SHINE 2006 WG2/3 - CIRs & Energetic Particles 1 Review of CIR-related Particle Composition, Charge States, & Energy Spectra Joe Mazur The Aerospace Corporation Glenn Mason Johns Hopkins/APL Joe Dwyer Florida Institute of Technology Mihir Desai Southwest Research Institute

SHINE 2006 WG2/3 - CIRs & Energetic Particles 2 After Stone et al., Space Sci Rev., 86, 1, 2000 Processes for 1 AU observations of solar material

SHINE 2006 WG2/3 - CIRs & Energetic Particles 3 Desai et al., JGR, 104, 6705, 1999Mason et al., ApJ Letters, 486, L149, AU 1 AU

SHINE 2006 WG2/3 - CIRs & Energetic Particles 4 Stream interface

SHINE 2006 WG2/3 - CIRs & Energetic Particles 5 Mason et al., ApJ Letters, 486, L149, 1997 see also Richardson et al., JGR 98, 13, 1993 Abundances

SHINE 2006 WG2/3 - CIRs & Energetic Particles 6 Ratios vs. solar wind speed

SHINE 2006 WG2/3 - CIRs & Energetic Particles 7 Abundance summary similar to solar system except for factor of 2-3 enhancement of He and C/O increase of He/O, C/O, and Ne/O with solar wind speed He abundance increases from 1 to 5 AU Mason & von Steiger et al. Space Sci. Rev. 89, 1999 (ISSI CIR Workshop held in 1998)

SHINE 2006 WG2/3 - CIRs & Energetic Particles 8 Ulysses 4.5 AU Gloeckler et al., JGR, 99, 17637, Pick up ion He + increases its contribution to CIRs at greater radial distances Suggested that other pickup ions (such as inner source) at 1 AU might account for some puzzling composition observations

SHINE 2006 WG2/3 - CIRs & Energetic Particles 9 Chotoo et al., JGR, 105, 23107, Acceleration of suprathermal He + in CIRs: enhanced over solar wind

SHINE 2006 WG2/3 - CIRs & Energetic Particles 10 Mobius et al. Geophysical Research Letters, 29, 2001 Mazur et al. ApJ 566, 2002

SHINE 2006 WG2/3 - CIRs & Energetic Particles 11 Mobius et al. Geophysical Research Letters, 29, 2001 SpeciesSAMPEXACE He2.00±0.12- C4.83± ±0.3 O6.12± ±0.35 Ne7.25± ±0.5 Fe13.00± ±0.6 Mazur et al. ApJ 566, 2002 Averaged CIR charge states: ~0.5 MeV/n

SHINE 2006 WG2/3 - CIRs & Energetic Particles 12 Möbius et al., AIP Conf. Proc. 598, 201, 2001

SHINE 2006 WG2/3 - CIRs & Energetic Particles 13 Charge state summary More pickup He at 4.5 AU than 1 AI (at 1 AU the pickup He is ~15% He++, while at 4.5 AU it is twice as abundant) Heavy ions at 1 AU show little evidence of pickup species

SHINE 2006 WG2/3 - CIRs & Energetic Particles 14 Mason et al., ApJ Letters, 486, L149, 1997

SHINE 2006 WG2/3 - CIRs & Energetic Particles 15 Summary Abundances Ion composition similar to solar system but with some differences Still puzzling dependence of some ratios on solar wind speed Charge states Little evidence of Z>2 pickup ions at 1 AU Large abundance of pickup helium at 5 AU Energy spectra Power law from tens of keV/n to ~1 MeV/n Steepening above ~1 MeV/n Spectral forms do not change out to 10’s of AU The source population is coming from the suprathermal region, but that population is not just heated solar wind; other constituents are important Most often the 1 AU particles are not accelerated at shocks requiring another mechanism (Jokipii et al. 2003) As we approach solar minimum we have the opportunity to revisit some of these observables with ACE

SHINE 2006 WG2/3 - CIRs & Energetic Particles 16 Essential new work needed: Complete ACE surveys with much larger number of species identified fully characterize properties of suprathermal / pick-up ion distributions detailed theoretical models to probe injection issues

