Evolution of solar wind structures between Venus and Mars orbits

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Presentation transcript:

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%, 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

Solar wind by ENLIL simulation

Solar wind propagation Timelag calculation:  Opitz, Karrer, Wurz et al. 2009 Solar Physics

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

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. 2009 SolPhys  Opitz, Wurz, Sauvaud et al. 2012 in prep., SolPhys  time lag: 0 → CR/2 → CR → 2*CR → ... → n*CR

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

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

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

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

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

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

Solar cycle

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

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.