_regexp = """

replace-regexp
\.parm('\([a-z0-9]+\)', *\([-+0-9.eEdD]+\))
.p.\1 = \2


p \([a-z0-9]+\) \([-+0-9.eEdD]+\) *$
        gen.p.\1 = \2
<F5>
"""

_doc = """
c This is a KEPLER generator file.  This generates the initial model, defines
c various variables, configures various parameters, and provides a set of
c commands for KEPLER to execute.  I've attempted to comment all of this below.

c --- Network cards ---
c KEPLER has an in-built APPROX19 network (this is the origin of Frank's various
c approx networks).  You set the initial network to be APPROX by choosing net 1.
c As I understand it, you can currently only select network 1 (APPROX), though
c other networks are defined and can be configured to "turn on" later, such as
c an NSE (NETNUM = 3) network and an ISE (NETNUM = 2, a QSE net) network.

c Note that the large adaptive network is run in a co-processing fashion, such
c that isotope compositions and related quantities are mapped back and forth
c between a large network calculation and the simpler APPROX19 calculation.  You
c _do_ get energy generation and such from the adaptive network with the proper
c parameters, so you can effectively run with the large network as "the"
c network, but for legacy reasons will still need to define APPROX19 here and the
c larger network with a "bg" BURN generator.

c These net cards define the isotopes carried by the network.  Though this
c presents as a user option, Alex advises that you must define the APPROX19
c network as it has been made into a hard-coded assumption in various parts of
c the code.  So in practice, all modern Kepler generators will have the
c following set of net cards.
net 1 h1 he3 he4 n14 c12 o16 ne20 mg24
net 1 si28 s32 ar36 ca40 ti44 cr48 fe52
net 1 ni56 fe54 pn1 nt1

c --- Mixture cards ---
c Mixture cards allow you to define compositions that can then be used in other
c cards to specify the chemical composition at different regions in the grid.

c This composition is a proxy for the deeper part of the NS ocean, and is meant
c to just be a sink for heat.  We achieve this with an iron 54 substrate.
m nstar 1.00 fe54

c He star abundance references
c m acret 1.0 he4 0.0 c12 0.0 o16
c m acret 0.3 he4 0.2 c12 0.5 o16
c m acret 0. h1 0.980 he4 0. c12 0.02 n14 0. o16
c H star abundance references
c m acret 0.759 h1 0.24 he4 0.001 n14

c Here we define the composition of material accreted from the companion
m acret 0.73 h1 0.250 he4 0.02 n14

c --- Grid cards ---
c Grid cards define the initial 1D grid of mass zones, and make use of mixture
c cards.  These are the cards you use to define the initial resolution.  Not every
c zone needs to be specified.  Intermediate zones will have their data
c interpolated (not sure exactly in what form) from provided grid zones.  You must
c always define grid point 0 and the final grid point (which defines the initial
c resolution).

c c Reference: THIS GRID FOR HE ACCRETION
c g 0   2.0000e25  1 nstar  4.0e+8  1.0e+9
c g 1   1.9000e25  1 nstar  4.0e+8  1.0e+9
c g 40  1.0000e22  1 nstar  4.0e+8  1.0e+8
c g 50  1.0000e21  1 nstar  4.0e+8  1.0e+8
c g 51  8.0000e20  1 acret  2.0e+8  1.0e+8
c g 54  2.0000e20  1 acret  1.0e+8  1.0e+6
c g 55  0.         1 acret  5.0e+7  1.0e+4
c p bmasslow 2.800000019998950D33

c Reference: THIS GRID IS FOR H-RICH ACCRETION
c See docs for more details on grid card definitions.
c Zone# mass(g)    net mix    temp (K) rho (g/cc)
g 0     2.0000e25  1   nstar  1.0e+8   1.0e+9
g 1     1.9000e25  1   nstar  1.0e+8   1.0e+9
g 40    1.0000e21  1   nstar  1.0e+8   1.0e+6
g 50    1.0000e20  1   nstar  1.0e+8   1.0e+6
g 51    8.0000e19  1   acret  5.0e+7   1.0e+6
g 54    2.0000e19  1   acret  2.5e+7   1.0e+8
g 55    0.         1   acret  1.1e+7   1.0e+4

c --- Parameter cards ---
c Now we set various parameters configuring how Kepler will run.
c These can be found in the docs.

