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

faster if the DOME radiative transfer method is used). dotcor=.false. is mainly used
together with iter=0 and irtmth=0 to compute high resolution observer’s frame spectra using
the DOME transfer code. The overhead of the temperature correction procedure for the OS/ALI
method is relatively small and can be neglected.
• tcor min: REAL variable. If the temperature corrections at all layers are all less than
tcor min, no more iterations will be preformed. The default value is 1K.
• idmin: INTEGER variable which gives the minimum damping factor for the temperature
iterations. The iterations will be damped with 2 −idmin in order to avoid over corrections and
oscillations. Usually this parameter should be between 1 and 2. If idmin < 0, −idmin gives the
maximum allowed temperature correction ∆T in % (this may help in difficult cases).
• ultcor: .TRUE., if the modified Unsöld-Lucy temperature correction method is selected (this
requires the OS/ALI radiative transfer), the default is .FALSE., selecting the Newton-hybrid
temperature correction.
• tsw: A technical parameter. At this standard optical depth, PHOENIX will switch from the
� κ(J − B) dλ condition to the “luminosity” condition. For an extinction optical depth scale, the
value of tsw should be around 1, for an absorption scale around 10 −2 . If the value is too small,
the temperature iteration will be strongly unstable in the outer parts of the atmosphere; if the
value is too large, large over-corrections of the temperature will occur. This variable is not used,
if dotcor (see below) is .false..
• tapp: A technical parameter. The temperature for τstd < τapp will be set constant. This
parameter is useful to speed up the temperature iteration for some models. Usually set to zero.
4.13 LTE atomic, ionic and molecular line parameters
• greli: lines selection threshold parameter. A LTE line will be included in the calculation, if
κlc/κcont ≥ greli for the reference layers, otherwise it is ignored. Here κlc denotes the
absorption coefficient at the line center and κcont the corresponding continuum absorption
coefficient. If greli = 0, all available lines will be included until the arrays for storing line data
are filled and the time consuming selection procedure is skipped. Not used, if EZL=.FALSE..
• gremlin: As greli but for molecular lines. Not used if ezlmol=.false..
• cas greli: As greli but for the NLTE lines from the Cassandra data structures. Not used if
inlte=0.
• skip select: LOGICAL variable, set to .TRUE. to skip molecular line selection after first
iteration when running in MPI parallel mode. Default is .FALSE.. Warning: if you use this
speed-up, make sure to select all important lines on the first run, e.g., by choosing extremely small
thresholds.
• grelvoigt: used only for iwhprof=2 and gives the threshold for lines with full Voigt profiles
(works like greli).
• gremvoigt: like grelvoigt but for the molecular lines
• nonunfm: set to .TRUE. to allow non uniform abundances in SN modes.
• binary compositions: Set to .TRUE. to read composition file in binary mode.
• nref: number of references points for the line selection procedure. Default is 3, if set to layer
the line selection procedure will be done automatically for all radial grid points.
• tauref: standard optical depth points used for the line selection procedure. Default set by
mkinput.
• sobid: .TRUE. to turn on Sobolev ID’s for SN models (used only for IDs, nothing else).
• nsobref: number of references points for Sobolev line ID procedure. Default is 4, if set to
layer the Sobolev line ID procedure will be done automatically for all radial grid points.
• tausobref: standard optical depth points used for the Sobolev line ID procedure. Default set
by mkinput.
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