr
goto 50
endif
endif
*
* Limit to a 10% increase in radius assuming no further mass loss
* and thus that the pertubation functions due to small envelope mass
* will not change the radius.
*
40 aj = ajhold + dtm
mc1 = mc
CALL hrdiag(mass,aj,mt,tm,tn,tscls,lums,GB,zpars,
& r1,lum1,kw,mc1,rc1,menv1,renv1,k21)
dr = r1 - rm0
it = it + 1
if(it.eq.20.and.kw.eq.4) goto 50
if(it.gt.30)then
WRITE(99,*)' DANGER2! ',it,kw,mass,dr,rm0
WRITE(*,*)' STOP: EVOLV1 FATAL ERROR '
CALL exit(0)
STOP
endif
if(ABS(dr).gt.0.1d0*rm0)then
dtdr = dtm/ABS(dr)
dtm = alpha2*MAX(rm0,r1)*dtdr
if(it.ge.20) dtm = 0.5d0*dtm
goto 40
endif
*
50 continue
*
* Ensure that change of type has not occurred during radius check.
* This is rare but may occur for HG stars of ZAMS mass > 50 Msun.
*
if(kw.ne.kwold)then
kw = kwold
mass = m0
CALL star(kw,mass,mt,tm,tn,tscls,lums,GB,zpars)
endif
*
* Choose minimum of time-scale and remaining interval (> 100 yrs).
*
dtm = MAX(dtm,1.0d-07*aj)
dtm = MIN(dtm,tsave-tphys)
*
10 continue
*
90 continue
*
tphysf = tphys
scm(ip+1,1) = -1.0
spp(jp+1,1) = -1.0
if(ip.ge.nv)then
WRITE(99,*)' EVOLV1 ARRAY ERROR ',mass
WRITE(*,*)' STOP: EVOLV1 ARRAY ERROR '
CALL exit(0)
STOP
endif
*
RETURN
END
***