Table of Contents
We divide a global atmospheric model into a "dynamical core" and a set of "physics" modules, the combination of which is sufficient to integrate the state of the atmosphere forward in time for a given time interval. The dynamical core must be able to integrate the basic fluid equations for an inviscid, adiabatic ideal gas over an irregular rotating surface forward in time. Included in the dynamical core is the horizontal and vertical advection, horizontal subgrid scale mixing, and the time differencing.
Our operational definition of a global atmospheric dynamical core is a module, or set of modules, which is capable of integrating a particular benchmark calculation defined by Held and Suarez (1994) so as to obtain a statistically steady "climate". Model physics is replaced by very simple linear relaxation of temperature to a specified spatial structure and the winds near the surface are relaxed to zero. Because the resulting flow is turbulent and cascades variance to small horizontal scales, either explicit or implicit horizontal mixing is required to obtain a solution, and, as stated above, is considered to be part of the dynamical core.
The global, hydrostatic finite difference dynamical core, also called the B-grid core, was developed from models described in Mesinger, et al. (1988)  and Wyman (1996) . The horizontal grid is the Arakawa B-grid and a hybrid sigma/pressure vertical coordinate is used. The step-mountain (eta coordinate) option is no longer supported.
The spectral dynamical core is a "plain vanilla" version of the classic Eulerian spectral model, with a spherical harmonic basis, for integrating the primitive equations on the sphere. The option of advecting tracers with a finite-volume grid point scheme is also available. Barotropic (2D non-divergent) and shallow water spherical models are also provided.
The finite-volume (FV) core is described in Lin 2004. The horizontal grid is currently based on the regular latitude-longitude grid. The vertical coordinate internal to the FV core is fully Lagrangian with remapping to a Euler coordinate as used in the physical parameterizations.
We will try our best to respond to your support requests and bug reports quickly, given the limits of our human resources devoted to this project. Please use the mailing lists (oar.gfdl.fmsgfdl.noaa.gov and oar.gfdl.fms-atmosgfdl.noaa.gov) as the forum for support requests: browse the mailing lists for answers to your questions, and post new questions directly to the mailing list. We would also appreciate it if you could answer other users' questions, especially those related to site and platform configuration issues that you may have encountered. We will provide very limited support for platforms not listed in Section 1.4, “Portability”, and for modifications that you make to the released code.
Our commitment at any given time is only on those platforms where we have adequate access for our own thorough testing. We will add supported platforms as we can.
The platforms we support at present are the following:
1) SGI Chipset: MIPS OS: Irix 6.5 Compiler: MIPSPro version 126.96.36.199 or higher Libraries: Message Passing Toolkit (MPT) version 188.8.131.52 or higher. netCDF version 3.4 or higher (64-bit version) 2) Linux Chipset: AMD OS: GNU/Linux Compiler: Intel Fortran Compiler Version 9.0-027 Libraries: MPI-1 (e.g MPICH-1.2.5) netCDF version 3.4 or higher (64-bit version)
The Flexible Modeling System (FMS) is free software; you can redistribute it and/or modify it and are expected to follow the terms of the GNU General Public License as published by the Free Software Foundation; either version 2 of the License, or (at your option) any later version.
FMS is distributed in the hope that it will be useful, but WITHOUT ANY WARRANTY; without even the implied warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the GNU General Public License for more details.
You should have received a copy of the GNU General Public License along with this release; if not, write to:
Free Software Foundation, Inc.
59 Temple Place, Suite 330
Boston, MA 02111-1307
or see: http://www.gnu.org/licenses/gpl.html
In addition to this web page, additional documentation for the atmospheric dynamical cores may be found in these documents:
Key features of the finite difference dynamical core are:
General features are:
Key features of the spectral dynamical core are:
Key features of the finite-volume dynamical core are:
We do not specify the precise interface expected of a dynamical core. Within FMS we do specify the precise interface for the atmospheric model as a whole, so as to allow it to communicate with land, ocean, and ice models. Atmospheric models are generally constructed for each core individually from the dynamical core and individual physics modules. Sets of physics modules are bundled into physics packages that can be used to more easily compare models with the same physics and different cores (the Held-Suarez forcing is the simplest example of such a package) but we also recognize that different cores may require the physics to be called in distinct ways.
