first year of science from sdo eve

First Year of Science from SDO EVE

R. A. Hock, F. G. Eparvier, T. N. Woods, A. R. Jones, L. Didkovsky

& the rest of EVE team

rachel.hock@lasp.colorado.edu

Laboratory for Atmospheric and Spaces PhysicsUniversity of Colorado Boulder

Woods et al., ApJ 2011 (accepted) & Hock, PhD Thesis

What does EVE measure?

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First light EVE spectrum with AIA & ESP bandpasses. EVE measures the spectral EUV irradiance from 5-105 nm with 0.1 nm spectral resolution an 10-second time cadence. AAS/SPD 2011 Las Cruces, NM

Temperature Coverage of EVE

Peak formation temperature from CHIANTI vs. wavelength

for bright lines in a EVE spectrum (quiet Sun)AAS/SPD 2011 Las Cruces, NM

Solar Activity during Year 1

Levels of solar activity during the first year of SDO observations

AAS/SPD 2011 Las Cruces, NM

Space Weather & Flare Location

Space Weather products are available from http://lasp.colorado.edu/eve/data_access/

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AAS/SPD 2011 Las Cruces, NM

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. AAS/SPD 2011 Las Cruces, NM

Flare Classification

AAS/SPD 2011 Las Cruces, NM

Compact FlaresC2.2 on 25 October 2010

✴ Non-eruptive

✴ Cohesive group of loops brighten concurrently

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AAS/SPD 2011 Las Cruces, NM

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 be the Skylab point flares previously categorized with compact flares

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AAS/SPD 2011 Las Cruces, NM

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

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AAS/SPD 2011 Las Cruces, NM

Arcade Flare Irradiances

Correlations of rise time in SXR with

(1) flare duration, (2) delay in EUV peak

irradiances, and (3) GOES magnitude

AAS/SPD 2011 Las Cruces, NM

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

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AAS/SPD 2011 Las Cruces, NM

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

AAS/SPD 2011 Las Cruces, NM

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Coronal Dimmings

Coronal dimming seen in both AIA 171 channel and EVE 17.1 nm line AAS/SPD 2011 Las Cruces, NM

Active Region Evolution

Sub-daily variations in EUV lines are associated with AR evolution and small flares AAS/SPD 2011 Las Cruces, NM

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5%

3%

The Future

✴ 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

AAS/SPD 2011 Las Cruces, NM