Class radLoss
source code
_SpecTrails._specTrails --+
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radLoss
Calculate the emission spectrum as a function of temperature and
density.
includes elemental abundances or ionization equilibria
temperature and density can be arrays but, unless the size of either
is one (1), the two must have the same size
the returned spectrum will be convolved with a filter of the specified
width on the specified wavelength array
the default filter is gaussianR with a resolving power of 1000. Other
filters, such as gaussian, box and lorentz, are available in
chianti.filters. When using the box filter, the width should equal the
wavelength interval to keep the units of the continuum and line spectrum
the same.
A selection of ions can be make with ionList containing the names of
the desired lines in Chianti notation, i.e. C VI = c_6
a minimum abundance can be specified so that the calculation can be
speeded up by excluding elements with a low abundance. With solar
photospheric abundances -
setting minAbund = 1.e-4 will include H, He, C, O, Ne setting minAbund
= 2.e-5 adds N, Mg, Si, S, Fe setting minAbund = 1.e-6 adds Na, Al, Ar,
Ca, Ni
Setting em will multiply the spectrum at each temperature by the value
of em.
em [for emission measure], can be a float or an array of the same
length as the temperature/density.
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| __init__(self,
temperature,
eDensity,
elementList=0,
ionList=0,
minAbund=0,
doContinuum=1,
abundanceName=0,
verbose=0,
allLines=1,
keepIons=0) |
source code
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radLossPlot(self)
to plot the radiative losses vs temperature |
source code
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Inherited from _SpecTrails._specTrails:
convolve,
ionGate,
lineSpectrumPlot,
spectrumPlot
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__init__(self,
temperature,
eDensity,
elementList=0,
ionList=0,
minAbund=0,
doContinuum=1,
abundanceName=0,
verbose=0,
allLines=1,
keepIons=0)
(Constructor)
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- Overrides:
_SpecTrails._specTrails.__init__
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