c - I/O, Graphics, and Termination Conditions -
c nedit: Number of cycles between "ASCII edits" (I think this means how often
c data is output to files)
p nedit 100000

c ndump: Number of cycles between restart dumps
p ndump 10

c irtype: x-axis type for plots
c 1 -> radius in cm
c 2 -> interior mass fraction, q
c 3 -> interior mass in M_sol
c 4 -> radius in cm
c 5 -> moment of inertia coordinate (Msun*Rsun**2)
c 6 -> zone #
c ... several more options, up to 26, see docs
c (Note: this provided generator had two instances of this, the second used to
c be further down but I don't think that matters)
p irtype 6
p irtype 4

c nsdump: Save every nsdump restart dumps
p nsdump 10

c iwinsize: Size of graphics window to be created in the form xxxxyyyy, where
c xxxx, yyyy = (width, height) in pixels.  Must use leading 0's.
p iwinsize 14001000

c ncycqq: Number of KEPLER cycles between post-processor dump cycles
p ncycqq 100000

c npixedit: Graphics edits to the monitor are made every npixedit KEPLER cycles
p npixedit 1

c h1hdep: Central hydrogen abundance at which the #hdep dump is made
p h1hdep -1.d0

c he4hedep: Central helium abundance at which the #hedep dump is made
p he4hedep -1.d0

c si28dep: Central si28 mass fraction at which the #sidep dump is made, if the
c mass fractions of o16 and he4 are below 0.01
p si28dep -1.d0

c iplotb: Control isotope/network used in abundance plots
c 0 -> Use APPROX/ISE/NSE abundances
c 1 -> Only plot BURN abundances in APPROX regime
c 2 -> Plot BURN abundances everywhere BURN is used (above bmasslow p# 419)
c 3 -> Plot BURN abundances everywhere
p iplotb 2

c jp0: Innermost zone to plot
p jp0 40

c lcout: Number of outer layers to be written in light curve output file, .lc
c 0 means write no file
p lcout 10

c ncnvout: Write out convection plot file data (*.cnv) every ncnvout cycles.
c Off when 0 (but I don't see these files, is this still working?)
p ncnvout 1

c abunlim: Least elemental mass fraction plotted or listed in a term ion edit
p abunlim 1.d-4

c no h/he burn dumps
c h1hburn: Hydrogen mass fraction at which to make the #hburn dump
p h1hburn -1.
c he4heburn: Helium mass fraction at which to make the #heburn dump
p he4hebrn -1.


c - Gridding and Boundaries -
c dstat says to take the specified initial grid configuration and adjust it to
c be in HSE via modifications of the density.  Docs say this is useful for
c degenerate cases like WD and NS, but I don't see why it wouldn't be useful in
c general.  Don't you always want HSE for stars?
dstat

c radius0: radius of inner boundary (cm)
p radius0 1.0e+06

c summ0: Mass inside inner boundary (g)
p summ0 2.8e+33

c xlum0: luminosity emerging from inner surface (erg/s)
p xlum0 1.6e+34

c dnrtmax: Maximum fractional density change allowed between zones before adzoning
p dnratmax .25

c rnmin: Minimum radius for which adzoning is considered (cm)
p rnmin 1.e+6

c tnmin: Minimum temperature for which adzoning is considered (K)
c (adzoning vs rezoning vs dezoning?)
p tnmin 1.e+4

c dnmin: Minimum density for which adzoning is considered
p dnmin 2.e-5

c izonef: Rezoning flag. izonef <= 0: no rezoning
p izonef 0

c idzonef: Dezoning flag. idzonef <= 0: no dezoning
p idzonef 0

c rnmax: Maximum radius for which rezoning is considered
p rnmax 1.e+14

c fracrz1: Multiplier in the effective values of the density, temperature, and
c radius gradients used to determine the necessity for adzoning or dezoning.
c This is a bound in a set of ranges used to determine the multiplicative
c factor.  See docs for details.
p fracrz1 .33

c fracrz2: See fracrz1 above and relevant docs section
p fracrz2 .5

c abarratm: Used for determining rezoning based on abar.  See abarrat0 and docs.
p abarratm 1.3

