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Evolution of solar wind structures between Venus and Mars orbits

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Presentation on theme: "Evolution of solar wind structures between Venus and Mars orbits"— Presentation transcript:

1 Evolution of solar wind structures between Venus and Mars orbits
YouResAstro 2012 in Budapest, 3-6 Sept 2012 Evolution of solar wind structures between Venus and Mars orbits Andrea Opitz Velence, Hungary

2 Solar wind  Pizzo 1978 JGR Continuous radial supersonic particle flow
Quasi-neutrality: electrons and ions H+ 96%, He2+ 4% heavies (C, N, O, Ne, Mg, Si, Fe) Fully ionized dilute plasma Interplanetary magnetic field lines frozen-in (Parker spiral) SIR characteristics: Higher density Higher magnetic field Magnetic field rotation Enhanced energetic ion flux CIR = Corotating interaction region

3 Solar wind by ENLIL simulation

4 Solar wind propagation
Timelag calculation:  Opitz, Karrer, Wurz et al Solar Physics

5 Solar wind properties STEREO = Solar Terrestrial Relations Observatory
 Opitz, Karrer, Wurz et al Solar Physics STEREO PLASTIC ion experiment

6 Temporal evolution: 360º β STEREO mission α
2007 March 1 − 2011 February 7: α = 0º → 180º β = 360º → 180º Carrington rotation: 27.28 days = 360º α  Opitz, Karrer, Wurz, et al SolPhys  Opitz, Wurz, Sauvaud et al in prep., SolPhys  time lag: 0 → CR/2 → CR → 2*CR → ... → n*CR

7 Temporal evolution of the solar wind
 from 0.1 day up to several Carrington rotations:  Solar wind bulk velocity 1 hour averages over 1 Carrington rotation time window.  Opitz, Wurz, Sauvaud et al Solar Physics, in preparation

8 Solar wind prediction V = Venus E = Earth 2007 August M = Mars
A = STEREO Ahead B = STEREO Behind 2007 August  Opitz, Fedorov, Wurz et al. 2010a, SolPhys

9 Venus STA STB VEX  Opitz, Fedorov, Wurz et al. 2010a, SolPhys 100
Goodness (%)

10 Earth STA STB SOHO  Opitz, Fedorov, Wurz et al. 2010a, SolPhys 100
Goodness (%)

11 Mars STA STB MEX  Opitz, Fedorov, Wurz et al. 2010a, SolPhys 100
Goodness (%)

12 SIR interaction with Mars
:00 UT Right plot created with AMDA tool  see poster by N. Andre

13 Solar cycle

14 Arbitrary CME

15 Conclusion Sun and solar wind conditions are well observed both remote and in-situ in real-time. Study of their effects on planetary environments is strongly supported by heliospheric modeling. Solar community can provide solar input prediction by different propagation methods and event selection.

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