1 / 18

UV Spectroscopy of CME Currrent Sheets

UV Spectroscopy of CME Currrent Sheets. John Raymond Angela Ciaravella Silvio Giordano Dave Webb. Overview. Reconnection occurs between the flare loops and the CME core. It converts magnetic energy to heat, Kinetic energy and energetic particles. It releases the overlying magnetic

jerica
Download Presentation

UV Spectroscopy of CME Currrent Sheets

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. UV Spectroscopy of CMECurrrent Sheets John Raymond Angela Ciaravella Silvio Giordano Dave Webb

  2. Overview Reconnection occurs between the flare loops and the CME core. It converts magnetic energy to heat, Kinetic energy and energetic particles. It releases the overlying magnetic arches, allowing CME to escape. It creates or adds to a twisted magnetic flux rope. It is crucial to areas of astrophysics, such as accretion disks. Lin & Forbes Model

  3. Current Sheet Models Petschek Turbulent Lazarian & Vishniac Tajima & Shibata Vršnak

  4. Diagnostics Temperature e.g., [Fe XVIII], [Fe XXI], X-rays Density Combine emission measure with column density Thickness Projection effects? Turbulent Speed Line widths (correct for thermal speed) Reconnection rate Inflow/outflow speeds; blobs, filaments (Yokoyama; Lin et al.)

  5. Innes et al. 2002 Apr 21, TRACE 195

  6. Reconnection Current Sheets Magnetic Reconnection is poorly understood. It heats and accelerates gas, produces energetic particles. Spectra determine electron and ion temperatures, densities, turbulence. Post-flare Arcade UV: High temperature feature between flare loops and CME CME Core [Fe XVIII] -- 6 x 106 K Lower T lines Ciaravella et al.

  7. 302° 1.66 R☼ 262° 228° November 4, 2003 CME Current Sheet Current Sheet Ciaravella & Raymond

  8. 2003 November 4 CS: Images [Fe XVIII] emission begins ~ 8 min after the CME “ “ peak move by ~ 4° south in 2.5 h narrows and becomes constant Si XII emission starts about 2h later: implies cooling OVI and CIII are patchy: cold plasmoids are detected offset from hot emission CS in MLSO-MK4 provides Ne

  9. time (UT) PA Fe XVIII Si XII logT EM Ne ne d ph/(cm2 sec sr) 1025 cm-5 1017 cm-2 107 cm-3 R¤ 17:20-19:09 251.6-261.9 1.39 11.0 6.61 2.4 20:27-21:00 251.6-261.9 5.13 6.83 6.81 3.1 21:06-21:28 251.6-258.9 6.44 6.59 6.90 4.4 4.5 9.8 0.07 22:03-22:35 251.6-257.5 5.74 6.95 6.79 3.4 4.9 7.0 0.10 23:19-00:02 251.6-256.0 4.06 9.95 6.72 3.4 5.0 6.8 0.11 00:42-01:38 251.6-254.5 1.46 9.61 6.62 2.4 5.9 4.1* 0.21* 03:29-04:57 250.2-257.5 1.10 7.72 6.62 1.8 MLSO Mark IV pB [Fe XVIII] Temperature and density in the CS decrease with time

  10. Do Blob motions give Alfvén speed? Sometimes. 400 km/s 5 x 1012 g Traces back to C III blob

  11. Turbulent (?) Line Widths vs. Time ~130 km/s TION Bemporad 2008

  12. Landi et al. 2012 - Cartwheel CME

  13. Landi et al. -- Cartwheel CME

  14. Landi et al. Effective Temperature from Fe XII and Fe XV linewidths ~ 110 km/s FWHM ~ 85 km/s

  15. White Light rays: 03/10/04 Ciaravella et al. MLSO + LASCO Many hours O VI displaced South Si XII broad O VI Fe XVIII Si XII

  16. [Fe XVIII] offset from O VI; Si XII is diffuse Sep 21, 2001

  17. [Fe XVIII] intensity poorly correlated with CME speed [Fe XVIII] intensity poorly correlated with height Observing bias?

  18. Summary Temperatures; 3 to 8 to 15 MK Slow cooling Densities: 4 to 10 x107 at 1.7 RSUN Thickness: 0.01 to 0.1 RSUN projection effects not all that bad Turbulent speed: ~ 100 km/s, slowly decreasing Reconnection rate: 0.01 to 0.1

More Related