Model:WACCM-EE: Difference between revisions

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{{Model identity2
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|Categories=Climate
|ModelDomain=Climate
|One-line model description=GCM for deep paleoclimate studies
|One-line model description=GCM for deep paleoclimate studies
|Extended model description=I am developing a GCM based on NCAR's WACCM model to studied the climate of the ancient Earth. WACCM has been linked with a microphysical model (CARMA). Some important issues to be examined are the climate of the ancient Earth in light of the faint young Sun, reducing chemistry of the early atmosphere, and the production and radiative forcing of Titan-like photochemical hazes that likely enshrouded the Earth at this time.
|Extended model description=I am developing a GCM based on NCAR's WACCM model to studied the climate of the ancient Earth. WACCM has been linked with a microphysical model (CARMA). Some important issues to be examined are the climate of the ancient Earth in light of the faint young Sun, reducing chemistry of the early atmosphere, and the production and radiative forcing of Titan-like photochemical hazes that likely enshrouded the Earth at this time.
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|CCA component=No but possible
|CCA component=No but possible
|IRF interface=No but possible
|IRF interface=No but possible
|CMT component=Not yet
|CMT component=No but possible
}}
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== References  ==
== References  ==
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== Issues ==
== Issues ==

Latest revision as of 20:16, 16 September 2020



WACCM-EE


Metadata

Also known as
Model type Modular
Model part of larger framework
Note on status model
Date note status model
Spatial dimensions
Spatial extent
Model domain Climate
One-line model description GCM for deep paleoclimate studies
Extended model description I am developing a GCM based on NCAR's WACCM model to studied the climate of the ancient Earth. WACCM has been linked with a microphysical model (CARMA). Some important issues to be examined are the climate of the ancient Earth in light of the faint young Sun, reducing chemistry of the early atmosphere, and the production and radiative forcing of Titan-like photochemical hazes that likely enshrouded the Earth at this time.
Keywords:

paleoclimate,

Name Eric Wolf
Type of contact Model developer
Institute / Organization University of Colorado, ATOC
Postal address 1 Campus Box 392
Postal address 2
Town / City Boulder
Postal code 80309
State Colorado
Country United States
Email address eric.wolf@colorado.edu
Phone 240-461-8336
Fax


Supported platforms
Unix, Linux, Mac OS
Other platform
Programming language

Fortran77, Fortran90

Other program language
Code optimized
Multiple processors implemented
Nr of distributed processors
Nr of shared processors
Start year development 2008
Does model development still take place? Yes
If above answer is no, provide end year model development
Code development status
When did you indicate the 'code development status'?
Model availability As code
Source code availability
(Or provide future intension) 		Through web repository
Source web address http://www.cesm.ucar.edu/working_groups/WACCM/
Source csdms web address
Program license type GPL v2
Program license type other
Memory requirements 1GB for input data
Typical run time 1.5 days per model year on 8 processor mac


Describe input parameters GCM initial conditions files (netcdf) files describe initial state of atmosphere up ~km 140
Input format
Other input format NetCDF
Describe output parameters netcdf output files describing atmospheric state, chemistry, etc
Output format
Other output format NetCDF
Pre-processing software needed? No
Describe pre-processing software
Post-processing software needed? Yes
Describe post-processing software IDL igeov viewer (IDL procedure)
Visualization software needed? Yes
If above answer is yes IDL
Other visualization software


Describe processes represented by the model General circulation model of early Earth. Particular detail is paid to chemistry, RT, and haze microphysics
Describe key physical parameters and equations Equations focused on are the radiative transfer equations, and equations governing haze microphysics
Describe length scale and resolution constraints Currently, 4x5 degree, with 66 vertical levels up to 140 km. Resolution can be increased if neccessary
Describe time scale and resolution constraints The model takes about 4-6 model years to reach equilibrium. The modeled time period is from the Archean Earth (3.8 - 2.5 Ga)
Describe any numerical limitations and issues Dynamics, chemistry, RT, microphysical, and slab ocean model are all coupled, thus the model runs slowly.


Describe available calibration data sets Haze microphysics can be checked against Bardeen 2008 for initial accuracy.
Upload calibration data sets if available:
Describe available test data sets I have numerous data sets produced by an 8 processor Mac and a local unix cluster to confirm the model is initialized correctly.
Upload test data sets if available:
Describe ideal data for testing Cassini data describing Titan photochemical haze. Laboratory work constraining haze properties.


Do you have current or future plans for collaborating with other researchers? Yes, I plan on collaborating with others in particular when it comes time to rework the model chemistry modules.
Is there a manual available? Yes
Upload manual if available:
Model website if any CCSM
Model forum / discussion board
Comments The Early earth haze microphysical code is working, incorporating fractal particle structures. Development is needed on linking microphysics to RT.

NOTICE: REGISTRATION IS NEEDED TO RECEIVE THE SOURCE CODE. SEND THE OWNER A LETTER THAT YOU ARE INTERESTED IN THE SOURCE CODE.

http://www.cesm.ucar.edu/working_groups/WACCM/


This part will be filled out by CSDMS staff

OpenMI compliant No but possible
BMI compliant No but possible
WMT component No but possible
PyMT component
Is this a data component
Can be coupled with:
Model info
Authors
Eric Wolf
Source code
Model citations
Nr. of publications: 1
Total citations: 188
h-index: 1
m-quotient: 0.06
QR-code

Link to this page
Other models by author



Introduction

History

References



Nr. of publications: 1
Total citations: 188
h-index: 1
m-quotient: 0.06



Featured publication(s)YearModel describedType of ReferenceCitations
Bardeen, C. G.; Toon, O. B.; Jensen, E. J.; Marsh, D. R.; Harvey, V. L.; 2008. Numerical simulations of the three-dimensional distribution of meteoric dust in the mesosphere and upper stratosphere. Journal of Geophysical Research, 113, D17202. 10.1029/2007JD009515
(View/edit entry)		2008 WACCM-EE
 Model overview 188
See more publications of WACCM-EE


Issues

Help

Input Files

Output Files

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