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intro.tex
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intro.tex
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\chapter{Preface}
\label{sec:intro}
%\section{A brief overview of libRadtran}
{\sl libRadtran} is a library of radiative transfer routines and
programs. The central program of the {\sl libRadtran} package is the
radiative transfer tool {\sl uvspec}. {\sl uvspec} was originally
designed to calculate spectral irradiance and actinic flux in the
ultraviolet and visible parts of the spectrum \citep{kylling92a} where
the name stems from. Over the years, {\sl uvspec} has undergone
numerous extensions and improvements. {\sl uvspec} now includes the
full solar and thermal spectrum, currently from 120~nm to
100~$\mu$m. It has been designed as a user-friendly and versatile tool
which provides a variety of options to setup and modify an atmosphere
with molecules, aerosol particles, water and ice clouds, and a surface
as lower boundary. One of the unique features of {\sl uvspec} is that
it includes not only one but a selection of about ten different
radiative transfer equation solvers, fully transparent to the user,
including the widely-used DISORT code by \citet{Stamnes1988c} and its
C-code version \citep{buras2011b}, a fast two-stream code
\citep{Kylling1995}, a polarization-dependent code polRadtran
\citep{Evans1991}, and the fully three-dimensional Monte
Carlo code for the physically correct tracing of photons in cloudy
atmospheres, MYSTIC \citep{mayer2009, emde2007, emde2010, buras2011a,
emde2011}. MYSTIC optionally allows to consider polarization and fully
spherical geometry. Please note that the public release includes only a
1D version of MYSTIC.
{\sl libRadtran} also provides related utilities, like e.g. a Mie program
({\sl mie}), some utilities for the calculation of the position of the
sun ({\sl zenith}, {\sl noon}, {\sl sza2time}), a few tools for
interpolation, convolution, and integration ({\sl spline}, {\sl conv},
{\sl integrate}), and several other small tools for setting up
{\sl uvspec} input and postprocessing {\sl uvspec} output.
Further general information about {\sl libRadtran} including examples
of use may be found in the
reference publication \citep{mayer2005}.
It is expected that the reader is familiar with radiative transfer
terminology. In addition, a variety of techniques and
parameterizations from various sources are used. For more information
about the usefulness and applicability of these methods in a specific
context, the user is referred to the referenced literature.
{\sl Please note that this document is by no means complete. It is
under rapid development and major changes will take place.}
\section*{Acknowledgements}
Many people have already contributed to {\sl libRadtran}'s
development. In addition to Bernhard Mayer (\email{bernhard.mayer (at)
lmu.de}), Arve Kylling (\email{arve.kylling (at) gmail.com}), Claudia Emde
(\email{claudia.emde (at) lmu.de}), Robert Buras
(\email{robert.buras (at) lmu.de}), Josef Gasteiger
(\email{josef.gasteiger (at) lmu.de}), Bettina Richter
(\email{bettina.richter (at) lmu.de}) and Ulrich
Hamann (\email{hamann (at) knmi.nl}) the following people have
contributed to {\sl libRadtran} or helped out in various other ways
(the list is almost certainly incomplete -- please let us know if we
forgot somebody):
\begin{itemize}
\item The \code{disort} solver was developed by Knut Stamnes, Warren Wiscombe,
S.C.~Tsay, and K.~Jayaweera
\item The translation from the FORTRAN version of the DISORT solver to C-code was performed by Timothy E.~Dowling
\item Warren Wiscombe provided the Mie code \code{MIEV0}, and the routines to calculate
the refractive indices of water and ice, \code{REFWAT} and \code{ICEWAT}.
\item Seiji Kato (\email{kato (at) aerosol.larc.nasa.gov}) provided the
correlated-k tables described in Kato et al. (1999).
\item Tom Charlock (\email{t.p.charlock (at) larc.nasa.gov}), Quiang Fu
(\email{qfu (at) atm.dal.ca}),
and Fred Rose (\email{f.g.rose (at) larc.nasa.gov}) provided the most recent version
of the Fu and Liou code.
\item David Kratz (\email{kratz (at) aquila.larc.nasa.gov}) provided the routines
for the simulation of the AVHRR channels described in
Kratz (1995).
\item Frank Evans (\email{evans (at) nit.colorado.edu}) provided the
\code{polradtran} solver.
\item Ola Engelsen provided data and support for different ozone
absorption cross sections.
\item Albano Gonzales (\email{aglezf (at) ull.es}) included the Yang et
al. (2000), Key et al. (2002) ice crystal parameterization.
\item Tables for the radiative properties of ice clouds for different
particle ``habits'' were obtained from Jeff Key and Ping Yang,
Yang et al. (2000), Key et al. (2002). In addition, Ping Yang and
Heli Wei kindly provided a comprehensive database of particle
single scattering properties which we used to derive a consistent
set of ice cloud optical properties for the spectral range 0.2 - 100 micron
following the detailed description in Key et al. (2002).
A comprehensive dataset including the full phase matrices has been
generated and provided by Hong Gang.
\item Paul Ricchiazzi (\email{paul (at) icess.ucsb.edu}) and colleagues
allowed us to include the complete gas absorption parameterization
of their model SBDART into {\sl uvspec}.
\item Luca Bugliaro (\email{luca.bugliaro (at) dlr.de}) wrote the analytical
TZS solver (thermal, zero scattering).
\item Sina Lohmann (\email{sina.lohmann (at) dlr.de}) reduced the ``overhead time''
for reading the Kato et al. tables dramatically which resulted in
a speedup of a factor of 2 in a twostr solar irradiance calculation.
\item Detailed ice cloud properties were provided by Bryan Baum
(\email{bryan.baum (at) ssec.wisc.edu}).
\item Yongxiang Hu (\email{yongxiang.hu-1 (at) nasa.gov}) provided the delta-fit
program used to calculate the Legendre coefficients for \code{ic\_properties baum\_hufit}.
\item Caro Klinger (\email{carolin.klinger (at) lmu.de}) implemented
thermal heating and cooling rate calculations in MYSTIC and provided the
approximate 3D neighboring column approximation (NCA), see Klinger
and Mayer (2016), Klinger and Mayer (2019).
\item Nina Crnivec (\email{nina.crnivec (at) physik.uni-muenchen.de})
developed the twomaxrnd solver.
\item Many unnamed users helped to improve the code by identifying
or fixing bugs in the code.
\end{itemize}