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evolv2.f
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***
SUBROUTINE evolv2(kstar,mass,tb,ecc,z,tphysf,
\ dtp,mass0,rad,lumin,massc,radc,
\ menv,renv,ospin,B_0,bacc,tacc,epoch,tms,
\ bhspin,tphys,zpars,bkick,kick_info,
\ bpp_index_out,bcm_index_out,kick_info_out)
IMPLICIT NONE
INCLUDE 'const_bse.h'
INCLUDE 'checkstate.h'
***
*
* B I N A R Y
* ***********
*
* Roche lobe overflow.
* --------------------
*
* Developed by Jarrod Hurley, IOA, Cambridge.
* .........................................................
*
* Advice by Christopher Tout, Onno Pols & Sverre Aarseth.
* ++++++++++++++++++++++++++++++++++++++++++++++++++
*
* Adapted from Aarseth's code 21st September 1996.
* Fully revised on 27th November 1996 to remove vestiges of N-body code and
* incorporate corrections.
* Fully revised on 1st April 1998 to include new stellar evolution formulae
* and associated binary evolution changes.
* Fully revised on 4th July 1998 to include eccentricity, tidal
* circularization, wind accretion, velocity kicks for supernovae and all
* associated orbital momentum changes.
*
***
*
* See Tout et al., 1997, MNRAS, 291, 732 for a description of many of the
* processes in this code as well as the relevant references mentioned
* within the code.
*
* Reference for the stellar evolution formulae is Hurley, Pols & Tout,
* 2000, MNRAS, 315, 543 (SSE paper).
* Reference for the binary evolution algorithm is Hurley, Tout & Pols,
* 2002, MNRAS, 329, 897 (BSE paper).
*
***
*
* March 2001 *
* Changes since version 3, i.e. since production of Paper3:
*
* 1) The Eddington limit flag (on/off) has been replaced by an
* Eddington limit multiplicative factor (eddfac). So if you
* want to neglect the Eddington limit you would set eddfac
* to a large value.
*
* 2) To determine whether material transferred during RLOF forms
* an accretion disk around the secondary or hits the secondary
* in a direct stream we calculate a minimum radial distance, rmin,
* of the mass stream from the secondary. This is taken from eq.(1)
* of Ulrich & Burger (1976, ApJ, 206, 509) which they fitted to
* the calculations of Lubow & Shu (1974, ApJ, 198, 383).
* If rmin is less than the radius of the secondary then an
* accretion disk is not formed.
* Note that the formula for rmin given by Ulrich & Burger is valid
* for all q whereas that given by Nelemans et al. (2001, A&A,
* submitted) in their eq.(6) is only valid for q < 1 where
* they define q = Mdonor/Maccretor, i.e. DD systems.
*
* 3) The changes to orbital and spin angular momentum owing to
* RLOF mass transfer have been improved, and an new input option
* now exists.
* When mass is lost from the system during RLOF there are now
* three choices as to how the orbital angular momentum is
* affected: a) the lost material carries with it a fraction
* gamma of the orbital angular momentum, i.e.
* dJorb = gamma*dm*a^2*omega_orb; b) the material carries with it
* the specific angular momentum of the primary, i.e.
* dJorb = dm*a_1^2*omega_orb; or c) assume the material is lost
* from the system as if a wind from the secondary, i.e.
* dJorb = dm*a_2^2*omega_orb.
* The parameter gamma is an input option.
* Choice c) is used if the mass transfer is super-Eddington
* or the system is experiencing novae eruptions.
* In all other cases choice a) is used if gamma > 0.0, b) if
* gamma = -1.0 and c) is used if gamma = -2.0.
* The primary spin angular momentum is reduced by an amount
* dm1*r_1^2*omega_1 when an amount of mass dm1 is transferred
* from the primary.
* If the secondary accretes through a disk then its spin
* angular momentum is altered by assuming that the material
* falls onto the star from the inner edge of a Keplerian
* disk and that the system is in a steady state, i.e.
* an amount dm2*SQRT(G*m_2*r_2).
* If there is no accretion disk then we calculate the angular
* momentum of the transferred material by using the radius at
* at which the disk would have formed (rdisk = 1.7*rmin, see
* Ulrich & Burger 1976) if allowed, i.e. the angular momentum
* of the inner Lagrangian point, and add this directly to
* the secondary, i.e. an amount dm2*SQRT(G*m_2*rdisk).
* Total angular momentum is conserved in this model.
*
* 4) Now using q_crit = 3.0 for MS-MS Roche systems (previously we
* had nothing). This corresponds roughly to R proportional to M^5
* which should be true for the majority of the MS (varies from
* (M^17 -> M^2). If q > q_crit then contact occurs.
* For CHeB primaries we also take q_crit = 3.0 and allow
* common-envelope to occur if this is exceeded.
*
* 5) The value of lambda used in calculations of the envelope binding
* energy for giants in common-envelope is now variable (see function
* in zfuncs). The lambda function has been fitted by Onno to detailed
* models ... he will write about this soon!
*
* 6) Note that eq.42 in the paper is missing a SQRT around the
* MR^2/a^5 part. This needs to be corrected in any code update
* paper with a thanks to Jeremy Sepinsky (student at NorthWestern).
* It is ok in the code.
