Work Description

Title: Dataset Containing Global Modeling Results Comparing Magnetopause Distances and CPCP Open Access Deposited

http://creativecommons.org/licenses/by-nc/4.0/
Attribute Value
Methodology
  • The data are simulation results from space weather simulations conducted using space weather models on NASA Community Coordinated Modeling Center (CCMC; ccmc.gsfc.nasa.gov). The data also include observations from various in-situ and ground-based measurements of the global state of the near-Earth space environment.
Description
  • Conducting quantitative metrics-based performance analysis of first-principles-based global magnetosphere models is an essential step in understanding their capabilities and limitations, and providing scope for improvements in order to enhance their space weather prediction capabilities for a range of solar conditions. In this study, a detailed comparison of the performance of three global magnetohydrodynamic (MHD) models in predicting the Earth’s magnetopause location and ionospheric cross polar cap potential (CPCP) has been presented. Using the Community Coordinated Modeling Center’s Run-on-Request system and extensive database on results from various magnetospheric scenarios simulated for a variety of solar wind conditions, the aforementioned model predictions have been compared for magnetopause standoff distance estimations obtained from six empirical models, and with cross polar cap potential estimations obtained from the Assimmilative Mapping of Ionospheric Electrodynamics (AMIE) Model and the Super Dual Auroral Radar Network (SuperDARN) observations. We have considered a range of events spanning different space weather activity to analyze the performance of these models. Using a fit performance metric analysis for each event, we have quantified the models’ reproducibility of magnetopause standoff distances and CPCP against empirically-predicted observations, and identified salient features that govern the performance characteristics of the modeled magnetospheric and ionospheric quantities.
Creator
Depositor
  • agnitm@umich.edu
Contact information
Discipline
Funding agency
  • National Science Foundation (NSF)
  • National Aeronautics and Space Administration (NASA)
Citations to related material
  • Mukhopadhyay, A., et al. (2020). Global Magnetohydrodynamic Simulations: Performance Quantification of Magnetopause Distances and Convection Potential Predictions. Forthcoming.
Resource type
Last modified
  • 11/16/2020
Published
  • 11/16/2020
Language
DOI
  • https://doi.org/10.7302/arg3-x036
License
To Cite this Work:
Agnit Mukhopadhyay (2020). Dataset Containing Global Modeling Results Comparing Magnetopause Distances and CPCP [Data set]. University of Michigan - Deep Blue. https://doi.org/10.7302/arg3-x036

Relationships

Files (Count: 6; Size: 3.16 MB)

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#README

This directory contains files pertaining to the manuscript "Global Magnetohydrodynamic Simulations: Performance Quantification of Magnetopause Distances and Convection Potential Predictions" by Agnit Mukhopadhyay (agnitm@umich.edu), Xianzhe Jia, Daniel Welling, and Michael Liemohn.

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Simulation Results from Global Models

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Simulated magnetopause standoff distance (MPSD) and cross polar cap potential (CPCP) results may be found in the directories termed 'SWMF', 'LFM' and 'OpenGGCM', named after the global models Space Weather Modeling Framework (SWMF), Lyon-Fedder-Mobarry (LFM) global magnetohydrodynamic model, and Open Geospace General Crculation Model (OpenGGCM). The individual files for MPSD are saved as 'MPSD_Ev*.txt' where * signifies the event number in question. Theindividual files for CPCP are saved as 'CPCP_Ev*.txt' where * signifies the event number in question.

The standard output from CCMC are stored. For further information, please look up the CCMC formatting schemes at ccmc.gsfc.nasa.gov or email the author at agnitm@umich.edu

Please refer to the manuscript and/ore reference at the end for more information about the individual models.

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Magnetopause Results from Empirical Models

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MPSD results derived using the empirical results listed in Table 2 of the manuscript have been shared in the 'MPSD_EMPIR/' directory. Each empirical model has its own directory, the listing for which has been described in the following. In each directory, the individual MPSD files are saved as 'MPSD_Ev*.txt' where * signifies the event number in question.

Model Citation Directory Name


Petrinec and Russell (1993) Pet1993/
Shue et al. (1997) Shu1997/
Shue et al. (1998) Shu1998/
Kuznetsov and Suvorova (1998) Kuz1998/
Lin et al. (2010) Lin2010/
Liu et al. (2015) Liu2015/

The Python codes for each of these models and the respective IMF files used to drive the results are present in the "Code/" directory. The IMF files (indicated by 'IMF_Ev*.txt' where * is the event number) contain the time stamp (year, month, day, hour, minutes, seconds), interplanetary magnetic field values, solar wind velocity, temperature and densities used to drive each model. The results at each time stamp is saved in the 'MPSD_Ev*.txt' files in each of the aforementioned directories. To re-plot results, please use the solar wind values to aquire the time stamps, and the MPSD values directly from the individual model files.

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CPCP Results from SuperDARN and AMIE

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CPCP results derived derived from Super Dual Auroral Radar Network (SuperDARN) observations and Assimmilative Mapping of Ionospheric Electrodynamics (AMIE) techniques have been shared in the 'CPCP_OBS/' directory. Each dataset has its own directory, the listing for which has been described in the following. In each directory, the individual CPCP files are saved as 'CPCP_Ev*.txt' where * signifies the event number in question.

Dataset Directory Name


SuperDARN (Khachikjan et al. 2008) SDARN/
AMIE (Kihn and Ridley, 2005) AMIE/

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Accessing Simulation Results on NASA CCMC

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The global simulations for each event was conducted via the NASA Community Coordinated Modeling Center (CCMC; ccmc.gsfc.nasa.gov). To access individual run results, use the following keywords on "View Results/Global Magnetospheric Runs/View ALL Global Magnetospheric Runs on Request" link.


