Flare Observations from SDO EVE

Flare Observations from SDO EVEFlare Observations from SDO EVEFlare Observations from SDO EVEFlare Observations from SDO EVE

Phillip C. ChamberlinPhillip C. Chamberlin - - [email protected]@nasa.gov

NASA Goddard Space Flight Center, Solar Physics LaboratoryNASA Goddard Space Flight Center, Solar Physics Laboratory

T. N. Woods, R. A. Hock, F. G. EparvierT. N. Woods, R. A. Hock, F. G. EparvierU of Colorado, Laboratory for Atmospheric and Space PhysicsU of Colorado, Laboratory for Atmospheric and Space Physics

D. L. Judge, L. Didkovsky, S. WiemanD. L. Judge, L. Didkovsky, S. WiemanU of Southern California, Space Science LaboratoryU of Southern California, Space Science Laboratory

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OutlineOutline

• The Extreme ultraviolet Variability Experiment - EVE

• Plot explanation and examples• Solar flares studied

• Impulsive phase differences (Short)• Long-term coronal heating (Long)• Comparisons to the Flare Irradiance Spectral

Model - FISM

• Conclusions and Future Work• Many questions to answer• Coordination is the key

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Flares StudiedFlares StudiedEVE/AIA Science Team Meeting - July 2010EVE/AIA Science Team Meeting - July 2010• Medium magnitude flares with impulsive

phase.• June 12 - M2.0

• Small magnitude flare with no impulsive phase.• May 7 - C2.0

• Other flare studied but not shown here• May 5 - C8.8 • May 23-24 - B1.0

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MEGS SpectrumMEGS Spectrum

• Use peak of contribution function (from CHIANTI 6.0) to pull out and combine lines.

• Normalized time series are then compiled.• Absolute energy analysis in the future.

MEGS A1MEGS A2MEGS BWarren, 2001

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MEGS Temperature ContourMEGS Temperature Contour

• Time (X-axis) vs Temp (Y-axis)• X-axis: Hours (.Fraction of Hours)• Y-axis: Log(T) from 4.5 to 7.3 in 0.1 steps

• Use peak of contribution function for each of ~90 ions used

• Normalized values from Blue (0) to red to orange to yellow (1)

Tem

pera

ture

- lo

g(T

)

4.5

5.0

5.5

6.0

6.5

7.0

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MEGS Temperature Time SeriesMEGS Temperature Time Series

• Normalized irradiance for each 0.1 log(T) bin from 4.5 to 7.3.• See impulsive phase enhancements in cooler emissions, and

cooling in hot emissions.• Smoothing to longer time scales to eliminate ‘noise’

• May be actual solar variations

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ESP Time SeriesESP Time Series

• ESP contains broad-band diodes around a strong emission line - but are sensitive to many blends.

• 0.25 Second temporal resolution.• 0.1-7nm channel correlates with GOES XRS 0.1-

0.8nm (long) channel.

ESP BL9 Flight (2006) and Rocket (2008)

-1.00E-060.00E+001.00E-062.00E-063.00E-064.00E-065.00E-066.00E-067.00E-06

15 20 25

Wavelength, nm

Efficiency, cnt/ph

Ch8R

Ch8F

ESP BL9 Flight (2006) and Rocket (2008)

-5.00E-07

0.00E+00

5.00E-07

1.00E-06

1.50E-06

2.00E-06

25 30 35

Wavelength, nm

Efficiency, cnt/ph

Ch9R

Ch9F

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June 12, 2010; M2.0 - AIAJune 12, 2010; M2.0 - AIA

Movie Courtesy K. Schrijver, LMSAL

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June 12, 2010; M2.0 - ShortJune 12, 2010; M2.0 - Short

• Peak 00:57 UT; DOY 163• Gradual hot thermal emission decay for log(T)>6.8.• Coordinated 2nd Peaks (but, other small flares)• Impulsive phase seen in log(T) < 6.4

• 7 of 10 flares have an impulsive phase (larger)

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June 12, 2010; M2.0 - LongJune 12, 2010; M2.0 - Long

• Peak 00:57 UT; DOY 163• Gradual hot thermal emission decay for log(T)>6.8.• Coordinated 2nd/3rd Peaks (but, other small flares).• Enhance 0.8-8MK plasma for ~5 hours after plots

end.

