1 SEP “Campaign Events” for SHINE 2003 Question: Can we identify solar/interplanetary factors that drive SEP spectral and compositional variability at.

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Presentation transcript:

1 SEP “Campaign Events” for SHINE 2003 Question: Can we identify solar/interplanetary factors that drive SEP spectral and compositional variability at high energies? Two possible events for addressing this question: 21 April 2002 and 24 August 2002 Ostensibly very similar flare/CME characteristics -- Ostensibly very similar flare/CME characteristics -- But very different SEP composition & spectra at high energies. A.J. Tylka, NRL (the largest SEP event of 2002) (the only ground- level event of 2002)

2 Compare SEP Fe/C vs. Energy Data from ACE/EPAM, Wind/LEMT, ACE/SIS Fe/C nearly identical at ~ MeV/nuc But the two events diverge dramatically at higher energies -- Fe/C differ by a factor of ~100 at 50 MeV/nuc. The origin of this behavior is perhaps the biggest puzzle to have emerged from Cycle 23 SEP observations.

3 Compare Solar Activity & Interplanetary Conditions 21 Apr Aug 2002 CME Characteristics (S. Yashiro) Speed (km/s) Speed (km/s) Width (deg) Width (deg) Position Angle (deg) Position Angle (deg)260Halo Flare Characteristics (NOAA/SGD) Size Size X1.5 / 1F X3.1 / 1F Location LocationS14W84S02W81 Duration: Start to Maximum/e (min) Duration: Start to Maximum/e (min)11542 SW Speed at 1 AU (km/s), averaged over the first 6 hours (CDAWeb) ~475~385 Associated Shock (C.W. Smith) Transit Time to 1 AU (hours) Transit Time to 1 AU (hours)5158 Velocity Jump (km/s) Velocity Jump (km/s)~200~100

4 What might we learn from these two events? These two SEP events show significant differences in terms of: Elemental Composition (esp. Fe/C above ~10 MeV/nuc)Elemental Composition (esp. Fe/C above ~10 MeV/nuc) Spectral ShapeSpectral Shape SizeSize Temporal StructureTemporal Structure However, the CMEs, flares, and interplanetary conditions associated with these two events are remarkably similar. Thus, these two events provide an opportunity to examine the origins of SEP variability under nearly “controlled conditions”. Comparisons between these events can help us isolate and model the drivers of SEP variability.

5 Advantages/Disadvantages as Campaign Events Advantages: 1.Overall, both events are well measured. 2.Lots of interest already in 21 April This study will educate the SHINE community on “our SEP puzzles”. 4.Lots of other events show characteristics similar to these two events – plenty of data for testing new hypotheses. 5.A tremendous success, if we can figure this out. Disadvantages: 1.We might not figure it out. 2.Unfortunate datagaps in RHESSI (esp. 24 August). 3.These are weak shocks by the time they get to 1 AU. (That is, they are no longer accelerating ions beyond ~0.5 MeV/nuc or less.)

6 Additional Comparisons FYI: The following pages offer comparisons of: GOES Proton Timelines Ion Timelines, Spectra, & Composition from Wind & ACE LASCO CME Measurements GOES X-Ray Timelines RHESSI Observations Wind/Waves Radio Emission Solar Wind Parameters, as reported by Wind GOES Protons – preceding 6 days GOES X-Rays – preceding 6 days Wind Waves Radio Emission – preceding 3 days CME Interactions – a la Gopalswamy et al. Time-Dependent Spectra & Composition (Maybe you’ll spot the answers here!!)

7 GOES Protons >10 MeV, >50 MeV, >100 MeV 21 April August 2002 >10 MeV profiles very similar, except for normalization. But >50, >100 MeV profiles have different shapes in the two events. No increase in high-energy particles at the time of shock arrival at the Earth (arrows). Thus, in both events, the high-energy particles are produced predominantly while the shock is still far from 1 AU. But the apparent duration of >50 MeV proton production is longer in the April event. Why? And how does this relate to the differences in ionic composition & spectra ? (See below.)