c fmax0: Adzone mass fraction parameter.
c See table in docs and related parameters (fmaxm, fmax1, fmaxcrz0, etc)
p fmax0 .01

c fmax1: See fmax0 and docs, has to do with adzoning on mass fraction ranges
p fmax1 .015

c fmax2: See fmax0 and docs, has to do with adzoning on mass fraction ranges
p fmax2 .03

c accrate: Rate at which mass in the form of new zones is added to the surface
c of the star (Msun/yr).
c
c The accumulated mass is stored in xmacrete (p# 212) until it is large enough
c to be added as a whole zone. The surface boundary pressure is gradually
c increased at a rate proportional to accrate until a mass (in xmacrete
c (p# 212)) equal to that in the current outer zone is reached. Then a new zone, the
c mirror image of the old outer zone, is added. Accretion composition is set by
c the compsurf command in TTYCOM. The boundary pressure from the accretion phantom
c is stored in pboundac (q# 96).
c
c Note: This prescription will work best for coarse and roughly equal surface zoning.
c
c Negative accretion rate means to read in time-dependent accretion rate data
c from file nameprob.acc. The file contains a comment line with version
c information, then a line with the number of entries ((I6)), then the data in two
c columns: time in seconds and accretion rate in grams per second. Format:
c (2E25.17). The resulting rate is multiplied by accrate to allow
c scaling without having to change the file. See also: accratef (p# 550) which
c seems to duplicate the scaling functionality.
p accrate 1.75d-9

c minzone: Do not rezone the innermost minzone zones
c minzone = 0 allows rezoning innermost zone
p minzone 51

c zonemmin: Minimum mass that a pair of zone may have and still be allowed to
c be adzoned
p zonemmin 1.5d19

c zonemmax: Do not dezone zones bigger than zonemmax
p zonemmax 1.d20







c - Convection -
c fracneut: If the semi convective test parameter, W, is < 0 but greater than
c -fracneut * abs(log(T1/T0)), then the zonal interface is flagged
c convectively neutral (?NEUT? or ?,?).
p fracneut .05

c dtsmult: The fractional amount of semi-convective mixing that can occur in
c one timestep is limited to approximately dtsmult
p dtsmult 1.e+99

c frcsound: Don't do convection if the absolute value of the zone velocity
c exceeds frcsound times the local sound speed.
c (Note: this provided generator had two instances of this, the second used to
c be further down but I don't think that matters)
p frcsound .0
p frcsound 1.

c convlim: Limit the convective velocity to a fraction convlim of the local sound speed
c (Note: this provided generator had two instances of this, the second used to
c be further down but I don't think that matters)
p convlim .0
p convlim 1.

c woversht: The semiconvective test parameter, W, is taken to be
c W = woversht * abs ( log (T1/T0)) for the special overshoot semiconvective
c zones where W would otherwise be < 0 and when Abar >= abarsemi (p# 324).
c If 0, no overshoot mixing.
p woversht 0.

c alpth: Efficiency factor for thermohaline convection
c If set to zero no thermohaline convection is considered. Thermohaline
c convections occurs in regions with destabilizing composition gradient, but
c stabilizing temperature gradient (salt finger instability).
c The implementation in KEPLER is according to Braun (1997, PhD thesis) and
c Kippenhahn et al. (1980)
c p alpth 0.


c - Microphysics -
c Below this mass coordinate, burn co-processing is turned off.
c (won't it always be off then?  All grid points are below this)
p bmasslow 2.800000019999895D33

c This specifies the BURN generator file's name.  See rpabg for the
c co-processing network's specification.
genburn rpabg

c Map the BURN abundances to the APPROX network.  This should overwrite any
c previously specified APPROX abundances, e.g. from the g cards.  In other
c words, the composition specified in rpabg takes precedence.
mapburn

c xkimt: Multiplier on IBEN1 opacity (why this value? what's IBEN opacity?)
c p xk1mt 1.5284

c xk2mt: Multiplier on IBEN2 opacity (why this value?)
c p xk2mt 1.5284

c xk3mt: Multiplier on Christy opacity (why this value?)
c p xk3mt 1.5284

c xk4mt: Multiplier on Compton opacity (why this value?)
c p xk4mt 1.5284

c rxkcmt: Multiplier on conductive opacity (why this value?)
c p rxkcmt 1.5284

c t7peek: Opacity will be no larger than xkmin (p# 50) + t7peek * rho * (T_7)**4
p t7peek 1.e+50