SHINE 2006 WG2/3 - CIRs & Energetic Particles 17 C. Chotoo, Ph.D. thesis, U of Maryland 1998

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SHINE 2006 WG2/3 - CIRs & Energetic Particles 20 Energy spectra summary power law from tens of keV/n to ~1 MeV/n steepening above ~1 MeV/n spectral forms do not change out to 10’s of AU See also Mason & von Steiger et al. Space Sci. Rev. 89, 1999 (ISSI CIR Workshop held in 1998)

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SHINE 2006 WG2/3 - CIRs & Energetic Particles 22 Energy spectra summary More pickup He at 4.5 AU than 1 AI (at 1 AU the pickup He is ~15% He++, while at 4.5 AU it is twice as abundant) Heavy ions at 1 AU show little evidence of pickup species

SHINE 2006 WG2/3 - CIRs & Energetic Particles 23 Möbius et al., AIP Conf. Proc. 598, 201, 2001

SHINE 2006 WG2/3 - CIRs & Energetic Particles 24 Möbius et al., AIP Conf. Proc. 598, 201, 2001

SHINE 2006 WG2/3 - CIRs & Energetic Particles 25 Richardson et al., JGR, 98, 13, 1993

SHINE 2006 WG2/3 - CIRs & Energetic Particles 26 Dwyer et al, in preparation, 2002

SHINE 2006 WG2/3 - CIRs & Energetic Particles 27 Fisk & Lee acceleration model-- particles in CIRs accelerated by compression at forward and reverse shocks at several AU: propagate in to 1 AU adiabatic deceleration in solar wind included yields distribution function spectra and gradients similar to observations above ~100 keV/n injection energy > 5 keV required, ie from postulated suprathermal tail of the solar wind composition similar to source material (assumed to be solar wind suprathermal tail) -- (note: no systematic measurements of solar wind comp. available at that time) L. A. Fisk and M. A. Lee, Astrophys. J., 237, 620, 1980

SHINE 2006 WG2/3 - CIRs & Energetic Particles 28 Suprathermals as a seed population-- SEP related events –“super events” in the inner solar-system ( Dröge et al ) –Peak intensities in August 1972 (Smart et al. 1990) Interplanetary shocks –Aug 1978 shock (Gosling et al. 1981) –IP shock survey (Tsurutani & Lin 1985) Sources? –long lived remnants of solar flares –planetary bow shocks –corotating interaction regions

SHINE 2006 WG2/3 - CIRs & Energetic Particles 29 Fisk & Lee CIR spectral form-- CIR spectral form: where: v = particle speed; r = radius of observer; rs = shock radius;  = shock strength;  diffusion coefficient  V = solar wind speed

SHINE 2006 WG2/3 - CIRs & Energetic Particles 30 CIR model status 1970s-80s Successful: –spectra above ~100 keV/n –composition “similar” to (unmeasured) solar wind –origin at several AU, and gradients Not successful / unaddressed: –C/O ratio –spectral forms vs. compression ratios –intensities

SHINE 2006 WG2/3 - CIRs & Energetic Particles 31 New CIR energetic particle observations & challenges to standard model-- Particle spectra continue to rise down to ~10 keV/nucleon at 1 AU C/O ratio dependence on solar wind speed Mg/O shows no FIP effect large abundance of He + at 1 and several AU 3 He abundance enhanced compared to solar wind

SHINE 2006 WG2/3 - CIRs & Energetic Particles 32 Butter Garlic Croutons: Enriched unbleached flour (wheat flour, malted barley flour, niacin, reduced iron, thiamine mononitrate, riboflavin, folic acid), partially hydrogenated soybean oil, salt, high fructose corn syrup, corn syrup solids, yeast, salt, contains 2% or less of the following: whey, maltodextrin, wheat gluten, ascorbic acid, dough conditioners (sodium stearoyl lactylate, calcium stearoyl lactylate, calcium peroxide, calcium sulfate, ammonium sulfate, calcium iodate, ascorbic acid), garlic powder, dehydrated parsley, annatto (color), sugar, natural (vegetable and dairy source) and artificial flavors, butter oil, alpha-tocopherol (antioxidant), smoke flavor, enzymes, L-cysteine, TBHQ (to preserve freshness).

