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Magnetopause crossing of geosynch. orbit and magnetopause location

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Magnetopause crossing of geosynch. orbit and magnetopause location

Team Leads: Y. Collado-Vega (CCMC), S. Merkin (JHU APL) (co-lead) (email team leads to be added to the team)
Team Members: M. Collier (NASA GSFC), H. Connor (NASA GSFC), D. Cramer (UNH), K. Garcia-Sage (NASA/GSFC), M. Georgoulis (AOA), H. Hietala (UCLA), I. Honkonen (NASA GSFC), A. Kellerman (UCLA), K. Kuntz (JHU), M. Kuznetsova (CCMC), N. Lugaz (UNH), R. Lopez (UTA),S. Merkin (JHU APL), S. Petrinec (LMCO), J. Raeder (UNH), L. Rastaetter (CCMC), K. Raymer (Leicester), S. Sazykin (RICE), D. Sibeck (NASA GSFC), H. Singer (NOAA), K. Trattner (LASP), B. Walsh (BU), Chih-Ping Wang (UCLA), D. Welling (UMICH), M. Wiltberger (NCAR), K. Winters (USAF)
Communications: (mailing list)

Working Team Description
This working team will be devoted to studies of the magnetopause (MP) location, the physical processes governing it, and the ability of global geospace models to reproduce and predict it.

Working Team Goals

  • Compile a list of previous publications summarizing the observational, theoretical and modeling knowledge regarding the MP geometry, dynamics, ability of models to predict it, etc. In particular, to what extent can we claim to know where the magnetopause is at a given time and at a given location in absence of in situ data (see Samsonov et al., 2016)
  • Define/discuss the physical processes governing the MP location and to what extent different models include these processes (e.g. ring current effects).
  • Summarize/Discuss previous events and statistical studies. Consider candidate events for simulations, including recent MMS MP season.
  • Define metrics for model-data comparison; techniques used. Consider dynamics vs. morphology-mertrics can be different.
  • Discuss modeling challenges during the meeting.
  • Ongoing-Compare model outputs with data and amongts each other; and define the differences.
  • Define which model settings can affect their output significantly and relate to missing physics, if possible.
  • If possible, define how models can have better agreement
  • Define improvements/capabilities needed for better predictions

User Needs

  • Determine end users and their needs, metrics, etc.
  • Science applications thresholds to understand the parameters needed for improvement
  • Real time simulations capabilities/now casting

Working Team Deliverables

  • Support GEM and LWS Programs and Challenges. In example - Focus Group on Dayside Kinetic Processes in Global Solar WindMagnetosphere Interaction. The metrics they will obtain with a CCMC-hosted modelling challenge comparing different (kinetic) global models against near-magnetopause observations during southward IMF can be compared to the metrics established in this workshop. Also, in a long term interval these results can be compared again when better models are developed.
  • Define (if possible) some settings that could make the models have better agreement on the magnetopause location. Make those settings available to everyone.
  • Ideas on how to create an ensemble of the model predictions and make that available to the scientific community.
  • TBD after discussion at the workshop

Physical Quantities and Metrics for Model Validation

  • Model settings
  • Inside/Outside of Magnetopause decision: variable, threshold, sampling time interval

Available Data Sources
Observations, impact information

Solar wind conditions (density, IMF all directions, solar wind speed)

MP crossings by THEMIS, MMS, other platforms

Participating Models

  • SWMF
  • LFM
  • OpenGGCM
  • VERB
  • Empirical models
  • Kinetic models (long term)
  • Others

Workshop Presentations and meeting notes

Presentations given at the workshop and meeting notes available at:

Tentative Agenda and Presentations

    Wednesday at 3PM
    1. Nowcasting and forecasting of the magnetopause and bow shock—A status update (Steven Petrinec, Lockheed Martin)
    2. GEM Model Challenges; Metrics and Skill Scores already done (Lutz Rastaetter, NASA GSFC)
    3. Events Description
      • Magnetospheric balance of solar wind dynamic pressure [Jan 13, 2013 and Jun 23, 2015 events] (Ramon Lopez, UTA).
      • Comparison of MHD models and Geosync. Orbits Crossings (Yari Collado-Vega, NASA GSFC)
      • Other Events
    Wednesday at 4:45PM
  1. The last-closed drift shell (LCDS) computations (Adam Kellerman, UCLA)
  2. Scientific "end-user" requirements in regards to our VERB code simulations and real-time forecasting (Adam Kellerman, UCLA)
  3. User needs identified by SWPC (Howard Singer, NOAA SWPC)
  4. User needs identified by SWRC (Antti Pulkkinen, NASA GSFC)
  5. New developments and why validation is important for Science: Soft X-ray Imaging of the Magnetosphere (Kip Kuntz, JHU)
  6. Discussion of the 5 min team update on Thursday
Thursday at 10:45AM
National Aeronautics and Space Administration Air Force Materiel Command Air Force Office of Scientific Research Air Force Research Laboratory Air Force Weather Agency NOAA Space Environment Center National Science Foundation Office of Naval Research

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