The B-grid and spectral dynamical cores share high-level superstructure code and low-level FMS infrastructure codes. The dynamical core is sandwiched between these levels. For the simple test cases provided with this release the superstructure only consists of a main program, but in more realistic models, drivers for component models and coupling software may also be considered part of the superstructure. The FMS infrastructure codes, which include many commonly-used utilities, are used by both the dynamical core and the superstructure code. The following figure depicts this hierarchy of model codes.
The dynamical cores have the same user interface at the atmospheric driver level. Atmospheric drivers are constructed for each core for specific types of models. The drivers included with this public release are for running in a dynamical core only mode using simple forcing from a shared module (the Held-Suarez GCM benchmark model). Other drivers exist for running coupled models using full atmospheric physics in either AMIP mode or fully coupled to a realistic ocean, ice, and land model.
A user selects which dynamical core to use prior to compiling the model. A list of path names to the source code of a specific core and the FMS shared codes is supplied to a compilation script. Refer to Section 5, “Preparing the runscript” for details on compiling the source code.
|parallelization tools:||Simple routines that provide a uniform interface to different message-passing libraries, perform domain decomposition and updates, and parallel I/O on distributed systems.|
|I/O and restart file utilities:||Routines for performing commonly used functions and for reading and writing restart files in native or NetCDF format.|
|time manager:||Simple interfaces for managing and manipulating time and dates.|
|time interp:||Computes weight and dates indices for linearly interpolating between two dates.|
|diagnostics manager:||Simple calls for parallel NetCDF diagnostics on distributed systems.|
|field manager/ tracer manager:||Code to read entries from a field table and manage the simple addition of tracers to the FMS code.|
|fast Fourier transform:||Performs simultaneous FFTs between real grid space and complex Fourier space.|
|topography:||Routines for creating land surface topography and land-water masks.|
|constants :||Sets values of physical constants and pi.|
|horiz_interp:||Performs spatial interpolation between grids.|
|axis_utils:||A set of utilities for manipulating axes and extracting axis attributes.|
|data_override:||Utility for spatial and temporal interpolation of data to the model grid and time.|
|memutils:||Various operations for memory management.|
|platform:||Provides public entities whose value may depend on the operating system and compiler.|
|main program:||For running a stand-alone atmospheric model.|
The Flexible Modeling System development team at GFDL uses a local implementation of GForge to serve FMS software, located at http://fms.gfdl.noaa.gov. In order to obtain the source code, you must register as an FMS user on our software server. After submitting the registration form on the software server, you should receive an automatically generated confirmation email within a few minutes. Clicking on the link in the email confirms the creation of your account.
After your account has been created, you should log in and request access to the FMS Atmospheric Dynamical Cores project. Once the FMS project administrator grants you access, you will receive a second e-mail notification. This email requires action on the part of the project administrator and thus may take longer to arrive. The email will contain instructions for obtaining the release package, which are described below.
The download will create a directory called atm_dycores in your current working directory containing the release package. The readme file in the atm_dycores directory gives a brief overview of the package's directory structure and contents.
Sample output is also available for download. See Section 6.1, “Model output” for more information on the sample output.
GForge is an Open Source collaborative software development tool, which allows organization and management of any number of software development projects. It is designed for managing large teams of software engineers and/or engineers scattered among multiple locations. Gforge is available at http://www.gforge.org. General user documentation can be found at http://gforge.org/docman/?group_id=1.
The sample runscripts use the utility mkmf, provided in the atm_dycores/bin directory, to create a makefile, and the make utility to compile the FMS source code. A listing of paths to all checked out source code files is included in the path_names files, located in each dynamical core directory under the atm_dycores/exp/ directory. The path_names file is used by the makefile utility mkmf to create a makefile. The path_names.html files included in the atm_dycores/exp/$dycore directory are created for the user's convenience and contain links to all the relevant documentation files that have been checked out from the download along with the source code. A makefile is used to determine the source code dependencies and the order in which source code files will be compiled. mkmf ("make-make-file" or "make-m-f") is a tool written in perl5 that will construct a makefile from distributed source. The result of the mkmf utility is a single executable program. Note that mkmf is called automatically in the sample runscripts.
mkmf has the ability to understand dependencies in f90, such as modules and use, the FORTRAN include statement and the cpp #include statement in any type of source. mkmf also places no restrictions on filenames, module names, etc. The utility supports the concept of overlays, where source is maintained in layers of directories with a defined precedence. In addition, mkmf can keep track of changes to cpp flags and knows when to recompile the affected source. This refers to files containing #ifdefs that have been changed since the last invocation.