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May 7, 2010; C2.0 - AIAMay 7, 2010; C2.0 - AIA


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May 7, 2010; C2.0 - ShortMay 7, 2010; C2.0 - Short

• GOES XRS Peak: 7:42 UT; DOY 127.• 2 Soft X-Ray peaks with gradual thermal cooling.• No impulsive phase - 3/10 flare observed “Compact”?• RHESSI derived EM (White) and Temp (Black, /2).

• RHESSI and HINODE/EIS can provide more information

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• GOES X-Ray Peak: 7:42 UT; DOY 127.• 2 Soft X-Ray peaks with gradual thermal cooling.• No impulsive phase - 3/10 flare observed “Compact”?• EVE/ESP EUV emission all peak simultaneously and

after the Soft X-Ray (0.1-7nm) peaks.

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May 7, 2010; C2.0 - LongMay 7, 2010; C2.0 - Long

• Peak: 7:42 UT; DOY 127• Long, gradual cooling (>13 hours)• But, increased emissions in later peak are still seen in

log(T)>7.0 - another, more gradual flare?

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• Peak: 7:42 UT; DOY 127• Long, gradual cooling (>13 hours)• But, increased emissions in later peak are still seen in

log(T)>7.0 - another, more gradual flare?

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May 5, 2010; C8.8 - FISMMay 5, 2010; C8.8 - FISM

• GOES XRS Peak 11:52 UT; DOY 125• EVE measurements more accurately represent all temperatures

• 10x spectral resolution• Impulsive and gradual phase are temperature dependent.

• FISM at 1nm bins can not account for all temperature ‘blends’ in its bin

• Late-phase in 1-6 MK emissions will not be modeled in FISM

Black: FISM 30.0-39.9 nm

Colors: EVE 0.1 nm bins

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SummarySummary• There are many, interesting questions about flares

that can be addressed with the new EVE data.• ‘2nd’ Peak/Cooling/Multiple Reconnections• Coronal Dimming• Impulsive Phase Enhancements

• Maximum temperature of IP emissions (enhanced density)• Existence/Non-existence of impulsive phase

• AIA will be critical in determining what is happening to cause these variations.• Also SOHO SEM/CDS/SUMER, HINODE XRT/EIS,

RHESSI, LYRA, SOLAR, …..• Models will also help immensely

• EVE measurements will help improve FISM• Spectral resolution, accuracy, temperature dependencies

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May 23-24, 2010; B1.0 - AIAMay 23-24, 2010; B1.0 - AIA


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May 23-24, 2010; B1.0May 23-24, 2010; B1.0

• DOYs 143-144• Small but very long-duration• 1st peak ~coordinated in cooler and hot emissions• Delayed 1st peak and 2nd peak in 5.0<log(T)<6.3• Dimming seen in some emissions ~log(T)=6.3

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May 5, 2010; C8.8 - AIAMay 5, 2010; C8.8 - AIA


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• GOES XRS Peak 11:52 UT; DOY 125• Gradual hot thermal emission decay for log(T)>6.8.• Impulsive phase only log(T) < 5.0• ESP 27-32 nm channel show early impulsive phase,

other EUV channels peak after soft X-ray channel

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• GOES XRS Peak 11:52 UT; DOY 125• Multiple late peaks, cooling or more energy release?• FISM will not be able to show these multiple peaks as

they are not seen in the GOES XRS proxy• May underestimate the 5-45 nm EUV emissions by 70% -

Woods et al., SPD, 2010.

Documents

Flare Observations from SDO EVE