*
* March 2003 *
* New input options added:
*
* ifflag - for the mass of a WD you can choose to use the mass that
* results from the evolution algorithm (basically a competition
* between core-mass growth and envelope mass-loss) or use the IFMR
* proposed by Han, Podsiadlowski & Eggleton, 1995, MNRAS, 272, 800
* [>0 activates HPE IFMR].
*
* wdflag - for the cooling of WDs you can choose to use either the standard
* Mestel cooling law (see SSE paper) or a modified-Mestel law that
* is better matched to detailed models (provided by Brad Hansen
* ... see Hurley & Shara, 2003, ApJ, May 20, in press)
* [>0 activates modified-Mestel].
*
* bhflag - choose whether or not black holes should get velocity kicks
* at formation
* [0= no kick; >0 kick].
*
* remnantflag - for the mass of neutron stars and black holes you can use either
* the SSE prescription or the prescription presented by
* Belczynski et al. 2002, ApJ, 572, 407 who found that SSE was
* underestimating the masses of these stars. In either case you also
* need to set the maximum NS mass (mxns) for the prescription
* [0= SSE, mxns=1.8; >0 Belczynski, mxns=3.0].
*
* Sept 2004 *
* Input options added/changed:
*
* ceflag - set to 1 this uses de Kool (or Podsiadlowski) CE prescription,
* other options, such as Yungelson, could be added as well.
*
* hewind - factor to control the amount of He star mass-loss, i.e.
* 1.0e-13*hewind*L^(2/3) gives He star mass-loss.
*
*
* ++++++++++++++++++++++++++++++++++++++++++++++++++
***
*
INTEGER loop,iter,intpol,k,ip,jp,j1,j2
INTEGER bcm_index_out, bpp_index_out
INTEGER kcomp1,kcomp2,formation(2)
PARAMETER(loop=20000)
INTEGER kstar(2),kw,kst,kw1,kw2,kmin,kmax
INTEGER kstar1_bpp,kstar2_bpp
*
REAL*8 km,km0,tphys,tphys0,dtm0,tphys00,tphysfhold
REAL*8 tphysf,dtp,tsave,dtp_original
REAL*8 aj(2),aj0(2),epoch(2),tms(2),tbgb(2),tkh(2),dtmi(2)
REAL*8 mass0(2),mass(2),massc(2),menv(2),mass00(2),mcxx(2)
REAL*8 mass1_bpp,mass2_bpp
REAL*8 rad(2),rol(2),rol0(2),rdot(2),radc(2),renv(2),radx(2)
REAL*8 lumin(2),k2str(2),q(2),dms(2),dmr(2),dmt(2)
REAL*8 dml,vorb2,vwind2,omv2,ivsqm,lacc,kick_info(2,17)
REAL*8 bkick(20)
REAL*8 kick_info_out(2,17)
REAL*8 sep,dr,tb,dme,tdyn,taum,dm1,dm2,dmchk,qc,dt,pd,rlperi
REAL*8 m1ce,m2ce,mch,tmsnew,dm22,mew
PARAMETER(mch=1.44d0)
REAL*8 yeardy,yearsc,aursun
PARAMETER(yeardy=365.24d0,aursun=214.95d0,yearsc=3.1557d+07)
REAL*8 acc1,tiny
PARAMETER(acc1=3.920659d+08,tiny=1.0d-14)
REAL*8 ecc,ecc1,tc,tcirc,ttid,ecc2,omecc2,sqome2,sqome3,sqome5
REAL*8 f1,f2,f3,f4,f5,f,raa2,raa6,eqspin,rg2,tcqr
REAL*8 k3,mr23yr,twopi
PARAMETER(k3=0.21d0,mr23yr=0.4311d0)
REAL*8 jspin(2),ospin(2),jorb,oorb,jspbru,ospbru
REAL*8 bhspin(2)
REAL*8 delet,delet1,dspint(2),djspint(2),djtx(2)
REAL*8 dtj,djorb,djgr,djmb,djt,djtt,rmin,rdisk
REAL*8 etaBH,maxspinBH
*
INTEGER pulsar
INTEGER mergemsp,merge_mem,notamerger,binstate,mergertype
REAL*8 fallback,sigmahold
REAL*8 vk,u1,u2,s,Kconst,betahold,convradcomp(2),teff(2)
REAL*8 B_0(2),bacc(2),tacc(2),xip,xihold
REAL*8 deltam1_bcm,deltam2_bcm,b01_bcm,b02_bcm
REAL*8 B(2),Bbot,omdot,b_mdot,b_mdot_lim,evolve_type
COMMON /fall/fallback
REAL ran3
EXTERNAL ran3
*
*
REAL*8 z,tm,tn,m0,mt,rm,lum,mc,rc,me,re,k2,age,dtm,dtr
REAL*8 tscls(20),lums(10),GB(10),zpars(20)
REAL*8 zero,ngtv,ngtv2,mt2,rrl1,rrl2,mcx,teff1,teff2
REAL*8 mass1i,mass2i,tbi,ecci
LOGICAL coel,com,prec,inttry,change,snova,sgl
LOGICAL supedd,novae,disk,inspiral
LOGICAL iplot,isave
REAL*8 rl,mlwind,vrotf,corerd,f_fac
EXTERNAL rl,mlwind,vrotf,corerd
*
REAL*8 kw3,wsun,wx
PARAMETER(kw3=619.2d0,wsun=9.46d+07,wx=9.46d+08)
LOGICAL output
*
REAL*8 qc_fixed
LOGICAL switchedCE,disrupt
Cf2py intent(in) kstar
Cf2py intent(in) mass
Cf2py intent(in) tb
Cf2py intent(in) ecc
Cf2py intent(in) z
Cf2py intent(in) tphysf
Cf2py intent(in) dtp
Cf2py intent(in) mass0
Cf2py intent(in) rad
Cf2py intent(in) lumin
Cf2py intent(in) massc
Cf2py intent(in) radc
Cf2py intent(in) menv
Cf2py intent(in) renv
Cf2py intent(in) ospin
Cf2py intent(in) B_0
Cf2py intent(in) bacc
Cf2py intent(in) tacc
Cf2py intent(in) epoch
Cf2py intent(in) tms
Cf2py intent(in) bhspin
Cf2py intent(in) tphys
Cf2py intent(in) zpars
Cf2py intent(in) bkick
Cf2py intent(in) kick_info
Cf2py intent(out) bpp_index_out
Cf2py intent(out) bcm_index_out
Cf2py intent(out) kick_info_out
if(using_cmc.eq.0)then
CALL instar
endif
*
* Save the initial state.