The calling syntax is:
mkmf [-a abspath][-c cppdefs][-d][-f][-m makefile][-p program] [-t template][-v][-x][args] -a abspath attaches the absolute path to the front of all relative paths to source files -c cppdefs list of cpp #defines to be passed to the source files -d debug flag -f formatting flag -m makefile name of makefile written -p program final target name -t template file containing a list of make macros or commands -v verbosity flag -x executes the makefile immediately args list of directories and files to be searched for targets and dependencies
The debug flag is much more verbose than -v and used only if you are modifying mkmf itself. The formatting flag restricts the lines in the makefile to 256 characters. Lines exceeding 256 characters use continuation lines. If filenames are omitted for the options [-m makefile] and [-p program], the defaults Makefile and a.out are applied. The list of make macro or commands contained in [-t template] are written to the beginning of the makefile.
When the mkmf utility is executed, it reads a template file and runs a list of make macros, commands and compilers. The template is a platform-specific file that contains standard compilation flags. Default template files are provided with the FMS source code and are located in the atm_dycores/bin directory. It is recommended that users set up their own compilation template specific for their platform and compiler. The template file contains the following variables:
FC compiler for FORTRAN files LD executable for the loader step CPPFLAGS cpp options that do not change between compilations FFLAGS flags to the FORTRAN compiler LDFLAGS flags to the loader step CFLAGS flags to the C compiler
For example, the template file for the SGI Intel Fortran Compiler contains:
FC = ifort LD = ifort CPPFLAGS = -I/usr/local/include FFLAGS = $(CPPFLAGS) -fno-alias -stack_temps -safe_cray_ptr -ftz -i_dynamic -assume byterecl -g -O2 -i4 -r8 -nowarn -Wp,-w LDFLAGS = -L/usr/local/lib -lnetcdf -lmpi -lsma CFLAGS = -D__IFC
An include file is any file with an include file suffix, such as .H, .fh, .h, .inc, which is recursively searched for embedded includes. mkmf first attempts to locate the include file in the same directory as the source file. If it is not found there, it looks in the directories listed as arguments, maintaining a left-to-right precedence. The argument list, args, is also treated sequentially from left to right. The default action for non-existent files is to create null files of that name in the current working directory via the UNIX touch command. There should be a single main program source among the arguments to mkmf, since all the object files are linked to a single executable.
The argument cppdefs should contain a comprehensive list of the cpp #defines to be preprocessed. This list is compared against the current "state", which is maintained in the file .cppdefs in the current working directory. If there are any changes to this state, mkmf will remove all object files affected by this change so that the subsequent make will recompile those files. The file .cppdefs is created if it does not exist. .cppdefs also sets the make macro CPPDEFS. If this was set in a template file and also in the -c flag to mkmf, the value in -c takes precedence. Typically, you should set only $CPPFLAGS in the template file and CPPDEFS via mkmf -c.
To execute the mkmf utility, the user must locate the appropriate path_names file in the atm_dycores/exp/$dycore directory. The script list_paths, in the atm_dycores/bin directory, can be used to create a new path_names file containing a list of all source code files in a given directory. The user should set up the compilation template file and execute the mkmf utility. With the appropriate options illustrated in the sample runscripts, the user can call mkmf from the compilation directory and cause mkmf to call the make command automatically after the Makefile is generated.
Underlying FMS is a modular parallel computing infrastructure. MPI (Message-Passing Interface) is a standard library developed for writing message-passing programs for distributed computing across loosely-coupled systems. Incorporated in the FMS source code is MPP (Massively Parallel Processing), which provides a uniform message-passing API interface to the different message-passing libraries. Together, MPI and MPP establish a practical, portable, efficient, and flexible standard for message passing.
There are a number of freely available implementations of MPI that run on a variety of platforms. The MPICH implementation, developed by researchers at Argonne National Lab and Mississippi State University, runs on many different platforms, from networks of workstations to MPPs. If MPICH is installed, the user can compile the source code with MPI. If the user does not have MPICH or the communications library, the FMS source code can be compiled without MPI in one of two ways. If the makefile is created external to the runscript, omit the -c cppdefs flag from the mkmf syntax. To compile the FMS source code without MPI delete -Duse_libMPI from the cppflags variable.
When MPI is not used, the messages from MPP_lib may display but the data is being copied by MPP. Compiling the FMS source code without MPI has been tested and the results show that 1 GB of memory is required for executing the code with and without MPI on a single PE.
