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Effects of Solar Storms on the Venusian Ionosphere: Comparisons with Mars

This study explores how solar storms impact the Venusian ionosphere and compares the results with Mars. Examining data from NASA and previous research, the study delves into the response of Venusian 557.7nm intensity to solar storms, electron impact, emissions, and aurora occurrences before and after coronal mass ejections (CMEs). Findings reveal changes in electron density and green line emission, shedding light on ionospheric alterations post-CME impact.

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Effects of Solar Storms on the Venusian Ionosphere: Comparisons with Mars

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  1. Effects of Solar Storms on the Venusian Ionosphere International Venus Conference April 7, 2016 Candace Gray - New Mexico State University Nancy Chanover, Tom Slanger, Karan Molaverdikhani, Kerstin Peter, Bernd Häusler, Silvia Tellman, Martin Pätzold, Oliver Witasse, Pierre-Louis Blelly, Glyn Collinson NASA Earth and Space Science Fellowship Award #NN12AM70H

  2. How does Venusian 557.7nm intensity respond to solar storms? • Emitting altitude and key chemical processes? • How does the Venusian ionosphere respond to CMEs? • How do these results compare with Mars?

  3. Variable • Solar wind • Charge particle precipitation • Electron impact • O2+ + e → O(1S, 1D) + O(3P) Zhang et. al 2012

  4. Emission expected to be present • Not detected in 1970s

  5. Venus Earth Venus Earth Keck Slanger et al. 2001

  6. X-class solar flares • Strongest flares • Brightest EUV emission • Nightglow • Short duration (min - hours) • Coronal mass ejections (CMEs) • Plasma ejection • Aurora • 1 - 2 day arrival time

  7. 3.5 m Astrophysical Research Consortium (ARC) Telescope • ARC Echelle Spectrograph • High resolution (R ~ 35,000) • 3500 – 10,000 Å • Two 6-week windows / 2 years

  8. Telescope override • 3 nights/window • Storm chasing

  9. Gray et. al 2014

  10. Solar Flare Solar Flare + CME Solar Flare Before and after CME

  11. June 15 and June 16, 2012 • Before and after CME flare Electron Energy Density June 15, 2012 June 16, 2012 Nightside Nightside Energy (eV) 105 1000 Flux (cm-2 sr-1 s-1) 100 104 10 103 1 Differential Energy Flux (cm-2 sr-1 ev-1 s-1) Differential Energy Flux (cm-2 sr-1 ev-1 s-1) 107 107 106 106 12 eV 12 eV 105 105 50 eV 70 eV 104 104 103 103 103 103 1 10 100 1 10 100 1 10 100 1 10 100 1 10 100 1 10 100 Electron Energy (eV) Electron Energy (eV) Gray et al. 2016, submitted

  12. Dayside • Persistent V1 and V2 layers • Solar flux • Nightside • Variable • Ion flow across terminator Martin Pätzold et al. 2007

  13. 200 Before CME After CME 180 Altitude (km) 557.7 nm detection 160 V2 140 140 V1 120 100 0 0.5 1.0 1.5 2.0 Electron Density x 104 (cm-3)

  14. M2 M1

  15. TRANSCAR • VEX electron flux and energy inputs • Compare pre/post CME green line emission • Increase in 557.7nm emission • O + e strongest source • No increase in V1 layer electron density

  16. What happens to Venus after a CME impact? • Increased solar wind dynamic pressure • Compressed ionosphere • “Disappearing” V2 layer • Electron precipitation • Auroral emission Russell et. al 2006

  17. Brace and Kilore 1999 200 Before CME After CME 180 Altitude (km) 180 160 160 V2 140 140 V1 120 100 0 0.5 1.0 1.5 2.0 Electron Density x 104 (cm-3)

  18. Green line a unique aurora • O + e likely source of green line emission • Increase in dynamic pressure from a CME • Compress ionopause, restricting ion flow • Reduce V2 electron density • Drive plasma to the nightside • Increase green line emission • Typical of non-magnetic planets?

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