*
* CE2flag = 0
kstar1_bpp = 0
kstar2_bpp = 0
mass1_bpp = 0.d0
mass2_bpp = 0.d0
mass1i = mass(1)
mass2i = mass(2)
tbi = tb
ecci = ecc
*
zero = 0.d0
ngtv = -1.d0
ngtv2 = -2.d0
twopi = 2.d0*ACOS(-1.d0)
Mbh_initial = 0.d0
* disrupt tracks if system get disrupted by a SN during the common
* envelope
disrupt = .false.
* value for bcm[ii,37] which tracks binary state; 0 for binary, 1 for merger, 2 for disrupted
binstate = 0
* value for bcm[ii,38] which tracks merger types; only set when binstate is 1
* the logic is to combine kstar values of merged objects. so 1313 or 0809.
mergertype = -1
*Captures original sigma so after ECSN we can reset it.
sigmahold = sigma
*memory for wind mass loss factor
betahold = beta
** SET PULSAR VALUES HERE**
* PDK
pulsar = 1 ! allows for pulsar physics; not a flag since we heart pulsars
Kconst = 2.5d-49
Bbot = 5e+7 !100.d0 or ~d+07.
b_mdot_lim = -1.0e-11 !limiting accretion induced field decay with mdot as a proxy for
* accretion temperature and number of impurities.
xihold = xi
xip = 1 !Modifies NS wind ang. mom. accretion.
formation(1) = 0 !helps determine formation channel of interesting systems.
formation(2) = 0
pisn_track(1) = 0 !tracks whether a PISN occurred for each
component.
pisn_track(2) = 0
merger = -1 !used in CMC to track systems that dynamically merge
notamerger = 0 !if 0 you reset the merger NS product to new factory settings else you don't.
mergemsp = 1 !if set to 1 any NS that merges with another star where the NS is an MSP stays an MSP...
merge_mem = 0
output = .false. ! .true. turns on, .false. turns off.
* WARNING: can fill up the output file very quickly.
* With N=2e6 .stdout was 3.2 GB in 6 mins. If needed you can
* be more selective with outputting, but must add this yourself!
* if(id1_pass.eq.1)then!.and.tphysf.gt.17.50d0.and.
** & tphysf.lt.17.6d0)then
* output = .true.
* endif
*
* Initialize the parameters.
*
if(using_cmc.eq.0)then
bcm_index_out = 0
bpp_index_out = 0
kick_info_out = 0.d0
endif
*
* Set the seed for the random number generator.
*
* idum1 = INT(sep*100)
if(idum1.gt.0.and.using_cmc.eq.0) idum1 = -idum1
*
* Set the collision matrix.
*
if(using_cmc.eq.0)then
CALL zcnsts(z,zpars)
endif
kmin = 1
kmax = 2
sgl = .false.
mt2 = MIN(mass(1),mass(2))
kst = 0
iter = 0 ! PDK addition, just incase you bail out before 4 loop (usually from multiple calls for one evolve)
*
if(mt2.lt.tiny.or.tb.le.0.d0)then
sgl = .true.