c tnucmin: Don't calculate nuclear burning in APPROX if the temperature is less
c than tnucmin
c NOTE: Unless the hydrogen burning rate is significant, no APPROX network
c calculations will be done below 1.e+7 K, even if tnucmin < 1.e+7 K
c (Note: this provided generator had two instances of this, the second used to
c be further down but I don't think that matters)
p tnucmin 1.0e+99
p tnucmin 1.d7

c jshell0: Innermost zone in which there is neutrino deposition (??)
p jshell0 51

c tqsemin: Floor on the temperature used in the ISE (aka QSE) calculation
p tqsemin 3.e+9

c siqselim: A sufficient condition to change a zone from the ISE to the NSE
c network is for the sum of the silicon and sulphur "group" elemental mass
c fractions to be less than or equal to siqselim
p siqselim .02

c wilsonmt: Docs warn caution when using this.
c Multiplier on the Wilson-based nuclear EOS (except for thee thermal ion
c component) if it is >= 0. Otherwise, the old non-relativistic, partial
c degeneracy model for the ion EOS is used.
p wilsonmt -1.

c iold: Set to value other than 0 to use old physics - mostly fix that energy
c generation in APPROX did not include neutrino losses and mass excess but only
c considered differences in binding energy.
c 0 -> use current physics
c 1 -> no nu loss in H burning and BE instead of ME and old nu loss routines
c      (old1/old2, < 1997)
c other options (2,4,8, see docs)
p iold 1

c kaptab: Select opacity table
c 0 -> old (??)
p kaptab 0

c btempmin: BURN co-processing is skipped if a zone's temperature is less than
c btempmin
c (Note: this provided generator had two instances of this, the second used to
c be further down but I don't think that matters)
p btempmin 1.1e8
p btempmin 1.d7

c mazful: Use Fuller et. al.'s weak rates in the BURN coprocessor
c if mazful = 1, otherwise use the old rates of Mazurek and Hansen
p mazful -1

c lburn: Substitute BURN network for APPROX network (including energy
c generation, Abar, Zbar, etc) when set to 1.
c Abundances are mapped to APPROX abundances for plot/edit purposes only
p lburn 1

c nadapb: Enable Adaptive BURN network adjustment
c 0 -> off
c 1 -> on
p nadapb 1


c - Numerical Parameters -
c dtnew: Initial timestep (sec)
p dtnew 1.e-4

c maxit: Maximum iterations on R, T, L (radius, temp, luminosity?) before retrying with smaller dt
p maxit 40

c dtcr: Maximum desired fractional change in radius per step
p dtcr .05

c dtct: Maximum desired fractional change in temperature per step
p dtct .05

c dtcd: Maximum desired fractional change in density per step
p dtcd .10

c dtcq: Maximum desired fractional linear contraction per step
p dtcq .1

c dtcdt: Maximum fractional change in timestep per step
p dtcdt .99

c nstop: Maximum number of cycles (cycles, same as steps?)
p nstop 1000000

c ipup: abundance update parameter. ipup=2 means don't update abundances in
c zones less than jshell0 (p# 93), the innermost zone with neutrino deposition.
p ipup 2

c dyemult: If iytsflag (p# 67) (has to do with ISE zones) >= 1, increase the
c timestep sensitivity to changes in ye by a factor of dyemult
p dyemult 50.

c dyqmult: If iytsflag (p# 67) >= 1, increase the timestep sensitivity to changes in yq
c by a factor of dyqmult
p dyqmult 2.

c dtcp: Maximum desired fractional change in abundances per step.
p dtcp .15

c yfloorx: Minimum elemental mass fraction that effects the timestep (I guess
c for the various restrictions on fractional change?)
p yfloorx 3.e-3

c cenu: velocity centering parameter. cenu=0.5 is exact energy conservation,
c cenu=1.0 is most stable.  A note in the docs says Kepler only behaves well for
c cenu=1.0, so modifying it requires some understanding of what you're doing.
p cenu 1.

c dtcut: Fractional timestep reduction when a step is redone
p dtcut .1

c tfcrbu: If the maximum fractional change in radius during a timestep exceeds
c tfcrbu * dtcr (p# 6), then redo step
p tfcrbu 2.

