1 get following to work
0 document this problem with molecules - time dependent
2 change the name of this routine to reflect the fact that it is entirely induced.
2 How should these affect locally emitted continuum calculated in rtdiffuse? Just subtract these rates from the emitted ones?
2 test on c checks whether collisions are possible at this temperature, should add photo excitation
2 these pops ARE NOT defined below
2 following needed to get badbugs/bug8.in to work
2 following needed to get badbugs/bug5.in to work
2 do something with this or set to LONG_MAX? after moving collapsed levels to iso.nCollapsed_max, this variable does nothing. iso.nTopOff[ipHE_LIKE] = 0;
2 Change this to higher number. Make this change by itself after all other changes pass suite.
1 update ct to Kimura et al. (1996)
1 above rate not intended for very low temperatures - find ref for low-T rate, probably is 1e-9 like above
0 these should be values at 1e5 K
2 not currently used - include as deexcitation process
2 this is redundant with contents of oxygen line arrays use them instead when removing this, make sure all line intensity predictions also go into oi line arrays
2 what are we trying to print here?
2 this assert is not passed if error made much smaller. This error should be related to a check on convergence of the molecular networks and their sum rules, with a criteria used here and there
0 PvH prefers test against err/10
2 add term for protons from Rouef, E., & Le Bourlot, J. 1990, A&A, 236, 515
1 add neutral helium Staemmler, V., & Flower, D. R. 1991, J. Phys. B, 24, 2343
3 change to atom_level3
2 - ground term is actually a fix level system, the vectors are created, with pointers ipFe1_54m , ipFe1_111m, must add collision date, use larger model atom
2 following to stop insane FeX strengths >>chng 96 jul 11, removed 1 / 10 factor, so using real data, 90.01 cs = cs * 0.1 >>chng 96 jun 03, transferred following >>chng 97 jan 31, I give up on this mess, use cs of unity
2 update atomic data to Chidichimo et al 1999 AASup 137, 175
2 * following not in cooling function
2 use atom_level3
1 update cs these to following reference: >>refer n2 cs Hudson, C.E. & Bell, K.L. 2004, MNRAS, 348, 1275 and A&A, 430, 725 they agree with Lennon & Burke
2 add proper temperature dependence when good coll strength calculations become available
2 put all these in cooling
2 - insert reference
2 - this check may also too liberal.
2 this should be setable at run time as per Robin Williams email rshock = 4e16;
2 Switch to supersonic when bad enough failure for STRONGD -- need to improve this logic when the p(rho) data is cleaner
2 this algorithm might be more efficient with Brent
2 should collisional heating/cooling be included here?
2 use something like log(ThermRatio) + log(delta) ????
2 this algorithm might be more efficient with Brent
2 a self-consistent treatment for the heating by Auger electrons should be used
2 a self-consistent treatment for the heating by Compton recoil electrons should be used
2 note that the number of primary electrons is given by yhat, which may not be one, so this is not necessarily consistent
2 avAuger depends on grain charge, this should be treated explicitly here
0 get better relationship between cr excit of Lya rate
2 - put H2Lines in outward beams in RT_diffuse
2 put supra thermal excitation into excitation of electronic bands
1 add part of hard heat to secondaries
2 find correct high-energy limit for these
2 this is part of the induce 2nu problem, which must be fixed for both he and h sequences.
2 - this structure is currently only used for helium itself... stuff numbers in for other elements, or drop the [nelem] dimension off of helike.HeCS
2 This routine, like the above one, needs to use proper energy.
2 sometimes rate is negative...is that okay?
2 following always true, why? either remove test or use it - it is here to save time - this step routine is called very often
2 this should be done with new populations after converged soln
2 - put in actual composition dependent Tad - this is only valid for bare surfaces - not ice - for ice Tad is 555K hmi.Tad is binding energy expressed as a temperature note that hmi.Tad is set to 800. in zero tau_nu the first equation in section 2.5 equation one paragraph before equation 2 at low grain temperatures all end in para, J=0
1 equivalent reaction for H2* is not included in chemistry, Big h2 does not include this reaction, what to do? GS
1 equivalent reaction for H2* is not included in chemistry, Big h2 does not include this reaction, what to do? GS
2 process is net source term for H(n=3) states, must be added in
2 process is net ionization term for H(n=3) states
1 equivalent reaction for H2* is not included in chemistry, Big h2 does not include this reaction, what to do? GS
1 equivalent reaction for H2* is not included in chemistry, Big h2 does not include this reaction, what to do? GS
1 equivalent reaction for H2* is not included in chemistry, Big h2 does not include this reaction, what to do? GS
1 equivalent reaction for H2* is not included in chemistry, Big h2 does not include this reaction, what to do? GS
1 equivalent reaction for H2* is not included in chemistry, Big h2 does not include this reaction, what to do? GS
