Wenhui Li and Joachim Raeder
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OpenGGCM Simulation vs THEMIS Observations in an Dayside Event PowerPoint PPT Presentation


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Wenhui Li and Joachim Raeder University of New Hampshire Marit Øieroset University of California, Berkeley THEMIS 2008 UCLA. OpenGGCM Simulation vs THEMIS Observations in an Dayside Event. THEMIS Observations on 06/03/2007 ( Øieroset et. al. 2008). Northward IMF with strong By

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OpenGGCM Simulation vs THEMIS Observations in an Dayside Event

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Openggcm simulation vs themis observations in an dayside event

Wenhui Li and Joachim Raeder

University of New Hampshire

Marit Øieroset

University of California, Berkeley

THEMIS 2008 UCLA

OpenGGCM Simulation vs THEMIS Observationsin an Dayside Event


Themis observations on 06 03 2007 ieroset et al 2008

THEMIS Observations on 06/03/2007(Øieroset et. al. 2008)

  • Northward IMF with strong By

    during ~15:25 -- ~17:00 UT

  • THEMIS-B in the magnetosheath

  • THEMIS-A, C, D and E detect a layer of nearly-stagnant magnetosheath plasma (T ~ 1 keV, N ~ 3-6 cm-3) attached to the magnetopause on closed field lines

  • From TH-D to TH-A, magnetospheric ion and electron flux increases

  • Thickness of the layer ~ 0.9 RE

  • No evidence for Kelvin-Helmholtz waves nor diffusion at the local magnetopause

  • Particle distributions suggest double-high latitude reconnection involving the same field lines


Themis observations on 06 03 2007 ieroset et al 20081

THEMIS Observations on 06/03/2007(Øieroset et. al. 2008)


Openggcm simulation vs themis a observations

OpenGGCM Simulation vs THEMIS-A Observations

NIMF CDPS MP


Openggcm simulation vs themis e observations

OpenGGCM Simulation vs THEMIS-E Observations

NIMF CDPS M.P.


Openggcm simulation vs themis c observations

OpenGGCM Simulation vs THEMIS-C Observations

NIMF CDPS M.P.


Openggcm simulation vs themis d observations

OpenGGCM Simulation vs THEMIS-D Observations

NIMF CDPS M.P.


Openggcm simulation vs themis b observations

OpenGGCM Simulation vs THEMIS-B Observations

M.P. NIMF


Openggcm simulation vs themis observations thickness of the cold dense plasma layer

OpenGGCM Simulation vs THEMIS Observations-- Thickness of the cold dense plasma layer

THEMIS: ~ 1.1 RE along THEMIS track

Simulation: ~ 1.3 RE

values on the line passing THA at 16:30 UT

CDPL

IMF

Open layer

~1.3


How the cold dense plasma layer forms

How the cold dense plasma layer forms?

  • Double high-latitude reconnection captures magnetosheath plasma

Solar Wind


How the cold dense plasma layer forms1

How the cold dense plasma layer forms?

2. New closed flux tubes slowly convect

around magnetopause toward nightside

-- results in a balance of inflow and outflow at dayside magnetopause

and form a cold dense plasma layer

Magnetic nulls

Solar wind

Frozen-in field lines

An entry flow path

(Li et. al. 2005)


Summary

Summary

  • THEMIS observed cold dense plasma layer in dayside closed field attached to magnetopause

  • The multi spacecrafts estimated the thickness of the cold dense plasma layer to be ~0.9 RE

  • An OpenGGCM simulation reproduces the THEMIS observations

  • Observations and simulation analysis indicate that double high-latitude reconnection causes the formation of this cold dense plasma layer


Additional information

Additional Information

A comprehensive study of magnetosphere under northward IMF conditions using OpenGGCM simulations can been found in:

Solar wind plasma entry into the magnetosphere under northward IMF conditions

Li et. al. 2008, JGR, newly published


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