Review of CIR-related Particle Composition, Charge States, & Energy Spectra

SHINE 2006WG2/3 - CIRs & Energetic Particles

1

Review of CIR-related Particle Composition, Charge States, &

Energy SpectraJoe Mazur

The Aerospace Corporation

Glenn Mason

Johns Hopkins/APL

Joe Dwyer

Florida Institute of Technology

Mihir Desai

Southwest Research Institute


2

After Stone et al., Space Sci Rev., 86, 1, 2000

Processes for 1 AU observationsof solar material

SolarPhotospheric

MaterialFractionation

CoronalMaterial

Solar WindAccelerationMechanism

CoronalMass

Ejections

SolarWind

InterplanetaryShock

Acceleration

Accelerationin CorotatingInt. Regions

Transportto 1 AU

Transportto 1 AU

SolarWind

Interpl.Shock

Particles

C I REvents

GradualSEP

Events

1 keV/nuc 1 MeV/nuc 1 GeV/nuc

SW

ISP

C I R

SEP

ShockAcceleration

by CMEs

ImpulsiveSolar Flare

Acceleration

Transportto 1 AU

ImpulsiveSEP

Events


3

Desai et al., JGR, 104, 6705, 1999

10-6

10-4

10-2

100

102

104

339 340 341 342 343 344 345

Day of 1994

0.06 MeV/nucleon

0.24 0.95

1.93

2.85

5.6

EPACT / WIND

300

400

500

600

700

800

SWE / WIND

Mason et al., ApJ Letters, 486, L149, 1997

5 AU 1 AU


4

0

0.05

0.1

0.15

0.2

0.25

149 150 151 152 153 154 day of 1995

Mg/O ratio

0.1

1

10

100

16O 70 keV/n

Vsw = 666 km/s

Stream interface


5

0.4

0.5

0.6

0.7

0.8

0.9

1

1.1

350 400 450 500 550 600 650 700 750

C/O

Solar wind speed (km/s)

In ecliptic SW

Coronal hole SW

Mason et al., ApJ Letters, 486, L149, 1997see also Richardson et al., JGR 98, 13, 1993

Abundances


6

0

0.05

0.1

0.15

0.2

350 400 450 500 550 600 650 700 750

Fe/O


0

0.05

0.1

0.15

0.2

350 400 450 500 550 600 650 700 750

Si/O


0

0.05

0.1

0.15

0.2

0.25

0.3

350 400 450 500 550 600 650 700 750

Mg/O


0

0.05

0.1

0.15

0.2

0.25

0.3

0.35

0.4

350 400 450 500 550 600 650 700 750

Ne/O


0.4

0.5

0.6

0.7

0.8

0.9

1

1.1

350 400 450 500 550 600 650 700 750

C/O


In ecliptic SW

Coronal hole SW

50

100

150

200

350 400 450 500 550 600 650 700 750

He/O


Coronal hole SW

In ecliptic SW

Ratios vs. solar wind speed


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)


8

Ulysses 4.5 AU

Gloeckler et al., JGR, 99, 17637, 1994.

10-9

10-7

10-5

10-3

10-1

101

103

105

107

109

1 10

F(W) Phase Space Density (s

3

/km6)

W Ion Speed (SC frame)/Vsw

HI-SCALE

SWICS

H+He+

He++

He

1991.292.0400-293.04004.485 AU

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


9

v’/Vsw1 0-4

1 0-2

1 00

1 02

1 04

1 06

1 1 0

H+

He+

He2+

CIR 1, F’

Chotoo et al., JGR, 105, 23107, 2000.