Simple (csh shell) scripts are provided for running the atmospheric dynamical cores. These runscripts perform the minimum required steps to compile and run the models and are intended as a starting point for the development of more practical run scripts. The scripts for all available dynamical core models are located in each atm_dycores/exp/$dycore directory.
Near the top of the scripts, variables are set to the full path name of the initial condition (optional), diagnostics table, tracer field table (optional), compilation directory, and the mppnccombine script. The script proceeds to compile and link the source code, create a working directory, and copy the required input data into the working directory. The mpirun command is then used to run the model. The final step for multi-processor runs, is to combine domain-decomposed diagnostics files into global files.
The default the scripts are set to run one or two days on a single processor. The number of processors used is controlled by a variable near the top of the scripts. Users may want to increase the number of processors to decrease the wallclock time needed for a run. The run length (in days) and the atmospheric time step, dt_atmos, in seconds is controlled by namelist &main_nml which is set directly in the runscripts for convenience.
To compile and link the model codes a template file provides platform dependent parameters, such as the location of the netCDF library on your system, to a compilation utility called mkmf. Sample template files for various platforms are provided in the bin directory. More information on mkmf and compiling the source code can be found in Section 4, “Compiling the source code”.
The sample scripts compile the model code with the MPI library and execute using the mpirun command. Refer to Section 4.3, “Compiling without MPI” for issues related to the MPI implementation and for compiling without MPI. The mpirun command is specific to Silicon Graphics machines, and users may need to change this to run on other platforms.
The following sections will describe some of the steps needed to understand and modify the simple runscripts.
The FMS diagnostics manager is used to save diagnostic fields to netCDF files. Diagnostic output is controlled by specifying file and field names in an ASCII table called diag_table. The diagnostic tables supplied with the dynamical cores are found in each atm_dycores/exp/$dycore directory in a file called diag_table. The bgrid, spectral, and FV test cases use a standard table for the Held-Suarez benchmark test case. In the runscript, the user specifies the full path to the appropriate diagnostics table, and it is copied to the file diag_table in the directory where the model is run.
The diagnostic table consists of comma-separated ASCII values and may be edited by the user. The table is separated into three sections: the global section, file section and field section. The first two lines of the table comprise the global section and contain the experiment title and base date. The base date is the reference time used for the time axis. For the solo dynamical cores the base date is irrelevant and is typically set to all zeroes. The lines in the file section contain the file name, output frequency, output frequency units, file format (currently, only netCDF), time units and long name for the time axis. The last section, the field section, contains the module name, field name, output field name, file name, time sampling for averaging (currently, all time steps), time average (.true. or .false.), other operations which are not implemented presently and the packing value. The packing value defines the precision of the output: 1 for double, 2 for floating, 4 for packed 16-bit integers and 8 for packed 1-byte. Any line that begins with a "#" is a comment.
A sample diagnostic table is displayed below.
"Model results from the Held-Suarez benchmark" 0 0 0 0 0 0 #output files "atmos_daily", 24, "hours", 1, "days", "time", "atmos_average", -1, "hours", 1, "days", "time", #diagnostic field entries. "dynamics", "ps", "ps", "atmos_daily", "all", .false., "none", 2, "dynamics", "bk", "bk", "atmos_average", "all", .false., "none", 2, "dynamics", "pk", "pk", "atmos_average", "all", .false., "none", 2, "dynamics", "zsurf", "zsurf", "atmos_average", "all", .false., "none", 2, "dynamics", "ps", "ps", "atmos_average", "all", .true., "none", 2, "dynamics", "ucomp", "ucomp", "atmos_average", "all", .true., "none", 2, "dynamics", "vcomp", "vcomp", "atmos_average", "all", .true., "none", 2, "dynamics", "temp", "temp", "atmos_average", "all", .true., "none", 2, "dynamics", "omega", "omega", "atmos_average", "all", .true., "none", 2, "dynamics", "div", "div", "atmos_average", "all", .true., "none", 2, "dynamics", "vor", "vor", "atmos_average", "all", .true., "none", 2, "dynamics", "tracer1", "tracer1", "atmos_average", "all", .true., "none", 2, "dynamics", "tracer2", "tracer2", "atmos_average", "all", .true., "none", 2, #"hs_forcing", "teq", "teq", "atmos_average", "all", .true., "none", 2,
The FMS field and tracer managers are used to manager tracers and specify tracer options. All tracers used by the model must be registered in an ASCII table called field_table. The field tables supplied with the dynamical cores are found in each atm_dycores/exp/$dycore directory. There are no field tables provided for the barotropic or shallow-water models. In the runscript, the user specifies the full path to the appropriate field table, and it is copied to file field_table.