0 update photoelectric opacity for H2 to include real cross sections and energies. this is not a higher priority because when H2 is formed there can be very little ionizing radiation. this process must be trivial compared with the Solomon process following reference gives cross section for all energies >>refer H2 photo cs Yan, M., Sadeghpour, H.R., & Dalgarno, A., 1998, ApJ, 496, 1044 Wilms, J., Allen, A., & McCray, R. 2000, ApJ, 542, 914
0 must include heating, Compton ionization
1 equivalent reaction for H2* is not included in chemistry, Big h2 does not include this reaction, what to do? GS
1 equivalent reaction for H2* is not included in chemistry, Big h2 does not include this reaction, what to do? reverse of this reaction i not in detailed balance,why? GS
2 this rate drives numerical instability in such models as secondary1 and 2.in
1 equivalent reaction for H2* is not included in chemistry, Big h2 does not include this reaction, what to do? GS
1 equivalent reaction for H2* is not included in chemistry, Big h2 does not include this reaction, what to do? GS
2 equivalent reaction for H2* is not included in chemistry, Big h2 does not include this reaction, what to do? GS
2 equivalent reaction for H2* is not included in chemistry, Big h2 does not include this reaction, what to do? GS
1 equivalent reaction for H2* is not included in chemistry, Big h2 does not include this reaction, what to do? GS
2 must add process H2+ + H- => H2 + H, Dalgarno&Lepp 87
2 put in H2+ + gamma => H + H+
1 equivalent reaction for H2* is not included in chemistry, Big h2 does not include this reaction, what to do? GS
2 equivalent reaction for H2* is not included in chemistry, Big h2 does not include this reaction, what to do? GS
2 equivalent reaction for H2* is not included in chemistry, Big h2 does not include this reaction, what to do? GS
2 equivalent reaction for H2* is not included in chemistry, Big h2 does not include this reaction, what to do? GS
2 equivalent reaction for H2* is not included in chemistry, Big h2 does not include this reaction, what to do? GS
0 had to comment following test out - NA change to hmole caused massive prints
2 - if pc lint ever fixes this bug in their product, remove this -e
2 this routine dumps all heating and cooling into only a very few lables, it would be best to break these out into individual labels that show element, iso sequence, and agent
1 this does not belong here - should be where radius incremnted
2 put this line back in! EFF = 43.6 / (43.6 + 0.27*COLFAC) R11 = FE(11)*FLUX(IPFE10)*3.122E-12*EFF * 1 ( PFE11A*ESCINC(T353(1),1E-4)/(1.+17.0/5.3*T353(3) ) + 2 PFE11B*ESCINC(T353(1)/3.,1E-4)/(1.+11.0/12.3*T353(3) ) ) contribution to Fe11 from continuum fluorescence call linadd( R11 , 7892 , 'Pump','i')
2 put this in
0 rm this old code for old NI collisions
2 these are actually in the optical depth arrays, should be moved to call PutLine - but some needed vars are not defined in structure
2 add charged heavy elements
1 stupid - why this test on opacity_abs ? - we only get here if we already passed above test on this very thing
0 these RJRW macros are permanent - remove tests & make final
2 impose size limits on PAH's, changeover to graphite ??
2 detect if PAH's are present in ionized regions ??
0 why not set to 0 and insist on positive value?
0 this cannot trip since var init to -99 and already tested, but then 10**x so 1e-99 - should change to init gas_phase to zero init is in zero.cpp
2 Need to include divergence terms in pressure balance if flux index is != 0
2 Need to include divergence terms in pressure balance if flux index is != 0
2 this is the molecular binding energy (?) not set to anything
2 - should this include mass in grains?
2 - should this include mass in grain mantle ice deposits?
0 add this press term due to cosmic rays - hextra.cr_energydensity
0 code has variable magnetic energydensity and pressure, which are equal, as they must be - del one or the other
2 introduce units option for wavelength and include area for intensity to make luminosity
2 possible to grab input lines to say what each parameter is? As in "PARAM1 is HDEN"?
2 This doesn't really seem to be the expression above!!!
2 Steve Kraemer says we're lacking radio recombination continua. Is this why? --RLP
2 should use ConEmitLocal for all continua, but not followed by DiffuseEscape - put that at the end. Once continua all bundled this way, it will be easy to save them as a function of depth and then do exact rt
2 Replace this constant with the appropriate macro, if any
2 add fegrain to outward beams, but within main formalism by including grains in all x-ray processes
1 dynamics; this test assumes that neg vel are subsonic, so that sobolev length would overestimate the optical depth, since ion is at most present over computed slab, and possibly more.
1 rewrite so tht this checks on size not sign of windv
- check rebinning of Tlusty models
- why was it necessary to change stars_tlusty.in? (change from r43 to r50?)
- check all interpolation modes of CoStar
- compare models with original code, dump atmospheres!
- check all Edges arrays...
- update Doxygen documentation
- write documentation for ascii files
2 include code for interpolating inv_att_len somewhere!!
2 why is charge of pah2_ism_01.opc so different??
2 use a canned interpolation routine, no need for special one here
there is a virtually identical routine in helike_recom.cpp -> combine
2 change this to CS_new
2 file opacities are disabled for now - reinstate this when arrays settle down
2 why are higher Lyman lines (ipResoRedist) not same as for H-like?
1.6.1