if(mt2.lt.tiny)then
mt2 = 0.d0
if(mass(1).lt.tiny)then
if(tphys.lt.tiny)then
mass0(1) = 0.01d0
mass(1) = mass0(1)
kst = 1
else
kmin = 2
lumin(1) = 1.0d-10
rad(1) = 1.0d-10
massc(1) = 0.d0
dmt(1) = 0.d0
dmr(1) = 0.d0
endif
ospin(1) = 1.0d-10
jspin(1) = 1.0d-10
dtmi(1) = 5.0d+04 !5Gyr, added for use of single stars in evolv2.f
else
if(tphys.lt.tiny)then
mass0(2) = 0.01d0
mass(2) = mass0(2)
kst = 2
else
kmax = 1
lumin(2) = 1.0d-10
rad(2) = 1.0d-10
massc(2) = 0.d0
dmt(2) = 0.d0
dmr(2) = 0.d0
endif
ospin(2) = 1.0d-10
jspin(2) = 1.0d-10
dtmi(2) = 5.0d+04 !5Gyr, added for use of single stars in evolv2.f
endif
endif
ecc = -1.d0
tb = 0.d0
sep = 1.0d+10
oorb = 0.d0
jorb = 0.d0
if(kstar(1).ne.14.d0.or.using_cmc.eq.0) bhspin(1) = 0.d0
if(kstar(2).ne.14.d0.or.using_cmc.eq.0) bhspin(2) = 0.d0
if(ospin(1).lt.0.0) ospin(1) = 1.0d-10
if(ospin(2).lt.0.0) ospin(2) = 1.0d-10
q(1) = 1.0d+10
q(2) = 1.0d+10
rol(1) = 1.0d+10
rol(2) = 1.0d+10
else
tb = tb/yeardy
sep = aursun*(tb*tb*(mass(1) + mass(2)))**(1.d0/3.d0)
oorb = twopi/tb
jorb = mass(1)*mass(2)/(mass(1)+mass(2))
& *SQRT(1.d0-ecc*ecc)*sep*sep*oorb
if(ospin(1).lt.0.d0) ospin(1) = oorb
if(ospin(2).lt.0.d0) ospin(2) = oorb
endif
*
do 500 , k = kmin,kmax
age = tphys - epoch(k)
mc = massc(k)
rc = radc(k)
CALL star(kstar(k),mass0(k),mass(k),tm,tn,tscls,lums,GB,zpars)
CALL hrdiag(mass0(k),age,mass(k),tm,tn,tscls,lums,GB,zpars,
& rm,lum,kstar(k),mc,rc,me,re,k2,bhspin(k),k)
aj(k) = age
epoch(k) = tphys - age
rad(k) = rm
lumin(k) = lum
teff(k) = 1000.d0*((1130.d0*lumin(k)/
& (rad(k)**2.d0))**(1.d0/4.d0))
massc(k) = mc
radc(k) = rc
menv(k) = me
renv(k) = re
k2str(k) = k2
tms(k) = tm
tbgb(k) = tscls(1)
*
if(tphys.lt.tiny.and.ospin(k).le.0.001d0)then
ospin(k) = 45.35d0*vrotf(mass(k),ST_tide)/rm
endif
jspin(k) = ospin(k)*(k2*rm*rm*(mass(k)-mc)+k3*rc*rc*mc)
if(.not.sgl)then
q(k) = mass(k)/mass(3-k)
rol(k) = rl(q(k))*sep*(1.d0-ecc)
endif
rol0(k) = rol(k)
dmr(k) = 0.d0
dmt(k) = 0.d0
djspint(k) = 0.d0
dtmi(k) = 1.0d+06
B(k) = 0.d0 !PK
if(kstar(k).ne.13)then
bacc(k) = 0.d0
tacc(k) = 0.d0
endif
*
500 continue
*
if(output) write(*,*)'Init:',mass(1),mass(2),massc(1),massc(2),
& rad(1),rad(2),kstar(1),kstar(2),sep,ospin(1),ospin(2),jspin(1),
& jspin(2),sigma,eddfac,z,id1_pass,id2_pass,tphysf,tphys,iter,tsave
*
if(mt2.lt.tiny)then
sep = 0.d0
if(kst.gt.0)then
mass0(kst) = 0.d0
mass(kst) = 0.d0
kmin = 3 - kst
kmax = kmin
endif
endif
*
* On the first entry the previous timestep is zero to prevent mass loss.
*
dtm = 0.d0
delet = 0.d0
djorb = 0.d0
*
* Setup variables which control the output (if it is required).
*
ip = 0
jp = 0
dtp_original = dtp
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
if(tphys.ge.tphysf) goto 140
4 iter = 0
intpol = 0
inttry = .false.
change = .false.
prec = .false.
snova = .false.
coel = .false.
com = .false.
inspiral = .false.
tphys0 = tphys
ecc1 = ecc
j1 = 1
j2 = 2
if(kstar(1).ge.10.and.kstar(1).le.14) dtmi(1) = 0.01d0
if(kstar(2).ge.10.and.kstar(2).le.14) dtmi(2) = 0.01d0
dm1 = 0.d0
dm2 = 0.d0
*
5 kw1 = kstar(1)
kw2 = kstar(2)
if(xi.eq.0)then
ospin(1) = 1.0d-10
ospin(2) = 1.0d-10
endif
*
dt = 1.0d+06*dtm
eqspin = 0.d0
djtt = 0.d0
*
if(output) write(*,*)'1st in 5: ',tphys,dt,kw1,kw2,
& mass(1),mass(2),intpol,iter
*
if(intpol.eq.0.and.ABS(dtm).gt.tiny.and..not.sgl)then
vorb2 = acc1*(mass(1)+mass(2))/sep
ivsqm = 1.d0/SQRT(1.d0-ecc*ecc)
do 501 , k = 1,2
*
* Determine the eddington limit for the accretor (3-k)
* Just in case the wind mass loss rates are *very* high
*
dme = 2.08d-03*eddfac*(1.d0/(1.d0 + zpars(11)))*rad(3-k)
* For BHs, follow Marchant et al. 2017
if(kstar(3-k).eq.14)then
maxspinBH = 6.d0**(1.d0/2.d0) * Mbh_initial
if(mass(3-k).lt.maxspinBH)then
etaBH = 1.d0 -
& (1.d0 - (mass(3-k)/(3.d0*Mbh_initial))**(2.d0))**(1.d0/2.d0)
else
etaBH = 0.42
endif
dme = 1.04e-3*eddfac*(1.d0/(1.d0 + zpars(11)))
& *(1.d0/etaBH)*rad(3-k)
endif
*
* Calculate wind mass loss from the previous timestep.