The field table consists of entries in the following format. The first line of an entry should consist of three quoted strings. The first quoted string will tell the field manager what type of field it is. The string "tracer" is used to declare a tracer field entry. The second quoted string will tell the field manager which model the field is being applied to. The supported types at present are "atmos_mod" for the atmosphere model, "ocean_mod" for the ocean model, "land_mod" for the land model, and, "ice_mod" for the ice model. The third quoted string should be a unique tracer name that the model will recognize.
The second and following lines of each entry are called methods in this context. Methods can be developed within any module and these modules can query the field manager to find any methods that are supplied in the field table. These lines can consist of two or three quoted strings. The first string will be an identifier that the querying module will ask for. The second string will be a name that the querying module can use to set up values for the module. The third string, if present, can supply parameters to the calling module that can be parsed and used to further modify values. An entry is ended with a backslash (/) as the final character in a row. Comments can be inserted in the field table by having a # as the first character in the line.
Here is an example of a field table entry for an idealized tracer called "gunk".
"TRACER", "atmos_mod", "gunk" "longname", "really bad stuff" "units", "kg/kg" "advec_vert", "finite_volume_parabolic" "diff_horiz", "linear", "coeff=.30" /
In this example, we have a simple declaration of a tracer called "gunk". Methods that are being applied to this tracer include setting the long name of the tracer to be "really bad stuff", the units to "kg/kg", declaring the vertical advection method to be "finite_volume_parabolic", and the horizontal diffusion method to be "linear" with a coefficient of "0.30".
A method is a way to allow a component module to alter the parameters it needs for various tracers. In essence, this is a way to modify a default value. A namelist can supply default parameters for all tracers and a method, as supplied through the field table, will allow the user to modify the default parameters on an individual tracer basis.
The following web-based documentation describes the available method_types for the dynamical cores.
Many model options are configurable at runtime using namelist input. All FMS modules read their namelist records from files called namelists. A module will read namelists sequentially until the first occurrence of its namelist record is found. Only the first namelist record found is used. Most (if not all) namelist variables have default values, so it is not necessary to list all namelist records in the namelists file. The runscripts provided set up the file input.nml by concatenating the core-specific namelist files.
|bgrid_core_driver_nml:||main namelist for the B-grid core. It controls the following options: time splitting, domain layout, polar filtering, pressure gradient, divergence damping, energy conservation, and restart file format.|
|bgrid_advection_nml:||advection scheme and tracer filling options|
|bgrid_horiz_diff_nml :||horizontal damping order and coefficients|
|bgrid_sponge_nml:||top model level sponge coefficients|
|bgrid_integrals_nml:||used to set the file name and output interval for global integrals|
|bgrid_cold_start_nml:||needed for cold-starting the model, only read when the restart file does not exist|
|spectral_dynamics_nml:||main namelist for the spectral core|
|atmosphere_nml:||atmospheric settings for the barotropic and shallow configurations|
|barotropic_dynamics_nml:||dynamical settings for the barotropic configuration|
|barotropic_physics_nml:||physics settings for the barotropic configuration|
|shallow_dynamics_nml:||dynamical settings for the shallow configuration|
|fv_core_nml:||main namelist for the finite-volume core|
Change the run length:
|The default run length set in the simple runscripts is relatively short. The run length is set in the namelist for the main program, which can be found in the runscripts. For example, the following change will increase the run length to 200 days.|
Change the model resolution:
|Because the simple test cases internally generate their initial state, the model resolution can be easily changed through namelist variables. For the B-grid core, modify the following namelist found in file atm_dycores/exp/bgrid/namelists. Note that nlon and nlat must be even numbers, and too low a resolution may result in an unphysical solution. For a T63 spectral core, modify the following namelist variables found in the file atm_dycores/exp/spectral/namelists.|
Change the model time step:
|If the model resolution is changed it may be necessary to also change the model time step. The time step for the atmospheric model is set in the namelist for the main program, which can be found in the runscripts. For example, in atm_dycores/exp/bgrid/fms_runscript the following will change the time step to 1200 seconds.|
Change the domains stack size:
|If you increase the model resolution or are running on a small number of processors, you may get the error message "MPP_UPDATE_DOMAINS user stack overflow". In this case, increase the domain stack size found in the core-specific namelist files. The new stack size should be greater than or equal to the number printed in the error message.|
Run the FV core on multiple processors:
|Decomposition is not supported in the x direction, so the first value is 1, and $npes is the number of processors the code is run on.|