Acceleration of suprathermal He+

in CIRs: enhanced 103 - 104 over solar wind


10

Mobius et al. Geophysical Research Letters, 29, 2001

Mazur et al. ApJ 566, 2002


11

Mobius et al. Geophysical Research Letters, 29, 2001

Species SAMPEX ACE

He 2.00±0.12 -

C 4.83±0.27 5.1±0.3

O 6.12±0.37 6.1±0.35

Ne 7.25±0.25 7.8±0.5

Fe 13.00±0.48 10.5±0.6

Mazur et al. ApJ 566, 2002

Averaged CIR charge states: ~0.5 MeV/n


12

Möbius et al., AIP Conf. Proc. 598, 201, 2001


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


14

10-7

10-5

10-3

10-1

101

103

0.01 0.1 1 10

WIND/ STEP & LEMT - SAMPEX / LICA12/6/94 18:00 - 12/7/94 18:00

MeV/nucleon

H

HeCNO

Fe

Mason et al., ApJ Letters, 486, L149, 1997


15

SummaryAbundances

Ion composition similar to solar system but with some differencesStill puzzling dependence of some ratios on solar wind speed

Charge statesLittle evidence of Z>2 pickup ions at 1 AULarge abundance of pickup helium at 5 AU

Energy spectraPower law from tens of keV/n to ~1 MeV/nSteepening above ~1 MeV/nSpectral 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


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


17

10-7

10-5

10-3

10-1

101

103

105

107

1 10

MASS, STICS, and STEPCIR 2: May 30, 1995 10:00-22:30 UT

Helium Spectra

V/Vsw (SC Frame)

MASS

STICS

STEP

C. Chotoo, Ph.D. thesis, U of Maryland 1998


18

10 -39

10 -37

10 -35

10 -33

10 -31

10 -29

10 -27

10 -25

0.001 0.01 0.1 1 10 100

Fisk & Lee 1 AU spectral form vs. distance to shock

1 AU1.5 AU2 AU3 AU4 AU5 AU6 AU

Energy/n

Shock location:


19

10-5

10-4

10-3

10-2

10-1

100

101

102

103

0.01 0.1 1 10

WIND/STEP Spectra5/30/95 9:39:04 to 5/31/95 14:19:28

MeV/nucleon

STEP C+N+O Flux

Fisk & Lee (1980) Spectral Form(numerical solution)


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)


21

Solar WindAccelerationMechanism

CoronalMass

Ejections

3He-rich Solar Flare

Accelelration

Slow SolarWind

TransientShock

Acceleration

CorotatingInt. Regions

Transportto 1 AU

Transportto 1 AU

SolarWind

ESPEvents

C I REvents

SolarPhotospheric

Material

Fractionation

CoronalMaterial

Fast SolarWind

InterstellarPick up

Ions

InnerSource(dust?)

Q = 1pick up

ions

Transportto 1 AU

3He-richSEP

Events

InterplanetarySuprathermal Ions

Transportto 1 AU

C M EAssocSEPs


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


23Möbius et al., AIP Conf. Proc. 598, 201, 2001


24Möbius et al., AIP Conf. Proc. 598, 201, 2001


25Richardson et al., JGR, 98, 13, 1993


26

C N Ne Mg Si S Fe0.01

0.10

1.00shock

CIR

solar wind

Dwyer et al, in preparation, 2002


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


28

Suprathermals as a seed population--

• SEP related events– “super events” in the inner solar-system (Dröge et al. 1992.)– 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


29

Fisk & Lee CIR spectral form--

CIR spectral form:

where: v = particle speed; r = radius of observer; rs = shock radius;

= shock strength; diffusion coefficientV = solar wind speed

f =

r

rs

⎛

⎝

⎜⎞

⎠

⎟

2 / ( 1 − ) + V / ( o

v )

v− 3 / ( 1 − )

exp −

6 o

v

V ( 1 − )2

⎛

⎝

⎜⎞

⎠


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


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• 3He abundance enhanced compared to solar wind


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).


33

0.05

0.1

0.15

pre-FS FS to SI SI to RS post-RS

Solar Wind Mg/O Abundance Variations in CIRsSWICS/ Ulysses: 15 CIRs (4.5 - 5.4 AU)

Mg/O

from: Wimmer-Schweingruber et al., JGR vol 102, 17407,1997


34Hilchenbach et al., Trnas. Am.Geophys. U., 78, F554, 1997


35

Interstellar Gas Flow in Inner Solar System

From: University of New Hampshire group WWW pagehttp://www-ssg.sr.unh.edu/tof/Missions/Ace/aceset.html


36

0.01

0.1

1

10

100

103

1 3 5 7 9 11 13

Seasonal Variation of CIR abundances(filled circles = STEP; open circles = LICA)He/O