*
!check for kstar added by PA
if(neta.gt.tiny .and. kstar(k)<15)then
rlperi = rol(k)*(1.d0-ecc)
dmr(k) = mlwind(kstar(k),lumin(k),rad(k),mass(k),
& massc(k),rlperi,z)
*
* Calculate how much of wind mass loss from companion will be
* accreted (Boffin & Jorissen, A&A 1988, 205, 155).
*
if(beta.lt.0.d0)then !PK. following startrack
beta = 0.125
if(kstar(k).le.1)then
if(mass(k).gt.120.d0)then
beta = 7.d0
elseif(mass(k).le.1.4d0)then
beta = 0.5
else
beta = 7.d0*((mass(k)-1.4d0)/(120.d0-1.4d0))
& + 0.5d0
endif
elseif(kstar(k).ge.7.and.kstar(k).le.9)then
if(mass(k).gt.120.d0)then
beta = 7.d0
elseif(mass(k).le.10.d0)then
beta = 0.125
else
beta = 7.d0*((mass(k)-10.d0)/(120.d0-10.d0))
& + 0.125d0
endif
endif
endif
vwind2 = 2.d0*beta*acc1*mass(k)/rad(k)
omv2 = (1.d0 + vorb2/vwind2)**(3.d0/2.d0)
dmt(3-k) = ivsqm*acc2*dmr(k)*((acc1*mass(3-k)/vwind2)**2)
& /(2.d0*sep*sep*omv2)
dmt(3-k) = MIN(dmt(3-k),0.8d0*dmr(k))
*
* Apply Eddington limit just in case
*
if(dt.gt.0)then
dmt(3-k) = MIN(dmt(3-k),dme)
endif
beta = betahold
else
dmr(k) = 0.d0
dmt(3-k) = 0.d0
endif
501 continue
*
* Diagnostic for Symbiotic-type stars.
*
!check for kstar added by PA
if(neta.gt.tiny .and. kstar(j2)<15)then
lacc = 3.14d+07*mass(j2)*dmt(j2)/rad(j2)
lacc = lacc/lumin(j1)
endif
*
* Calculate orbital angular momentum change due to wind mass loss.
*
ecc2 = ecc*ecc
omecc2 = 1.d0 - ecc2
sqome2 = SQRT(omecc2)
*
djorb = ((dmr(1)+q(1)*dmt(1))*mass(2)*mass(2) +
& (dmr(2)+q(2)*dmt(2))*mass(1)*mass(1))*
& sep*sep*sqome2*oorb/(mass(1)+mass(2))**2
delet = ecc*(dmt(1)*(0.5d0/mass(1) + 1.d0/(mass(1)+mass(2))) +
& dmt(2)*(0.5d0/mass(2) + 1.d0/(mass(1)+mass(2))))
*
* For very close systems include angular momentum loss owing to
* gravitational radiation.
*
if(sep.le.100000.d0.and.grflag.eq.1)then
djgr = 8.315d-10*mass(1)*mass(2)*(mass(1)+mass(2))/
& (sep*sep*sep*sep)
f1 = (19.d0/6.d0) + (121.d0/96.d0)*ecc2
sqome5 = sqome2**5
delet1 = djgr*ecc*f1/sqome5
djgr = djgr*jorb*(1.d0+0.875d0*ecc2)/sqome5
djorb = djorb + djgr
delet = delet + delet1
endif
*
do 502 , k = 1,2
* Evaluate convective/radiative limits for a variety of stars as based
* on the work of Belczynski et al. (2008). As option.
* Note only certain stars of type k = 0, 1, 2, 4, 5, 6, 9 **double check
* 0, 1 have range of 0.35-Mms,conv. Mms,conv is function of metalicity.
* 2 & 4 have a temperature dependence. Convective if Teff < 10**3.73
* 3, 5 & 6 are giants and have no radiative envelopes.
* 9's envelope is convective when M < Mhe,conv, Mhe,conv = 3.0Msun.
*
if(ST_cr.le.0)then
if(kstar(k).le.1)then
convradcomp(k) = 1.25d0
else
convradcomp(k) = 99999999.d0
endif
else
if(kstar(k).le.1)then
* Main sequence mass limit varying with metallicity
convradcomp(k) = 1.25d0
if(z.gt.0.001d0.and.z.lt.zsun)then
convradcomp(k) = 0.747d0 + 55.73d0*z - 1532*z*z
elseif(z.le.0.001d0)then
convradcomp(k) = 0.8d0
endif
elseif(kstar(k).eq.2.or.kstar(k).eq.4)then
* H-rich HG and CHeB temperature limit
convradcomp(k) = 10.d0**3.73d0
elseif(kstar(k).le.6)then
* No limit or all other giant stars
* (compare this large value to mass).
convradcomp(k) = 99999999.d0
elseif(kstar(k).eq.9)then
* Mass limit for evolved He star
convradcomp(k) = 3.d0
endif
endif
*
* Calculate change in the intrinsic spin of the star.
*
*
* Pulsar wind spinup. PK.