The FV core is set up so that the defaults generally produced the best results. For example, the model will automatically determine a most efficient time step size if n_split is absent from the namelist input or is set to ZERO. The tracer time step is dynamically determined every time step to maintain CFL condition in the north-south direction to be less than ONE. If the user is uncertain about any namelist input, please use the default.1. Required namelist input from the user:
|east-west dimension (e.g., nlon=144 for M45 resolution). The resolution (degrees) is 360/nlon. Due to the use of FFT at high latitudes for polar filtering, nlon must be an even number.|
|north-south dimension (mlat=90 for M45 resolution). The meridional resolution (degrees) is 180/(mlat-1). For better load balance, it is recommend that mlat be divisible by 3 (e.g., 60, 90, 180). However, any number would work.|
|vertical dimension (total number of layers).|
|total number of tracers (including all physics tracers nt_phys). For the standard AM2 physics, ncnst=4.|
2.1 Input that controls the advection operators:
The following "ORD" values determine the transport schemes to be used for different spatial directions and different prognostic variables. These options are mainly for testing/development purposes and a typical user should just use the defaults (Piecewise Parabolic Method with the monotonicity constraint as described in Lin 2004). Setting these values to 2 will force the model to use the 2nd order accurate Van Leer scheme instead.
|advection operator in the zonal direction for momentum.|
|advection operator in the zonal direction for thermodynamics.|
|advection operator in the zonal direction for tracers.|
|advection operator in the meridional direction for momentum.|
|advection operator in the meridional direction for thermodynamics.|
|advection operator in the meridional direction for tracers.|
|advection operator in the vertical direction for momentum.|
|advection operator in the vertical direction for thermodynamics.|
|advection operator in the vertical direction for tracers.|
2.2 Miscellaneous optional input:
|total number of tracers needed by physics (4 in AM2).|
|number of non-advected tracers. This is used by some chemistry packages in which not all tracers are advected.|
|number of time splits for the Lagrangian (horizontal) dynamics. The model contains an algorithm for the automatic determination of the most efficient value. If instability arises, the user may want to increase the value of n_split (therefore, reducing the size of time step).|
|loop decomposition in East-West direction. This may have some impact on the computational speed if the platform is cache based or is "OpenMP" capable.|
|remapping time step (equal to model time step). The option of using different remapping time step than the physics is currently not supported.|
|energy fixer. Range[0,1.]. The default is ZERO (no energy conservation correction). Setting consv_te to ONE force the dynamics to maintain exact conservation of total energy for each time step.|
|"native" (IEEE) or "netcdf".|
|run the model without any physics (diabatic) forcing. This flag is mainly used to turn off the Held-Suarez in the "solo" mode.|
|run the model with full (AM2) physics with virtual effects (when computing geopotential).|
|activate a vertical filling algorithm for tracers (needed if physics/chemistry produced negatives).|
|adjust the initial global mean dry mass to pre-set value.|
|total number of sponge layers (counting from top; default is 1). The horizontal transport scheme is set to the highly diffusive first order upwind scheme within the sponge layers.|
|number of diffusive layers (counting from the bottom; default is 0). This mirrors the top sponge layers. This option may be useful only in certain idealized environment -- it is not recommended for general usage.|
|ignore time stamp in the restart file. This option is useful for swapping restart files from a different time/date.|
|dimensionless divergence damping parameters: D = a_div + b_div * cos(lat). The physical damping coefficient will be equal to D * dx * dy / dt.|
|dimensionless divergence damping parameters: D = a_div + b_div * cos(lat).|
|use set_eta(), instead of restart, for (ak,bk). This is useful for doing model model cold start. Several settings are available, ranging from 18 to 100 layers. The routine for setting the definition of the "eta" coordinate (for remapping) is located in src/atmos_fv_dynamics/tools/set_eta.f90.|
|use the tendency approach for updates. This option is no longer supported.|
|relax H2o to Haloe data between 1 and 10 mb. This is a rarely used option. It is mainly used for starting the model from a totally dry atmosphere.|
|polar filter physical tendencies. This option may be useful for high resolution runs. Default is .F.|
|transport the age tracer as the last tracer. This option is no longer supported.|
|print max/min of some selected fields (0: off; positive n: every n hours; negative n: every time step).|
|test case number if "SW_DYN" (shallow water dynamics) is defined during compilation. In this mode, nlev must be set to ONE.|
|computational layout (layout = 1, $npes). Decomposition is not supported in the x-direction and $npes is the number of processors.|
FMS uses restart files to save the exact (bit-reproducible) state of the model at the end of a model run. The restart files are used as an initial condition to continue a model run from an earlier model integration. A module (or package of modules) will write data to a restart file if it is needed for a bit-reproducible restart. The input restart files (the initial conditions) are read from the INPUT subdirectory. The output restart files are written to the RESTART subdirectory. The simple runscripts create these two directories when setting up the model run.