c tfctbu: If the maximum fractional change in temperature during a timestep
c exceeds tfctbu * dtct (p# 7), then redo step
p tfctbu 10.

c fclmax: Maximum allowed relative convergence error in luminosity
c (wtf is this so huge?)
p fclmax 1.e+99

c fclbu: Reduce timestep by dtcut (p# 53) and redo step if convergence error in
c luminosity is still greater than fclbu after maxit (p# 5) iterations
p fclbu 1.e+99

c iautoout: This is said to be deprecated parameter for crays in docs, but not
c sure why it's set to 5 here.  Should ask Alex.
p iautoout 5

c iflgabar: Another deprecated parameter.  Should be 0.  For reference:
c The mean atomic weight, Abar, calculated in subroutine sdot is implicitly
c coupled to the ion equation of state only if iflgabar /= 0 and the normal
c APPROX network is being used.
p iflgabar 0

c yfloorbx: Elemental mass fraction floor for making abundance backups
c (See abunminx (p# 204)).
p yfloorbx .003

c fcrmax: Maximum allowed relative convergence error in radius
p fcrmax 1.d-8

c fctmax: Maximum allowed relative convergence error in temperature
p fctmax 1.d-8


c=======================================================================
c Now follows the command file
c=======================================================================
//*
c ------- PARAMETERS --------
c .... accretion rate 1.75D-8 (L/Ledd) * 1.7/(X + 1)
p accrate 1.75D-8
c .... substrate luminosity - accrate * 6.0816737e+43 * (Q/MeV)
c .... 1.0642929e+36 (L/Ledd) * (Q/MeV)
p xlum0   1.0642929e+36
c -------------------------
c ..... SCALE to He/C/O L_Edd accretion: factor 1.7 / (X + 1)
o x {isoh1(jm)} def
o xeddf {1.7 / (1.0 + x)} def
p accrate {xeddf} *
p xlum0 {xeddf} *
c .......
c substrate Luminosity, Q/MeV
p xlum0 0.75 *
c .......
c set fraction of Eddington accretion rate
o xledd 0.02 def
p accrate {xledd} *
p xlum0 {xledd} *
c -------------------------
c get model in equilibrium
p ncnvout 0
p nstop 1000000000
p tnucmin 1.d10
p tnumin 1.d7
p accmass 1.d13
p optconv 0.67
p iaccadv 0
p iacceadv 1
c for APPROX ONLY
p jp0 0
p irtype 4
plot
c =========================
c MATCH TO accmass - set mass of outer zone
@xm(jm)<1.01d17
p maxbak 20
p accdepth 1.d99
p iterbarm 999999
c =========================
@time>1.d17
zerotime
p toffset 0.
setcycle 0
cutbin
c --- time-dependent accretion rate only ---
c resetacc
c p accrate -1.
c ------------------------------------------
p lburn 1
p dtnew 1.
p iaccadv 1
c use accdepth 5.d20 for He
c use accdepth 1.d20 for H
c values above may be good for 0.1 Ledd,
c but require scaling for lower accretion rates or more heating
p accdepth 1.d20
p tnucmin 1.d7
p izonef 1
p idzonef 1
p iazonef 0
p zonermax 10.
p zonemmax 1.d99
p ddmin 1.d4
c --- decretion ---
p decrate -1.D0
p idecmode 1
p jshell0 0
p ipup 5
c --- use y coordinate for zoning ---
c p fmax0 1.
c p fmax1 1.
c p fmax2 1.
c p zonemmax 1.d99
c p zonermax 1.d99
c p zoneymax 0.02
c
c --- some other stuff ---
c boundary pressue
c p pbound 5.d18
c use 10% mass of outer zone
p pbound {6.67259e-8 * zm(0) * xm(0) / (4. * 3.14159 * rn(0) ^ 4 ) * 0.1}
c
c --- rotation ---
c p centmult .667
c 600 Hz rotation?
c p angjacc 2.51327d15
c p nangdis 1
c p magnet 8
c p xmagfbr 1.d-10
c p xmagfbt 1.d-5
c
c --- plotting ---
c p ipixtype 31700
p irtype 11
c
c --- output ---
p ibwarn 0
c
c --- termination condition ---
c @time>8.E+05
c end
"""