*
if(kstar(k).eq.13.and.pulsar.gt.0)then
* Place propeller stuff here eventually.
if(xip.eq.1)then
* Modify spin angular momentum accretion according to Ruffert (1999)
* or magnetic field strength limit tested (but by no means established - in fact it
* is likely to change, especially when propeller and ablation are implemented)
* in Kiel et al. (2008).
if(B(k).gt.0.d0)then
xi = MIN(1.d0,(0.01d0*(2.0d+11/B(k)))+0.01d0)
xi = 0.01
else
xi = 0.01
endif
endif
djtx(k) = (2.d0/3.d0)*xi*dmt(k)*rad(3-k)*rad(3-k)*
& ospin(3-k)
djspint(k) = (2.d0/3.d0)*(dmr(k)*rad(k)*rad(k)*ospin(k))-
& djtx(k)
xi = xihold
if(output) write(*,*)'502 1:',k,djspint(k),djtx(k),
& dmt(k),rad(3-k),ospin(3-k),xi,xihold
else
djtx(k) = (2.d0/3.d0)*xi*dmt(k)*
& rad(3-k)*rad(3-k)*ospin(3-k)
djspint(k) = (2.d0/3.d0)*
& (dmr(k)*rad(k)*rad(k)*ospin(k)) - djtx(k)
endif
*
* Include magnetic braking for stars that have appreciable convective
* envelopes. This includes MS stars with M < 1.25, HG stars near the GB
* and giants. MB is not allowed for fully convective MS stars.
*
* if(mass(k).gt.0.35d0.and.kstar(k).lt.10)then
* djmb = 5.83d-16*menv(k)*(rad(k)*ospin(k))**3/mass(k)
* djspint(k) = djspint(k) + djmb
*
* if(mass(k).gt.0.35d0.and.kstar(k).lt.10.and.
* & menv(k).gt.0.0d0)then
* if (ospin(k) .le. wx) djmb = kw3 * rad(k)**4.0d0 *
* & (ospin(k)/wsun)**3.0d0
* if (ospin(k) .gt. wx) djmb = kw3 * rad(k)**4.0d0 *
* & (ospin(k)/wsun)**1.3d0 * (wx/wsun)**1.7d0
* djspint(k) = djspint(k) + djmb
djmb = 0.d0
if(htpmb.eq.0)then
* HTP02 method
if(mass(k).gt.0.35d0.and.kstar(k).lt.10)then
djmb = 5.83d-16*menv(k)*
& (rad(k)*ospin(k))**3/mass(k)
djspint(k) = djspint(k) + djmb
endif
else
if(ST_cr.le.0.and.mass(k).gt.0.35d0.and.
& kstar(k).lt.10.and.menv(k).gt.0.0d0)then
* Ivanova & Taam (2002) method
if(ospin(k).le.wx) djmb = kw3 * rad(k)**4.0d0 *
& (ospin(k)/wsun)**3.0d0
if(ospin(k).gt.wx) djmb = kw3 * rad(k)**4.0d0 *
& (ospin(k)/wsun)**1.3d0 * (wx/wsun)**1.7d0
djspint(k) = djspint(k) + djmb
elseif(ST_cr.gt.0.and.menv(k).gt.0.d0.and.
& ((kstar(k).le.1.and.mass(k).gt.0.35d0.and.
& mass(k).le.convradcomp(k)).or.
& (kstar(k).eq.2.and.teff(k).le.convradcomp(k)).or.
& (kstar(k).eq.4.and.teff(k).le.convradcomp(k)).or.
& ((kstar(k).eq.3).or.(kstar(k).eq.5).or.
& (kstar(k).eq.6))))then
* Ivanova & Taam (2002) method
if(ospin(k).le.wx) djmb = kw3 * rad(k)**4.0d0 *
& (ospin(k)/wsun)**3.0d0
if(ospin(k).gt.wx) djmb = kw3 * rad(k)**4.0d0 *
& (ospin(k)/wsun)**1.3d0 * (wx/wsun)**1.7d0
djspint(k) = djspint(k) + djmb
endif
endif
* Limit to a 3% angular momentum change for the star owing to MB.
* This is found to work best with the maximum iteration of 20000,
* i.e. does not create an excessive number of iterations, while not
* affecting the evolution outcome when compared with a 2% restriction.
*
if(djmb.gt.tiny)then
dtj = 0.03d0*jspin(k)/ABS(djmb)
dt = MIN(dt,dtj)
if(output) write(*,*)'mb1:',tphys,dt,djmb,djt
endif
*
if(kstar(k).eq.13.and.pulsar.gt.0)then
*
* NS(pulsar) magnetic braking. PK.
* No contact binary NS system.
*
if(bdecayfac.eq.0)then
if(B_0(k).eq.0.d0)then
B(k) = 0.d0
elseif((tphys-epoch(k)-tacc(k)).lt.tiny)then
B(k) = B_0(k)*exp(-CK*bacc(k)) + Bbot
else
B(k) = B_0(k)*
& EXP(-(tphys-epoch(k)-tacc(k))/bconst)*
& exp(-CK*bacc(k)) + Bbot
endif
else
if(B_0(k).eq.0.d0)then
B(k) = 0.d0
elseif((tphys-epoch(k)-tacc(k)).lt.tiny.and.