The initial condition file specified in the simple runscripts is a cpio archive file that contains the restart files created by individual modules. The test cases provided with this release do not specify an initial condition file, but rather generate their initial states internally. The test case will however create output restart files, and a user may want to archive or move the output restart files so they can be used as an initial condition when continuing a model run.
To create a cpio archive file:
cd RESTART /bin/ls *.res* | cpio -ov > OutputRestart.cpio
or, simply move the output files to the input directory:
rm INPUT/*.res* mv RESTART/*.res* INPUT mpirun -np 1 fms.exe # rerun the model
Because the restart file for the main program contains information about the current model time, there is no need to modify any namelist or input files before rerunning the model.
The restart file created by the B-grid core is called bgrid_prog_var.res.nc and the restart file created by the spectral core is called spectral_dynamics.res.nc. Here are some specific details about the restart file for each core.
Running the FMS source code in a parallel processing environment will produce one output netCDF diagnostic file per processor. mppnccombine joins together an arbitrary number of data files containing chunks of a decomposed domain into a unified netCDF file. If the user is running the source code on one processor, the domain is not decomposed and there is only one data file. mppnccombine will still copy the full contents of the data file, but this is inefficient and mppnccombine should not be used in this case. Executing mppnccombine is automated through the runscripts. The data files are netCDF format for now, but IEEE binary may be supported in the future.
mppnccombine requires decomposed dimensions in each file to have a domain_decomposition attribute. This attribute contains four integer values: starting value of the entire non-decomposed dimension range (usually 1), ending value of the entire non-decomposed dimension range, starting value of the current chunk's dimension range and ending value of the current chunk's dimension range. mppnccombine also requires that each file have a NumFilesInSet global attribute which contains a single integer value representing the total number of chunks (i.e., files) to combine.
The syntax and arguments of mppnccombine are as follows:
mppnccombine [-v] [-a] [-r] output.nc [input ...] -v print some progress information -a append to an existing netCDF file -r remove the '.####' decomposed files after a successful run
An output file must be specified and it is assumed to be the first filename argument. If the output file already exists, then it will not be modified unless the option is chosen to append to it. If no input files are specified, their names will be based on the name of the output file plus the extensions '.0000', '.0001', etc. If input files are specified, they are assumed to be absolute filenames. A value of 0 is returned if execution is completed successfully and a value of 1 indicates otherwise.
The source of mppnccombine (mppnccombine.c) is packaged with the FMS dynamical cores in the atm_dycores/postprocessing directory. mppnccombine.c is automatically compiled in the runscript when more than 1 processor is specified. It should be compiled on the platform where the user intends to run the FMS Memphis atmospheric dynamical cores source code. A C compiler and netCDF library are required for compiling mppnccombine.c.
Output from a FMS model run will be written to the directory where the model was run. FMS models write output in ASCII, binary, and netCDF formats. ASCII or text output files have the *.out suffix. For example, files of the form *integral.out contain global integrals and logfile.out contains the namelist and revision number output. Note that the spectral model does not produce *integral.out files. Standard output and standard error messages created by the model may be directed to a file called fms.out. The diagnostics files, specified in the diagnostics table, are written as netCDF files with the *.nc suffix. The output restart files are written to the subdirectory RESTART and will have the *.res.nc or *.res suffix.
You may download sample output data for comparison at https://fms.gfdl.noaa.gov/projects/fms/ under the "Files" tab. Each tar file expands to a directory containing a readme file along with netcdf and ascii output. The files bgrid_output.tar.gz, fv_output.tar.gz and spectral_output.tar.gz contain daily snapshots of surface pressure and time means of all fields over the 200 to 1200 day period. The file bgrid_shallow_output.tar.gz contains daily snapshots of surface pressure and time means of all fields over a 30 day period. The file spectral_barotropic_output.tar.gz contains 1000 days of diagnostic output with a 200 day spin-up period for the spectral barotropic model. spectral_shallow_output.tar.gz contains 30 days of diagnostic output for the spectral shallow water model.