Event 1 : August 31, 2001 00:00 UT to September 1, 2001 01:00 UT

SWMF Run Name - Agnit_Mukhopadhyay_031717_1
LFM Run Name - Agnit_Mukhopadhyay_031717_3
OpenGGCM Run Name - Agnit Mukhopadhyay_031717_2


Event 2 : October 5, 2001 00:00 UT to October 6, 2001 06:00 UT

SWMF Run Name - Agnit_Mukhopadhyay_031717_4
LFM Run Name - Agnit_Mukhopadhyay_031717_6
OpenGGCM Run Name - Agnit_Mukhopadhyay_031717_5


Event 3 : September 8, 2002 18:00 UT to 23:00 UT

SWMF Run Name - Agnit_Mukhopadhyay_031717_7
LFM Run Name - Agnit_Mukhopadhyay_031717_9
OpenGGCM Run Name - Agnit_Mukhopadhyay_031717_8


Event 4 : October 29, 2003 06:00 UT to October 30, 2003 06:00 UT

SWMF Run Name - Agnit_Mukhopadhyay_031717_10
LFM Run Name - Agnit_Mukhopadhyay_031717_12
OpenGGCM Run Name - Agnit_Mukhopadhyay_070917_5


Event 5 : November 19, 2004 00:00 UT to November 20, 2004 00:00 UT

SWMF Run Name - Agnit_Mukhopadhyay_031717_13
LFM Run Name - Agnit_Mukhopadhyay_031717_12
OpenGGCM Run Name - Agnit_Mukhopadhyay_031717_14


Event 6 : February 18, 2004 14:00 UT to February 19, 2004 00:00 UT

SWMF Run Name - Agnit_Mukhopadhyay_031717_16
LFM Run Name - Agnit_Mukhopadhyay_031717_18
OpenGGCM Run Name - Agnit_Mukhopadhyay_031717_17


Event 7 : December 14, 2006 12:00 UT to December 16, 2006 00:00 UT

SWMF Run Name - CCMC_CCMC_102708_2
LFM Run Name - Spencer_Hatch_110320_1
OpenGGCM Run Name - CCMC_CCMC_123008_2

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References:

[1] Lin, R. L., Zhang, X. X., Liu, S. Q., Wang, Y. L., and Gong, J. C. (2010). A three-dimensional asymmetric magnetopause model. Journal of Geophysical Research: Space Physics 115. doi:10.1029/2009JA014235

[2] Liu, Z.-Q., Lu, J. Y., Wang, C., Kabin, K., Zhao, J. S., Wang, M., et al. (2015). A three-dimensional high mach number asymmetric magnetopause model from global mhd simulation. Journal of Geophysical Research: Space Physics 120, 5645-5666. doi:10.1002/2014JA020961

[3] Lyon, J. G., Fedder, J. A., and Mobarry, C. M. (2004). The Lyon-Fedder-Mobarry (LFM) global MHD magnetospheric simulation code. Journal of Atmospheric and Solar-Terrestrial Physics 66, 1333-1350. doi:https://doi.org/10.1016/j.jastp.2004.03.020

[4] Khachikjan, G. Y., 389 Koustov, A. V., and Sofko, G. J. (2008). Dependence of superdarn cross polar cap potential upon the solar wind electric field and magnetopause subsolar distance. Journal of Geophysical Research: Space Physics 113. doi:10.1029/2008JA013107

[5] Kihn, E. A. and Ridley, A. J. (2005). A statistical analysis of the assimilative mapping of ionospheric electrodynamics auroral specification. Journal of Geophysical Research: Space Physics 110. doi:10.1029/2003JA010371

[6] Kuznetsov, S. N. and Suvorova, A. V. (1998). An Empirical Model of the Magnetopause for Broad Ranges of Solar Wind Pressure and BZ IMF (Dordrecht: Springer Netherlands). 51-61. doi:10.1007/978-94-011-5214-3_5

[7] Petrinec, S. M. and Russell, C. T. (1993). An empirical model of the size and shape of the near-Earth magnetotail. Geophysical Research Letters 20, 2695-2698. doi:10.1029/93GL02847

[8] Raeder, J., McPherron, R. L., Frank, L. A., Kokubun, S., Lu, G., Mukai, T., et al. (2001). Global simulation of the Geospace Environment Modeling substorm challenge event. Journal of Geophysical Research-Space Physics 106, 381-395. doi:10.1029/2000ja000605

[9] Shue, J.-H., Chao, J. K., Fu, H. C., Russell, C. T., Song, P., Khurana, K. K., et al. (1997). A new functional form to study the solar wind control of the magnetopause size and shape. Journal of Geophysical Research: Space Physics 102, 9497-9511. doi:10.1029/97JA00196

[10] Shue, J.-H., Song, P., Russell, C. T., Steinberg, J. T., Chao, J. K., Zastenker, G., et al. (1998). Magnetopause location under extreme solar wind conditions. Journal of Geophysical Research: Space Physics 103, 17691-17700. doi:10.1029/98JA01103

[11] Toth, G., Sokolov, I. V., Gombosi, T. I., Chesney, D. R., Clauer, C. R., De Zeeuw, D. L., et al. (2005). Space Weather Modeling Framework: A new tool for the space science community. Journal of Geophysical Research 110, A12226. doi:10.1029/2005JA011126

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