& bacc(k).eq.0.d0)then
B(k) = B_0(k) + Bbot
elseif((tphys-epoch(k)-tacc(k)).lt.tiny)then
B(k) = B_0(k)/(1.d0 + (bacc(k)/1.0d-6)) + Bbot
elseif(bacc(k).eq.0.d0)then
B(k) = B_0(k)*EXP(-(tphys-epoch(k)-tacc(k))/bconst)
& + Bbot
else
B(k) = B_0(k)*
& EXP(-(tphys-epoch(k)-tacc(k))/bconst)/
& (1.d0 + (bacc(k)/1.0d-6)) + Bbot
endif
endif
omdot = Kconst*B(k)*B(k)*ospin(k)**3
djmb = 0.4d0*mass(k)*rad(k)*rad(k)*omdot
djspint(k) = djspint(k) + djmb
if(output) write(*,*)'502 2:',k,djspint(k),djmb
if(djmb.gt.tiny)then
dtj = 0.1d0*(jspin(k)/ABS(djmb))
dt = MIN(dt,dtj)
endif
endif
*
* Calculate circularization, orbital shrinkage and spin up.
*
dspint(k) = 0.d0
if(((kstar(k).le.9.and.rad(k).ge.0.01d0*rol(k)).or.
& (kstar(k).ge.10.and.k.eq.j1)).and.tflag.gt.0)then
*
raa2 = (rad(k)/sep)**2
raa6 = raa2**3
*
* Hut's polynomials.
*
f5 = 1.d0+ecc2*(3.d0+ecc2*0.375d0)
f4 = 1.d0+ecc2*(1.5d0+ecc2*0.125d0)
f3 = 1.d0+ecc2*(3.75d0+ecc2*(1.875d0+ecc2*7.8125d-02))
f2 = 1.d0+ecc2*(7.5d0+ecc2*(5.625d0+ecc2*0.3125d0))
f1 = 1.d0+ecc2*(15.5d0+ecc2*(31.875d0+ecc2*(11.5625d0
& +ecc2*0.390625d0)))
*
if(ST_cr.le.0.and.
& ((kstar(k).eq.1.and.mass(k).ge.1.25d0).or.
& kstar(k).eq.4.or.kstar(k).eq.7))then
*
* Radiative damping (Zahn, 1977, A&A, 57, 383 and 1975, A&A, 41, 329).
*
tc = 1.592d-09*(mass(k)**2.84d0)
f = 1.9782d+04*SQRT((mass(k)*rad(k)*rad(k))/sep**5)*
& tc*(1.d0+q(3-k))**(5.d0/6.d0)
tcqr = f*q(3-k)*raa6
rg2 = k2str(k)
elseif(ST_cr.gt.0.and.
& ((kstar(k).le.1.and.mass(k).gt.convradcomp(k)).or.
& (kstar(k).eq.2.and.teff(k).gt.convradcomp(k)).or.
& (kstar(k).eq.4.and.teff(k).gt.convradcomp(k)).or.
& (kstar(k).eq.9.and.mass(k).gt.convradcomp(k)).or.
& (kstar(k).eq.7).or.(kstar(k).eq.8)))then
*
* Radiative damping (Zahn, 1977, A&A, 57, 383 and 1975, A&A, 41, 329).
*
tc = 1.592d-09*(mass(k)**2.84d0)
f = 1.9782d+04*SQRT((mass(k)*rad(k)*rad(k))/sep**5)*
& tc*(1.d0+q(3-k))**(5.d0/6.d0)
tcqr = f*q(3-k)*raa6
rg2 = k2str(k) !for startrack comparison this should be =0.31622777d0 (sqrt(0.1)).
elseif(kstar(k).le.9)then
*
* Convective damping (Hut, 1981, A&A, 99, 126).
*
* In BSE paper Equation 30, the default scaling coefficient is 2./21
* the fprimc_array kstar dependent array that is fed in
* keeps this same coefficient by default but allows user to
* specify their own
*
tc = mr23yr*(menv(k)*renv(k)*(rad(k)-0.5d0*renv(k))/
& (3.d0*lumin(k)))**(1.d0/3.d0)
ttid = twopi/(1.0d-10 + ABS(oorb - ospin(k)))
f = MIN(1.d0,(ttid/(2.d0*tc))**2)
!kstar(k) to kstar(k)+1 by PA for kstar(k)=0
tcqr = fprimc_array(kstar(k)+1)*
& f*q(3-k)*raa6*menv(k)/
& (tc*mass(k))
rg2 = (k2str(k)*(mass(k)-massc(k)))/mass(k)
elseif(ST_tide.le.0)then
*
* Degenerate damping (Campbell, 1984, MNRAS, 207, 433)
*
f = 7.33d-09*(lumin(k)/mass(k))**(5.d0/7.d0)
tcqr = f*q(3-k)*q(3-k)*raa2*raa2/(1.d0+q(3-k))
rg2 = k3
endif
*
* Circularization.
*
sqome3 = sqome2**3
delet1 = 27.d0*tcqr*(1.d0+q(3-k))*raa2*(ecc/sqome2**13)*
& (f3 - (11.d0/18.d0)*sqome3*f4*ospin(k)/oorb)
tcirc = ecc/(ABS(delet1) + 1.0d-20)
delet = delet + delet1
*
* Spin up of star.
*
dspint(k) = (3.d0*q(3-k)*tcqr/(rg2*omecc2**6))*
& (f2*oorb - sqome3*f5*ospin(k))
if(output) write(*,*)'502 3:',k,dspint(k),tcqr
*
* Calculate the equilibrium spin at which no angular momentum
* can be transferred.
