Insights into Solar Wind Charge Exchange in the Solar System

Exploring the intricacies of solar wind charge exchange within the solar system, this content delves into plasma interactions, forbidden lines, and the unique environments provided by comets. Discussions on spatial and temporal variations, neutral chemical compositions, and spectroscopic analyses shed light on the fascinating phenomena surrounding solar wind interactions.

• Solar Wind
• Charge Exchange
• Comets
• Plasma Interactions
• Forbidden Lines

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1. Dennis Bodewits Diagnostics of solar wind charge exchange 2020-08 AtomDB workshop dennis@auburn.edu

2. Charge exchange Solar wind 1-2 MK plasma Collisionless 250 1000 km/s variable <1.5 KeV Simple molecules Forbidden lines

3. Solar wind charge exchange in the solar system Swift UVOT +XRT observations of Comet Lulin; Bodewits et al. 2012, Carter et al. 2012, APOD 2009/02/21 Bhardwaj et al. 2007 ; Dennerl et al. 2012; Branduardi et al. 2017

4. ESA/ China Solar Wind Magnetosphere Ionosphere Link Explorer (SMILE) http://sites.bu.edu/cupid/ https://sci.esa.int/web/smile/-/59312-science-with-smile

5. Planets! Comets! Our space telescopes! Ugh, this is so NASA Ooh, solar wind! \_( )_/ Wait, fusion??

6. Comets are cool! Comets provide different environments Move around solar system (rh, latitude) Activity levels (collisionally thick/thin) Spatial: Comets are extended sources Plasma interaction regions Neutral distribution Temporal variation Comet outbursts Solar wind variations (CMEs, flares, shocks) Spectroscopy Solar wind origins (freeze in temperature) Forbidden lines: astronomical lab Neutral chemical composition (H2O, CO2, CO, ..) Dust?

7. Comets are cool! Comets provide different environments Move around solar system (rh, latitude) Activity levels (collisionally thick/thin) Spatial: Comets are extended sources Plasma interaction regions Neutral distribution Temporal variation Comet outbursts Solar wind variations (CMEs, flares, shocks) Spectroscopy Solar wind origins (freeze in temperature) Forbidden lines: astronomical lab Neutral chemical composition (H2O, CO2, CO, ..) Dust? Lisse et al. 2005

8. ESA/Rosetta Comets are cool! Comets provide different environments Move around solar system (rh, latitude) Activity levels (collisionally thick/thin) Spatial: Comets are extended sources Plasma interaction regions Neutral distribution Temporal variation Comet outbursts Solar wind variations (CMEs, flares, shocks) Spectroscopy Solar wind origins (freeze in temperature) Forbidden lines: astronomical lab Neutral chemical composition (H2O, CO2, CO, ..) Dust? ESA/NASA SOHO

9. C+N OVII OVIII Comets are cool! Comets provide different environments Move around solar system (rh, latitude) Activity levels (collisionally thick/thin) Spatial: Comets are extended sources Plasma interaction regions Neutral distribution Temporal variation Comet outbursts Solar wind variations (CMEs, flares, shocks) Spectroscopy Solar wind origins (freeze in temperature) Forbidden lines: astronomical lab Neutral chemical composition (H2O, CO2, CO, ..) Dust? Solar wind freeze-in Temperature Bodewits et al. A&A 2007

10. Comets are cool! Comets provide different environments Move around solar system (rh, latitude) Activity levels (collisionally thick/thin) Spatial: Comets are extended sources Plasma interaction regions Neutral distribution Temporal variation Comet outbursts Solar wind variations (CMEs, flares, shocks) Spectroscopy Solar wind origins (freeze in temperature) Forbidden lines: astronomical lab Neutral chemical composition (H2O, CO2, CO, ..) Dust? Bockelee-Morvan et al. 2017

11. OVII emission from different electron donors Kronos package; O7+ + x O6+* @ 311 km/s (Mullen et al. 2017) K f H2O CO2 O Difference relative strength fir Different K-series K i K K r CO2, CO, C: similar fir, K- strong H2O, H, OH, O: stronger f, K- strong K K

12. XMM-RGS spectrum of Mars Halo CO2: similar fir, K- strong H2O, O: stronger f, K- strong f K- Journal of Geophysical Research: Planets, Volume: 122, Issue: 12, Pages: 2401-2428, First published: 08 November 2017, DOI: (10.1002/2017JE005336) Dennerl et al. 2006, A&A http://www.lpl.arizona.edu/~hubbard/Pty S206/Lectures3/Mar06.htm Why is the K-d strong? atomic oxygen! Wikipedia

13. Thank you! dennis@auburn.edu Don t miss: 10:45: Emanuele Bonamente, Charge exchange from comets with NICER 10:50: Steve Bromley, COLTRIMS of bare highly charged ions and simple molecules