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SHINE 2006 WG2/3 - CIRs & Energetic Particles 34 Hilchenbach et al., Trnas. Am.Geophys. U., 78, F554, 1997

SHINE 2006 WG2/3 - CIRs & Energetic Particles 35 Interstellar Gas Flow in Inner Solar System From: University of New Hampshire group WWW page

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SHINE 2006 WG2/3 - CIRs & Energetic Particles 37 Dwyer et al, in preparation, He is enriched in CIRs -- about 4 times the solar wind value compared to 4 He

SHINE 2006 WG2/3 - CIRs & Energetic Particles 38 Role of pick up ions -- consistent with He + abundance tempting explanation for C/O ratio, but –no seasonal variation of heavy ion abundances detected, but data is sparse –at 1 AU C + is a small fraction of CIR carbon

SHINE 2006 WG2/3 - CIRs & Energetic Particles 39 Gloeckler & Geiss, Space Sci. Rev, 86, 127, 1998 CY 1994, = 2.8AU; = -65° =784 km/s

SHINE 2006 WG2/3 - CIRs & Energetic Particles 40 Mazur, Mason & Mewaldt, 2002, ApJ, in press SAMPEX: geomagnetic latitude cutoffs of: (a) 14 CIRs ( ), and (b) all 1998 SEP events

SHINE 2006 WG2/3 - CIRs & Energetic Particles 41 Mazur, Mason & Mewaldt, 2002, ApJ, in press SAMPEX: Calibration of adjusted magnetic invariant latitude cutoffs for CIRs and SEP events

SHINE 2006 WG2/3 - CIRs & Energetic Particles 42 Mazur, Mason & Mewaldt, 2002, ApJ, in press SAMPEX: Observed magnetic cutoffs for CIR events, vs inferred cutoff if ions were singly ionized. Singly stripped ions must be no more than a few percent of total.

SHINE 2006 WG2/3 - CIRs & Energetic Particles 43 CIR abundance details show that bulk solar wind source does not fit the new observations-- Source population is coming from suprathermal region, but that population is not just heated solar wind -- other constituents important Do other shock-associated energetic particle observations show evidence for suprathermal seed ions? YES: SEPs, ESPs -- tracer ion is 3 He

SHINE 2006 WG2/3 - CIRs & Energetic Particles 44 Mason et al., Ap.J. Letters, 525, L133, He and 4 He time intensity profiles in large June 4, 1999 solar particle event

SHINE 2006 WG2/3 - CIRs & Energetic Particles 45 Enhanceed abundances of 3 He in large SEP events ACE/SIS 8-13 MeV/nACE/ULEIS MeV/n Wiedenbeck et al., AIP Conf Proc 528, 107, 2000 Mason et al., Ap.J. Letters, 525, L133, 1999

SHINE 2006 WG2/3 - CIRs & Energetic Particles 46 Suprathermals show times more variation in intensity than solar wind -- likely critical issue in energetic particle intensities

SHINE 2006 WG2/3 - CIRs & Energetic Particles 47 Conclusions: 1 AU CIRs CIR source is not bulk solar wind, but rather the suprathermal region (v/vsw >~ 1.5) time dependent, multiple ingredients: solar wind suprathermal tail pick up ions (interstellar) pick up ions (inner source) other remnants (large SEP events, impulsive SEP events) at < few hundred keV/n, CIR ions are “locally accelerated”

SHINE 2006 WG2/3 - CIRs & Energetic Particles 48 CIRs observed in early 2000 on ACE typical appearance note change in C/O ratio in CIRs vs. solar events

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SHINE 2006 WG2/3 - CIRs & Energetic Particles 51 Introduction Dependence of some abundances on coronal hole speed No reflection of solar wind abundance changes across stream interface - pointing to another source (the suprathermals) / Ubiquitous tails Little influence of Z>2 pickup ions at 1 AU Most 1 AU events don’t have shocks complicated time profile that includes local acceleration and transport of ions from shocks later in the events, as long as a week (Reames)