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TSI and VUV Radiative Energies During X-Class Solar Flares

TSI and VUV Radiative Energies During X-Class Solar Flares . Chris Moore Undergraduate Student U. of Iowa (2 summers at LASP/U. Of Colorado) Phillip Chamberlin, Rachel Hock, Greg Kopp LASP/U. of Colorado. Research Objectives.

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TSI and VUV Radiative Energies During X-Class Solar Flares

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  1. TSI and VUV Radiative Energies During X-Class Solar Flares Chris Moore Undergraduate Student U. of Iowa (2 summers at LASP/U. Of Colorado) Phillip Chamberlin, Rachel Hock, Greg Kopp LASP/U. of Colorado Moore - Onset of SC 24

  2. Research Objectives • Analyzing the energy contribution of solar flares, in the VUV, soft/hard X-rays and the microwave wavelengths. • Finding the energy composition from the impulsive and gradual phase of each spectral region • Search for a center to limb variation

  3. Impulsive and Gradual phases Neupert effect (1968) + + =

  4. The Flare Irradiance Spectral Model (FISM) • FISM is an empirical model of the solar vacuum ultraviolet (VUV; 0.1-190 nm) irradiance at 60 second temporal resolution. • Phil Chamberlin developed for his Ph.D. Dissertation (U. of Colorado, 2005) • Current version released June 2008 • Updated for SEE V9 data • Uses traditional proxies (MgII c/w, F10.7, and Ly) as well as new proxies (0-4 nm, 36.5 nm, and 30.5 nm) to model the daily component - provide more accurate CLV. • Uses the GOES 0.1-0.8 nm irradiance as the proxy to model flare variations. • FISM is the first flare model that can be used for near real-time space weather operations. Moore - Onset of SC 24

  5. Solar Variation on Various Time Scales Transition region emissions increased by up to a factor of 10 during the impulsive phase EUV irradiance increased by a factor of 2 and XUV increases by a factor of 100 during the gradual phase Flare Variations were as large or larger than the solar cycle variations for the Oct 28, 2003 flare Moore - Onset of SC 24

  6. TSI Flare Budget - Revisited • Reanalysis of TSI and VUV spectral contributions from Woods, Kopp,  and Chamberlin, JGR, 2006 • Updated using V9 TIMED SEE data • Lower contributions from 0.1-27 nm (/10) • Revised spectral distribution • Better TSI fitting algorithm • Addition of RHESSI Contribution • Have run analysis for 21 April 2002 and 23 July 2002 events (Emslie, Dennis, Holman, and Hudson, JGR, 2005) • Using TSI “Model” –NOTE: Very limited: based on 5 flares Moore - Onset of SC 24

  7. TIM/TSI scaling • Accuracy of 100 ppm (.01%)

  8. October 28, 2003 - X17 - (E08, S16) November 4, 2003 - X28 - (W83, S19) TSI Flare Budget - Revisited Numbers from WKC Also have data for 10/29/03, 11/2/03*, 1/15/05*, 1/19/05*, 1/20/05*, 9/7/05, 12/5/06*, 12/6/06, 12/13/06* * - Modeled TSI (can do for any flare, but these selected because of good RHESSI data) Moore - Onset of SC 24

  9. Impulsive Phases Oct. 28, 2003 (X17) 1.56 x 10^31 ergs Oct. 29, 2003 (X10) 8.54 x 10^30 ergs Nov. 4, 2003 (X28) 5.7 x 10^30 ergs Sep. 7, 2005 (X17) 2.18 x 10^30 ergs Dec. 6, 2006 (X6.5) 8.83 x 10^30 ergs Gradual Phases Oct. 28, 2003 (X17) 3.46 x 10^32 ergs Oct. 29, 2003 (X10) 1.28 x 10^32 ergs Nov. 4, 2003 (X28) 1.36 x 10^32 ergs Sep. 7, 2005 (X17) 1.48 x 10^32 ergs Dec. 6, 2006 (X6.5) 3.75 x 10^31 ergs TSI results