C/ONe/O4He/OC/ONe/O

Month of Year


37

2 3 4 5 6mass (nucleons)

0

100

200

300

3He/4He =0.0016 ± 0.0002

ACE/ULEIS 0.4-1.0 MeV/nsum of 6 CIRs

Dwyer et al, in preparation, 2002

3He is enriched in CIRs -- about 4 times the solar wind value compared to 4He


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


39Gloeckler & Geiss, Space Sci. Rev, 86, 127, 1998CY 1994, <r> = 2.8AU; <latitude> = -65°<vsw>=784 km/s


40

10

-1

10

0

relative flux

(a) CIR

He

O

Fe

10

-1

10

0

60 62 64 66 68 70

relative flux

adjusted invariant latitude

(b) SEP

HeO

Fe

Mazur, Mason & Mewaldt, 2002, ApJ, in press

SAMPEX:

geomagnetic latitude cutoffs of:

(a) 14 CIRs (1992- 95), and

(b) all 1998 SEP events


41

10

1

10

2

10

3

62 63 64 65 66 67

Rigidity (MV)


He

C

O

Ne

Fe

Fe

Ne

O

C

He SEP

CIR


SAMPEX:

Calibration of adjusted magnetic invariant latitude cutoffs for CIRs and SEP events


42

10

-3

10

-2

10

-1

10

0

carbon

C

+1

10

-3

10

-2

10

-1

10

0

oxygen

O

+1

flux (#/cm

2

-sec-sr-MeV/n)

10

-3

10

-2

10

-1

10

0

55 60 65 70 75


neon

Ne

+1


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.


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 3He


44

10

-4

10

-3

10

-2

10

-1

10

0

10

1

10

2

155 156 157 158 159 160

ACE / ULEIS 0.7 MeV/nucleon

Day of 1999

4

He

3

He

2B N17W69

Mason et al., Ap.J. Letters, 525, L133, 1999

3He and 4He time intensity profiles in large June 4, 1999 solar particle event


45

Enhanceed abundances of 3He in large SEP events

ACE/SIS 8-13 MeV/n

0

2,000

4,000

6,000

8,000

10,000

12,000

14,000

0

20

40

60

80

100

120

140

2 3 4 5 6

Mass (AMU)

(a)

"finite" 3He

ACE/ULEIS 0.5-2 MeV/n

Wiedenbeck et al., AIP Conf Proc 528, 107, 2000Mason et al., Ap.J. Letters, 525, L133, 1999


46

Suprathermals show 10-100 times more variation in intensity than solar wind -- likely critical issue in energetic particle intensities

0.01

0.1

1

10

100

1000

50 70 90 110 130 150

WIND / EPACT / STEP30 keV/n Fe

Day of 2000

104

105

106

107

108

109

50 70 90 110 130 150

WIND / SWENp * Vsw ^2

Day of 2000


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”


48

200

300

400

500

600

700

800

900

1000

10 20 30 40 50 60

ACE / SWEPAM solar wind speed

SWEPAM Vsw

Day of 2000

0.001

0.01

0.1

1

10

10 20 30 40 50 60

ACE / ULEIS 270 keV/nucleon

C12 0.2731 MeV/nuc O16 0.2731 MeV/nuc

Day of 2000

27 daysCIRCIR CIRSEP

CIRs observed in early 2000 on ACE

•typical appearance

•note change in C/O ratio in CIRs vs. solar events


49

10

100

1000

10 4

10 20 30 40 50 60

ACE / ULEIS E> 200 keV/nCIR and SEP mass histograms

tof_mass -- cir tof_mass -- SEP renormalized

Mass (AMU)

2/6/2002


50

100

1000

10 4

10 15 20 25 30

ACE / ULEIS E> 200 keV/nCIR and SEP mass histograms

tof_mass -- cir tof_mass -- SEP renormalized

Mass (AMU)

2/6/2002


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)

Review of CIR-related Particle Composition, Charge States, & Energy Spectra

Documents

Transcript of Review of CIR-related Particle Composition, Charge States, & Energy Spectra