Version 15 June 2007 compiled: 11-11-2009 - Hamburger Sternwarte

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adapting the code in the subroutine wavcon in misc.f. tcirc=0 will also disable the impinging radiation field. 4.<strong>15</strong> Eulerian and Lagrangian continuum wavelength grids • intber: An array containing the interval boundaries for the wavelength grid used for the observer’s frame by PHOENIX. The wavelengths are given in ˚A, a zero indicates the last point used. The length of the array is fixed to 50, the last value should be 0 if not all entries are used. • intdis: This array contains the step size between the corresponding intber points [ ˚A]. If the step size is larger than the difference between the corresponding intber points, an error message will be issued. If the total number of wavelength points is too large to fit into the internal arrays on PHOENIX, a warning will be printed, and the maximum number of points will be used. To increase this maximum number of points, increase maxobs in all subroutines of PHOENIX and recompile. These computed Euler grid will only be used, if iter is zero, otherwise it will be ignored. • cmtber: analogous to intber, but for the Lagrangian frame • cmtdis: analogous to intdis, but for the Lagrangian frame. The number of Lagrange frame points will influence the CPU time used for one temperature iteration (linear). • fmt vfld: string for format code for spectrum output to channel 7, used for models with a velocity field. Note: the number and type of the arguments must be exactly like the default setup or a runtime error will occur. This setting is useful if high resolution wavelength and flux outputs are needed. • fmt stat: string for format code for spectrum output to channel 7, used for static models. Note: the number and type of the arguments must be exactly like the default setup or a runtime error will occur. This setting is useful if high resolution wavelength and flux outputs are needed. • fmt id: string for format code for spectrum output to channel 7, used for static models in ID mode (see doid). Note: the number and type of the arguments must be exactly like the default setup or a runtime error will occur. This setting is useful if high resolution wavelength and flux outputs are needed. • read wl grid: logical switch. Defaults to false. If set to true PHOENIX reads a wavelength grid from an input file called wl.grid. This file can contain several “wavelength chunks”. The first line of a chunk is the number of wavelength points for this chunk in integer format. Then follow the wavelength points, one wavelength point per line, read in as double precision. Usually, there is only one chunk. The wavelength points need not to be sorted. The grid will be ADDED to the existing LAGRANGIAN frame grid. 4.16 NLTE parameters The number of NLTE species has rapidly increased since the first version of the manual was written. The new version of the NLTE routines use a generalized input scheme for the NLTE species description, see below. One goal is the existing parameters here. The number of levels treated in NLTE can be set for each ion individually. The naming convection for the parameters is nXX# where XX is the chemical symbol (e.g., fe for iron) and # is the ionization stage (1 for the neutral element, 2 singly ionized stages etc.). For example, nsi4=50 specifies that 50 levels of Si IV are treated in NLTE. The number given in the input file will be set to the maximum number of levels available if it exceeds that value. • chianti path: full pathname to CHIANTI data file root directory, this is used only if NLTE species using CHIANTI data files are requested. The directory structure has to be a standard CHIANTI 3.03 system. • chianti4 path: same as chianti path, but for CHIANTI 4.02 data. • aped path: same as chianti path, but for APED (ATOMDB) data. 24
• phoenix path: full pathname to PHOENIX .atom files. Used only if NLTE species using PHOENIX data files are requested. This path is also used to locate special line profiles (as they depend on the atomic level data used). • h1 internal: .TRUE. (default) to use the internally coded PHOENIX model atom for H I. .FALSE. uses the external file data. • he1 internal: .TRUE. (default) to use the internally coded PHOENIX model atom for He I. .FALSE. uses the external file data. • he2 internal: .TRUE. (default) to use the internally coded PHOENIX model atom for He II. .FALSE. uses the external file data. • ne1 internal: .TRUE. (default) to use the internally coded PHOENIX model atom for Ne I. .FALSE. uses the external file data. • nlte z list(???): nuclear charge for NLTE species number “???”, 1 for H, 2 for He etc. • nlte ion stg list(???): Ionization state for species number “???’, e.h., 1 for I (neutral), 2 for II (singly ionized) etc. • nlte level number(???): Number of levels to be considered in the model atom for species number “???”. Can be set to large number to request maximum available. • nlte dataset(???): Code for NLTE dataset to use for species number “???”: 1 for PHOENIX .atom file, 2 for CHIANTI version 3 dataset, 3 for CHIANTI version 4 dataset and 4 for APED (ATOMDB) dataset. Other values are reserved and will be available later. • nlte line mode: INTEGER flag selecting the formula to use for Cassandra NLTE lines. Currently allowed values are 0: strict LTE formula, 1: standard Cassandra formula, 2: classic formula. Default is ’1’. ’2’ is automatically selected in opacity table mode. ’0’ should be selected if Cassandra is just used to compute detailed line profiles for cool stars. • profile files(???): List of file names for special NLTE line profile files. The max. number of files is set in input.f. The path to the files is given in phoenix path. The files must be compatible with cas profile read and give all profiles for a given set of transitions that share the same relative profile for a number of temperatures and perturbers. • n wl 4 prfs: number of wavelength points per special NLTE line profile for normalization and interpolation. Points are automatically distributed. • use van reg: set to .TRUE. to allow the use of the Van Regemorter formula for collisional rates if no other data are available. .FALSE. will resort to Allen’s old formula. • pb h coll rates: set to .TRUE. to use new H I bound-bound collision rates from Przybilla & Butler (2004) for levels n
Page 1 and 2: Messages of the day: PHOENIX Versio
Page 3 and 4: • deviations from “local thermo
Page 5 and 6: with χs,s+1 =| χs − χs+1 |, th
Page 7 and 8: • linecom.f: module with data str
Page 9 and 10: e wrong! • Unit 19: Output files.
Page 11 and 12: • newcia: set which CIA version t
Page 13 and 14: 3. OR a velocity law for a red gian
Page 15 and 16: • itaugrid: The type of tau-grid
Page 17 and 18: 4.5.5 Ad’hoc Gravitational Settli
Page 19 and 20: luminosity (used in makehydro) •
Page 21 and 22: faster if the DOME radiative transf
Page 23: • uselin: INTEGER array with flag
Page 27 and 28: 4.19 EOS parameters, e.g., abundanc
Page 29 and 30: References Albrow, M., An, J., Beau
Page 31 and 32: Bean, J. L., Sneden, C., Hauschildt
Page 33 and 34: Howell, S. B., Hauschildt, P. H., &
Page 35: Schweitzer, A., Hauschildt, P. H.,

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