  10. TSI Flare Budget - Modeled • Emslie, Dennis, Holman, and Hudson, JGR, 2005 • Modeled the total ‘final’ radiant energy of two limb flares from GOES temperature and emission measure • 21 April 2002: 3 x 1031 +/- 0.3 x 1031 • 23 July 2002: 1 x 1031 +/- 0.3 x 1031 • New TSI Model • Use the FISM energy and location on disk to estimate TSI energy released in flare • 21 April 2002: 3.4 x 1031 • 23 July 2002: 3.3 x 1031 Moore - Onset of SC 24

  11. TSI model • Based on VUV, TSI can be modeled to show energy release that would have been seen during TSI eclipse periods or before TIM operation • N = # of center/limb flares seen in TSI (Take limb flares to be greater than 70º east or west) • TI = impulsive phase energy in TSI • TG = gradual phase energy in TSI • VI = impulsive phase energy in VUV • VG = gradual phase energy in VUV • FI = VI/TI = fraction of impulsive phase energy from VUV compared to TSI • FG = VG/TG = fraction of gradual phase energy from VUV compared to TSI • a = (1\N) * [∑ (from N to i =1) (FI(i))] = average fraction of impulsive phase energy from VUV • b = (1\N) * [∑ (from N to i =1) (FG(i))] = average fraction of gradual phase energy from VUV • A = 1/a = factor that can be multiplied by the observed impulsive phase VUV wavelengths to obtain an estimated value for the TSI • B = 1/b = factor that can be multiplied by the observed gradual phase VUV wavelengths to obtain an estimated value for the TSI

  12. TSI Flares Flares (GOES Classification) (Location) 28-Oct-2003 (X17) (E08 S16) 4-Nov-2003 (X28) (W83 S19) Spectral Region Imp. Phase Grad. Phase Imp. Phase Grad. Phase TSI 1.56 x10^31 3.46 x 10^32 5.7 x 10^30 1.36 x 10^32 VUV [0.1-190 nm] (% of TSI) 7.17 x 10^30 (46%) 1.1 x 10^ 32 (34%) 2.35 x 10^30 (41%) 5.17 x 10^31 (38%) 29-Oct-2003 (X10) (W10 S17) 7-Sep-2005 (X17) (E77 S11) Imp. Phase Grad. Phase Spectral Region Imp. Phase Grad. Phase 2.18 x 10^30 1.48 x 10^32 TSI 8.54 x 10^30 1.28 x 10^32 8.42 x 10^30 (386%) 1.07 x 10^32 ergs (72%) VUV [0.1-190 nm] (% of TSI) 5.17 x 10^30 (61%) 4.35 x 10^31 (34%) 6-Dec-2006 (X6.5) Spectral Region Imp. Phase Grad. Phase TSI 8.83 x 10^30 3.75 x 10^31 VUV [0.1-190 nm] (% of TSI) 2.06 x 10^30 (23%) 1.83 x 10^31 (49%)

  13. Modeled Flares Flares (GOES Classification) (Location) 15-Jan-2005 (X1.2) (E14 N8) 19-Jan-2005 (X1.3) (W5 N15) Spectral Region Imp. Phase Grad. Phase Imp. Phase Grad. Phase TSI *2.24 x 10^30* *2.33 x 10^31* *2.42 x 10^30* *4.94 x 10^31* VUV [0.1-190 nm] 9.7 x 10^29 9.1 x 10^30 1.05 x 10^30 1.93 x 10^31 20-Jan-2005 (X1.3) (W61 N14) 2-Nov-2003 (X8.3) (E56 N14) Spectral Region Imp. Phase Grad. Phase Imp. Phase Grad. Phase TSI *9.05 x 10^30* *1.61 x 10^32* *9.70 x 10^30* *9.82 x 10^ 31* VUV [0.1-190 nm] 3.92 x 10^30 6.3 x 10^31 4.2 x 10^30 3.83 x 10^31 5-Dec-2006 (X9) (E79 S07) 13-Dec-2006 (X3) (W23 S05) Imp. Phase Grad. Phase Spectral Region Imp. Phase Grad. Phase *1.45 x 10^31* *8.23 x 10^31* TSI *7.38 x 10^29* *2.67 x 10^31* 6.3 x 10^30 3.21 x 10^31 VUV [0.1-190 nm] 1.51 x 10^30 1.47 x 10^31 21-Apr-2002 (X1.5) (W84 S14) 23-Jul-2002 (X4.8) (E72 S13) Spectral Region Imp. Phase Grad. Phase Imp. Phase Grad. Phase TSI *5.07 x 10^29* *3.4 x 10^31* *9.26 x 10^29* *1.81 x 10^31* VUV [0.1-190 nm] 1.04 x 10^30 1.87 x 10^31 1.89 x 10^30 1.81 x 10^31

