Daniel Heyner, Christian Nabert, Evelyn Liebert, Karl-Heinz Glassmeier

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Presentation transcript:

Concerning the Reconnection-Induction Balance at the Magnetopause of Mercury Daniel Heyner, Christian Nabert, Evelyn Liebert, Karl-Heinz Glassmeier BepiColombo-MESSENGER Workshop 2015

Compression & Erosion compressed eroded “Onion Peel Model” normal 1:38 IMF Abk. Return Flux! normal

Dayside MP-Erosion Processes at Mercury Onion-Peel model: imbalance in flux transport Field-aligned R1 Currents: fringe fields Open magnetosphere: IMF penetration Neutral sheet current: fringe fields Proximity of the planet: Role of induced fields? First step: Quantify external field change. 1:22

Induction as Consequence of Erosion Reconnection transports magnetic flux to the nightside Magnetopause (currents!) moves closer to planet External field amplification Slavin et al., (2014)  Induced currents Secondary fields enhance subsolar magnetospheric field (counteracting their source) 2:15

Tail flux 2 … 3.5-fold enhancement Tail Loading Events Slavin et al., (2010) Slavin et al. (2010) : Tail flux 2 … 3.5-fold enhancement 2-3 min 2:16

External Field from Neutral Sheet Currents dipole field Enhanced tail flux (Slavin et al., (2010) & Johnson et al., (2012)): 1:27

Spherical Harmonic Analysis 2:28 SHA results Subsolar point!

Solve induction equation Induction Modeling Solve induction equation Rikkitake-factor Liebert, (2013) 2:00 Induction modeling with nested shells Rikitake factor: real part, imaginary part

2 Shell Model: Results T=3min Amplitude ratio (surface) Skin Depth Induction results Low silicate shell conductivity: external field only reacts to the core High silicate shell conductivity: external field reacts to the crust Geometric decrease to r = 1.45 RM: 0.33 Maximum effect:

During phases of subsolar reconnection: tail field enhancement Summary During phases of subsolar reconnection: tail field enhancement Major effect in decreasing subsolar magnetopause distance Induction in the planetary interior may compensate for app. 20…40% (at average magnetopause distances) Outlook to Bepi Colombo: Two probes Time lag

Bz from Various Sources (Y=Z=0) Enhanced tail field Normal tail field 2:11 Externe Feldanteile

Terrestrial Dayside MP-Erosion (empirical) Stationary erosion: Delayed convective flux return from the nightside Saturation for strong negative BIMF,z Shue et al. (1998) 1:12

Magnetic field is amplified (dynamo effect) Fieldline Stretching Fieldline stretching Magnetic field is amplified (dynamo effect) Reconnected dayside flux Enhanced tail flux (Slavin et al., (2010) & Johnson et al., (2012)): 0:48 Verstärkung durch Verlängerung -> also keine komplette Erosion der tagseitigen Magnetosphäre wie von Slavin angenommen

Compression & Erosion II Pressure balance at magnetopause yields: Taking into account the effect of erosion due to reconnection: Erosion – compression law Leicht anderer Exponent für Merkur

Parabolic Magnetosphere Model Alexeev et al. (2008) 0:25 Johnson used Messenger orbital data to obtain average model Average model control parameters from Johnson et al. (2012), who analysed orbital Messenger data.

IMF Penetration

Comparison of Erosion Effects

Rikitake-Factor for a 2-shell model Induction parameter

Induction Modelling

R1 Currents R1 Ströme, Bild von Anderson

n Bz dBz t