8 Ion Timelines (from Wind & ACE) 21 April 2002 Timelines are similar, except for Larger intensities in the April eventLarger intensities in the April event Higher Fe/O ratio at ACE/SIS energies in the August event. (Compare bottom two traces in the two plots.)Higher Fe/O ratio at ACE/SIS energies in the August event. (Compare bottom two traces in the two plots.) 24 August 2002

9 Ion Spectral Shapes (event-integrated) Spectra have more pronounced “exponential rollovers” in the April event. Spectra closer to power-laws (especially Fe) in the August event. Data from ACE/EPAM, Wind/LEMT, ACE/SIS IronOxygen

10 Elemental Composition (event-integrated) ACE/EPAM ~1 MeV/nuc Wind/LEMT ~5 MeV/nuc ACE/SIS ~30 MeV/nuc X/C, normalized to corona, for He - Fe

11 LASCO CMEs -- 1 parameter fits 21 April August 2002 *from Seijo Yashiro.

12 LASCO CMEs -- 2 parameter fits 21 April August 2002 *from Seijo Yashiro.

13 GOES X-rays 21 April August 2002 X1.5 at S14W84, 115-minutes duration* X3.1 at S02W81, 42-minutes duration* *As defined by GOES: from start until maximum has decreased by 1/e.

14 RHESSI Observations 24 August 2002 Provided by Säm Krucker 21 April 2002

15 Wind/Waves Radio Emissions From 21 April August 2002

16 Solar Wind Parameters from Wind Provided by K. Olgilvie, via NSSDC’s CDAWeb April August 2002

17 GOES Protons – Previous 6 Days April August 2002

18 GOES X-Rays – Previous 6 Days April August 2002

19 Wind/Waves Radio – Previous 3 Days August April 2002 From

20 CME Interactions 21 April August 2002 Provided by Seiji Yashiro & Nat Gopalswamy

21 Time-Dependent Spectra & Composition Event-Integrated spectra & composition can provide only a first hint.Event-Integrated spectra & composition can provide only a first hint. Time-dependent spectra & composition needed for detailed modeling.Time-dependent spectra & composition needed for detailed modeling. Data below provided by:Data below provided by: –ACE/SIS (from the ACE Science Center, courtesy of the SIS team) –Wind/LEMT (from Don Reames) –ACE/EPAM (from Carol Maclennan, on behalf of the EPAM team) –Plots will be updated as additional data become available.

22 Time-Dependent O & Fe Spectra (Hours 0.0 – 3.0) 21 April August 2002 Pre-Event Bgrd Hours 0.0 – 1.0 Hours 1.0 – 2.0 Hours 2.0 – 3.0

23 Time-Dependent O & Fe Spectra (Hours 3.0 – 8.0) 21 April August 2002 Hours 3.0 – 4.0 Hours 4.0 – 5.0 Hours 5.0 – 6.0 Hours 6.0 – 8.0

24 Time-Dependent O & Fe Spectra (Hours 8.0 – 18.0) 21 April August 2002 Hours 8.0 – 10.0 Hours 10.0 –12.0 Hours Hours

25 Time-Dependent O & Fe Spectra (Hours ) 21 April August 2002 Hours 18.0 – 22.0 Hours 22.0 – 30.0 Hours Hours

26 Time-Dependent O & Fe Spectra (Hours 46.0 – 90.0) 21 April August 2002 Hours Hours Hours Hours 78.0 – 90.0

27 Time-Dependent C/O, Ne/O, Fe/O (Hours 0.0 – 3.0) 21 April August 2002 Pre-Event Bgrd Hours 0.0 – 1.0 Hours 1.0 – 2.0 Hours 2.0 – 3.0

28 Time-Dependent C/O, Ne/O, Fe/O (Hours 3.0 – 8.0) 21 April August 2002 Hours 3.0 – 4.0 Hours 4.0 – 5.0 Hours 5.0 – 6.0 Hours 6.0 – 8.0

29 Time-Dependent C/O, Ne/O, Fe/O (Hours 8.0 – 18.0) 21 April August 2002 Hours 8.0 – 10.0 Hours 10.0 –12.0 Hours Hours

30 Time-Dependent C/O, Ne/O, Fe/O (Hours ) 21 April August 2002 Hours 18.0 – 22.0 Hours 22.0 – 30.0 Hours Hours

31 Time-Dependent C/O, Ne/O, Fe/O (Hours 46.0 – 90.0) 21 April August 2002 Hours Hours Hours Hours 78.0 – 90.0

32 Time & Energy Dependent Fe/O 21 April August 2002 Wind/LEMT ~3-10 MeV/nuc ~3-10 MeV/nuc ACE/SIS ~10-80 MeV/nuc

33 Time & Energy Dependent Si/O Wind/LEMT ~3-10 MeV/nuc ~3-10 MeV/nuc ACE/SIS ~10-80 MeV/nuc 21 April August 2002

34 Time & Energy Dependent Ne/O Wind/LEMT ~3-10 MeV/nuc ~3-10 MeV/nuc ACE/SIS ~10-80 MeV/nuc 21 April August 2002

35 Time & Energy Dependent C/O Wind/LEMT ~3-10 MeV/nuc ~3-10 MeV/nuc ACE/SIS ~10-80 MeV/nuc 24 August April 2002