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Flare Irradiance Studies with the EUV Variability Experiment on SDO

Flare Irradiance Studies with the EUV Variability Experiment on SDO. R. A. Hock, F. G. Eparvier, T. N. Woods, A. R. Jones, University of Colorado at Boulder L. Didkovsky University of Southern California B. J. Thompson NASA Goddard Space Flight Center. All about EVE.

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Flare Irradiance Studies with the EUV Variability Experiment on SDO

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  1. Flare Irradiance Studies with the EUV Variability Experiment on SDO • R. A. Hock, F. G. Eparvier, T. N. Woods, A. R. Jones, University of Colorado at Boulder • L. Didkovsky • University of Southern California • B. J. Thompson • NASA Goddard Space Flight Center

  2. All about EVE PI: Tom Woods, Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder CO SCIENCE THEMES: Specify the solar EUV spectral irradiance and its variability on multiple time scales Advance current understanding of how and why the solar EUV spectral irradiance varies Improve the capability to predict the EUV spectral irradiance variability Understand the response of the geospace environment to variations in the solar EUV spectral irradiance and the impact on human endeavors

  3. Multiple EUV Grating Spectrograph (MEGS) • At 0.1 nm resolution • MEGS-A: 5-36 nm • MEGS-B: 35-105 nm • At 1 nm resolution • MEGS-SAM: 0-7 nm • At 10 nm resolution • MEGS-Photometers: @ 122 nm • Ly-a Proxy for other H I emissions at 80-102 nm and He I emissions at 45-58 nm • EUV Spectrophotometer (ESP) • At 4 nm resolution • 17.5, 25.6, 30.4, 36 nm • At 7 nm resolution • 0.1 - 7 nm (zeroth order) • Solar Aspect Monitor (SAM) • .1 - 7 nm image All about EVE

  4. All about EVE First light EVE spectrum with AIA & ESP bandpasses. EVE measures the spectral EUV irradiance from 5-105 nm with 0.1 nm spectral resolution a 10-second time cadence.

  5. Temperature Coverage of EVE Peak formation temperature from CHIANTI vs. wavelength for bright lines in a EVE spectrum (quiet Sun)

  6. Active Region Evolution 5% 3% Sub-daily variations in EUV lines are associated with AR evolution and small flares

  7. Solar Activity during Year 1 Levels of solar activity during the first year of SDO observations

  8. Space Weather & Flare Location Space Weather products are available from http://lasp.colorado.edu/eve/data_access/

  9. ...not just flares anymore 2048 pixels • EVE is proving to be a remarkable instrument for understanding the global nature of EUV irradiance variability • Future work will focus on moving from qualitative study of the EUV irradiance variability to quantitative study 1024 pixels

  10. Coronal Dimmings Coronal dimming seen in both AIA 171 channel and EVE 17.1 nm line

  11. Radiative Output of Solar Flares Four M1.0 flares have significantly different light curves in the EUV. EVE allows us to quantify how the corona cools after a flare.

  12. Flare Classification

  13. Compact FlaresC2.2 on 25 October 2010 • Non-eruptive • Cohesive group of loops brighten concurrently

  14. Localized Eruptive FlaresC4.6 on 12 November 2010 • Localized brightening associated with EUV surges • Occurs at the edge of an AR at the footpoint of a loop that connects to a different part of the AR or to another AR entirely. • Possibly the Skylab point flares previously categorized with compact flares

  15. Arcade FlaresC2.3 on 14 December 2010 • Long(ish) duration events with EUV emission lasting hours • Generally associated with filament eruptions & coronal dimmings • Arcade of post-flare loops in corona and 2-ribbon footpoints in chromosphere

  16. Late Phase FlaresC8.8 on 5 May 2010 • Two spatially-distinct but related enhancements in 2-3 MK emission tens of minutes to hours apart • Previously observed but EVE has shown that these flares have a strong and unique irradiance signature that can account for up to 40-80% of the energy radiated in the EUV

  17. Example of a Late Phase Flare Comparison of AIA and EVE lightcurves & a cartoon of the evolution of the 5 May 2010 C8.8 flare

  18. Distribution of Flare Types

  19. Distribution of Flare Types

  20. Future Work • Continue to update the flare catalog including • Adding ~150 flares from March 2011 • Adding association with CMEs • Validating impulsive phase using RHESSI data • Validating extracted parameters from EVE data • Start to associate flare parameters with physical quantities: • Loop length • Arcade length • Magnetic field strength

  21. Arcade Flare Irradiances Correlations of rise time in SXR with (1) flare duration, (2) delay in EUV peak irradiances, and (3) GOES magnitude

  22. Irradiance Flare Peak Width

  23. Impulsive PhaseMeasured by He II 30.4 nm C1.0+ C4.0+

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