There are several graphical packages available to display the model output. These packages widely vary depending on factors, such as the number of dimensions, the amount and complexity of options available and the output data format. The data will first have to be put into a common format that all the package can read. FMS requires the data to be stored in netCDF format since it is so widely supported for scientific visualization. The graphical package is also dependent upon the computing environment. This section will discuss a two-dimensional browser that is used on workstations, ncview. Please reference the GFDL Scientific Visualization Guide for information on additional graphical packages.
ncview is a visual browser for netCDF data format files and displays a two-dimensional, color representation of single precision floating point data in a netCDF file. You can animate the data in time by creating simple movies, flip or enlarge the picture, scan through various axes, change colormaps, etc. ncview is not a plotting program or an analysis package. Thus, contour lines, vectors, legend/labelbar, axis/tic-marks and geography are not included. The user is unable to perform X-Z or Y-Z cross-sections, unless there is a fourth dimension, time. Rather, ncview's purpose is to view data stored in netCDF format files quickly, easily and simply.
ncview is capable of short user spin-up, fast cross sectioning, magnification, predefined color palettes which can be inverted and 'scrunched' to highlight high or low values, animation along the least quickly varying dimension only with speed control and printing. It also has the ability to read a series of files as input, such as a sequence of snapshot history files. A time series graph for variables pops up by clicking the mouse at a specific point. Other options include a mouse-selectable colormap endpoints with optional reset, map overlay and a filter for one-dimensional variables.
In ncview, the user can <left-click> on any point in a plot to get a graph of the variable verses time at that point. Also, <Ctrl><left-click> on any point to set the colormap minimum to the value at that point, while <Ctrl><right-click> on any point will set the colormap maximum to the value at that point. Use the "Range" button to set (or reset) the colormap min/max. For additional information on ncview, refer to the ncview UNIX manual page (man ncview) or the ncview homepage.
The test cases provided with this release have been run on the SGI Altix Intel Itanium2 1.5 GHz (ifort.9.0-027/mpt-1.12-1) and Origin 3800 MIPS R14000 600 MHz (mipspro_743m/mpt_1900) large-scale clusters at the Geophysical Fluid Dynamics Lab. The table below summarizes the performance for each of the test cases.
Model Resolution Run length (days) # pe Time (sec) on Altix Time (sec) on Origin 3800 bgrid N45 (144 x 90 x 20) 200 15 2303 7757 bgrid_shallow N45 (144 x 90) 200 15 130 378 fv M45 (144 x 90 x 20) 200 15 2425 6201 spectral T42 (128 x 64 x 20) 200 16 384 1399 spectral_barotropic T85 (256 x 128) 200 16 63 243 spectral_shallow T85 (256 x 128) 200 16 112 392
 Held, I. M., and M. J. Suarez, 1994: A proposal for the intercomparison of the dynamical cores of atmospheric general circulation models. Bull. of the Am. Meteor. Soc., 75(10), 1825--1830. Download PDF
 Mesinger, F., Z. I. Janjic, S. Nickovic, D. Gavrilov and D. G. Deaven, 1988: The step-mountain coordinate: Model description and performance for cases of Alpine lee cyclogenesis and for a case of an Appalachian redevelopment. Mon. Wea. Rev., 116, 1493--1518.
 Wyman, B. L., 1996: A step-mountain coordinate general circulation model: Description and validation of medium-range forecasts. Mon. Wea. Rev., 124, 102--121.
 Simmons, A. J. and D. M. Burridge, 1981: An energy and angular-momentum conserving vertical finite-difference scheme and hybrid vertical coordinates. Mon. Wea. Rev., 109, 758--766.
 Lin, S.-J., 1997: A finite-volume integration method for computing pressure gradient force in general vertical coordinates. Quart. J. Roy. Meteor. Soc., 123, 1749--1762.
 Lin, S.-J. and R.B. Rood, 1996: Multidimensional flux-form semi-Lagrangian transport schemes. Quart. J. Roy. Meteor. Soc., 123, 1749--1762.
 Lin, S.-J. and R.B. Rood, 1997: An Explicit Flux-Form Semi-Lagrangian Shallow-Water Model on the Sphere, Quart. J. Roy. Meteor. Soc., 123(544), 2477--2498.