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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. Solar wind.  Pizzo 1978 JGR. Continuous radial supersonic particle flow Quasi-neutrality: electrons and ions H + 96%, He 2+ 4%

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Evolution of solar wind structures between Venus and Mars orbits

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  1. 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. 2009 Solar Physics

  5. Solar wind properties STEREO = Solar Terrestrial Relations Observatory  Opitz, Karrer, Wurz et al. 2009 Solar Physics STEREO PLASTIC ion experiment

  6. Temporal evolution: 360º STEREO mission 2007 March 1 − 2011 February 7: α = 0º → 180º β = 360º → 180º Carrington rotation: 27.28 days = 360º β α  Opitz, Karrer, Wurz, et al. 2009 SolPhys  Opitz, Wurz, Sauvaud et al. 2012 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. 2012 Solar Physics, in preparation

  8. Solar wind prediction V = Venus E = Earth 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 (%) 0

  10. Earth STA STB SOHO  Opitz, Fedorov, Wurz et al. 2010a, SolPhys 100 Goodness (%) 0

  11. Mars STA STB MEX  Opitz, Fedorov, Wurz et al. 2010a, SolPhys 100 Goodness (%) 0

  12. SIR interaction with Mars 2008-01-01 00:00 UT Right plot created with AMDA tool  see poster by N. Andre

  13. Solar cycle

  14. Arbitrary CME http://www.helio-vo.eu/

  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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