  14. Future Work • Search for additional spectral contributions to the impulsive and gradual phase to the TSI • RHESSI • White Light, through TRACE 1600 angstrom and WL bands • SPM 9 (VIRGO-SOHO) • Microwave wavelengths

  15. Conclusion • Valid estimates of the TSI radiated energy from flares • Very dependent on background subtraction • Able to estimate TSI energies of all other flares when not observed by TIM with model • Model scales VUV values and incorporates CLV using flare location • Model only based on 5 flares - very limited statistics • Looking forward to results for new solar cycle • Continuing measurements from SORCE TIM • New TSI flare measurements from GLORY TIM (launch July 2009) • New VUV flare measurements from SDO EVE (launch Mid-2009 to early  2010)

  16. Back Up Slides

  17. X17 Flare Comparison to SEE 139.5 nm Si IV; Log(T)=4.85 Moore - Onset of SC 24

  18. TSI Flare Observations From Woods, Kopp, and Chamberlin (WKC), JGR, 2006 Moore - Onset of SC 24

  19. EUV Variability Experiment (EVE) • University of Colorado / LASP • Thomas N. Woods (PI) • Francis G. Eparvier • Gary J. Rottman • Phillip C. Chamberlin • University of Southern California • Darrell L. Judge, Donald R. McMullin • Naval Research Laboratory • Judith L. Lean • John T. Mariska • Harry P. Warren • MIT Lincoln Laboratory • Gregory D. Berthiaume • University of Alaska •Scott M. Bailey • NOAA• Rodney A. Viereck • Space Environment Technologies • W. Kent Tobiska • CU/CIRES/NOAA •Timothy J. Fuller-Rowell • Utah State University •Jan J. Sojka Launch in mid-2009 onboard the Solar Dynamics Observatory (SDO) http://lasp.colorado.edu/eve/ Moore - Onset of SC 24

  20. Dl 0.1 1 4 7 10 nm How does EVE measure the EUV? • Multiple EUV Grating Spectrograph (MEGS) • At 0.1 nm resolution • MEGS-A: 5-37 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 • 0-7 nm (zeroth order) • In-flight calibrations from ESP and MEGS-P on daily basis and also annual calibration rocket flights Moore - Onset of SC 24

  21. How will EVE help VUV Flare Studies? • 10 sec (0.25 sec for ESP) temporal resolution, 100% duty cycle • EVE will measure all flares with very good temporal resolution and concurrent spectral information. • Only 11 impulsive phase observations and 29 gradual phase observations at one point during the flare from TIMED SEE. • Extend the solar XUV and EUV irradiance measurement set with better accuracy. • Higher spectral resolution, especially for  < 27nm • EVE is 0.1 nm spectral resolution from 5-105 nm, 1.0 nm from 0.1-5 nm. • EVE will help determine the relationship between EUV and XUV flares. • Help refine timing of the Neupert Effect? Moore - Onset of SC 24

  22. CME’s Release energy up to 40 billion Hiroshima sized atomic bombs NOAA SWPC Particle events Auroras Geomagnetic storms Power grids Airlines (rerouting for polar flights) Disruptions GPS Radio blackouts Solar flares effect on Earth

  23. A magnetic flux tube emerges above the solar surface in active regions Magnetic flux tube is more buoyant than the surrounding plasma Eventually a filament of plasma is released after the stretching of the magnetic field lines reached their eruptive limit This gives rise to the two phases of the solar flare Dynamics of Solar Flares

  24. Dynamics of Solar Flares 2 • Energy is forced back into the atmosphere by magnetic reconnection, this is the energy input (Impulsive phase) • It is not visible until the Transition region, the corona is not dense enough • This influx of energy creates thermal heating in the atmosphere, seen in all regions • This is the slow phase (Gradual phase) of the solar flare

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