*
eqspin = oorb*f2/(sqome3*f5)
*
* Calculate angular momentum change for the star owing to tides.
*
djt = (k2str(k)*(mass(k)-massc(k))*rad(k)*rad(k) +
& k3*massc(k)*radc(k)*radc(k))*dspint(k)
if(kstar(k).le.6.or.ABS(djt)/jspin(k).gt.0.1d0)then
djtt = djtt + djt
endif
endif
502 continue
*
* Limit to 2% orbital angular momentum change.
*
djtt = djtt + djorb
if(ABS(djtt).gt.tiny)then
dtj = 0.02d0*jorb/ABS(djtt)
dt = MIN(dt,dtj)
endif
dtm = dt/1.0d+06
if(output) write(*,*)'bin lim orb ang mom:',tphys,dt,kstar(1)
*
elseif(ABS(dtm).gt.tiny.and.sgl)then
do 503 , k = kmin,kmax
!check for kstar added by PA
if(neta.gt.tiny .and. kstar(k)<15)then
rlperi = 0.d0
dmr(k) = mlwind(kstar(k),lumin(k),rad(k),mass(k),
& massc(k),rlperi,z)
else
dmr(k) = 0.d0
endif
dmt(k) = 0.d0
djspint(k) = (2.d0/3.d0)*dmr(k)*rad(k)*rad(k)*ospin(k)
if(output) write(*,*)'503 1:',k,djspint(k)
*
* Evaluate convective/radiative limits for a variety of stars as based
* on the work of Belczynski et al. (2008). As option.
* Note only certain stars of type k = 0, 1, 2, 4, 5, 6, 9 **double check
* 0, 1 have range of 0.35-Mms,conv. Mms,conv is function of metalicity.
* 2 & 4 have a temperature dependence. Convective if Teff < 10**3.73
* 3, 5 & 6 are giants and have no radiative envelopes.
* 9's envelope is convective when M < Mhe,conv, Mhe,conv = 3.0Msun.
*
if(ST_cr.le.0)then
if(kstar(k).le.1)then
convradcomp(k) = 1.25d0
else
convradcomp(k) = 99999999.d0
endif
else
if(kstar(k).le.1)then
* Main sequence mass limit varying with metallicity
convradcomp(k) = 1.25d0
if(z.gt.0.001d0.and.z.lt.zsun)then
convradcomp(k) = 0.747d0 + 55.73d0*z - 1532*z*z
elseif(z.le.0.001d0)then
convradcomp(k) = 0.8d0
endif
elseif(kstar(k).eq.2.or.kstar(k).eq.4)then
* H-rich HG and CHeB temperature limit
convradcomp(k) = 10.d0**3.73d0
elseif(kstar(k).le.6)then
* No limit or all other giant stars
* (compare this large value to mass).
convradcomp(k) = 99999999.d0
elseif(kstar(k).eq.9)then
* Mass limit for evolved He star
convradcomp(k) = 3.d0
endif
endif
* if(mass(k).gt.0.35d0.and.kstar(k).lt.10)then
* djmb = 5.83d-16*menv(k)*(rad(k)*ospin(k))**3/mass(k)
* djspint(k) = djspint(k) + djmb
* if(mass(k).gt.0.35d0.and.kstar(k).lt.10.and.
* & menv(k).gt.0.0d0)then
* if (ospin(k) .le. wx) djmb = kw3 * rad(k)**4.0d0 *
* & (ospin(k)/wsun)**3.0d0
* if (ospin(k) .gt. wx) djmb = kw3 * rad(k)**4.0d0 *
* & (ospin(k)/wsun)**1.3d0 * (wx/wsun)**1.7d0
* djspint(k) = djspint(k) + djmb
*
*MB
djmb = 0.d0
if(htpmb.eq.0)then
if(mass(k).gt.0.35d0.and.kstar(k).lt.10)then
djmb = 5.83d-16*menv(k)*(rad(k)*ospin(k))**3/mass(k)
djspint(k) = djspint(k) + djmb
endif
elseif(htpmb.eq.1)then
if(ST_cr.le.0.and.
& mass(k).gt.0.35d0.and.kstar(k).lt.10.and.
& menv(k).gt.0.0d0)then
* Old BSE convective/radiative divide...
if(ospin(k).le.wx) djmb = kw3 * rad(k)**4.0d0 *
& (ospin(k)/wsun)**3.0d0
if(ospin(k).gt.wx) djmb = kw3 * rad(k)**4.0d0 *
& (ospin(k)/wsun)**1.3d0 * (wx/wsun)**1.7d0
djspint(k) = djspint(k) + djmb
elseif(ST_cr.gt.0.and.(menv(k).gt.0.d0.and.
& ((kstar(k).le.1.and.mass(k).gt.0.35d0.and.
& mass(k).le.convradcomp(k)).or.
& (kstar(k).eq.2.and.teff(k).le.convradcomp(k)).or.
& (kstar(k).eq.4.and.teff(k).le.convradcomp(k)).or.
& ((kstar(k).eq.3).or.(kstar(k).eq.5).or.
& (kstar(k).eq.6)))))then
* MB given in Ivanova & Taam (2002)
* if(mass(k).gt.0.35d0.and.kstar(k).lt.10.and.
* & menv(k).gt.0.0d0)then
if(ospin(k).le.wx) djmb = kw3 * rad(k)**4.0d0 *