SHINE 2004 Session 4 1

New Radiation Belts and Other Effects of Cycle 23 SEP Events

J. E. Mazur, J. B. Blake, P. L. Slocum

The Aerospace Corporation

M. K. Hudson

Dartmouth College

G. M. Mason

University of Maryland

This work was supported in part under The Aerospace Corporation's Mission Oriented Investigation and Experimentation program, funded by the U.S. Air Force Space and Missile Systems Center under Contract No. FA8802-

04-C-0001, and under contract Z667103 between the University of Maryland and The Aerospace Corporation.

SHINE 2004 Session 4 2

Outline• Brief review of observational facts of

new radiation belts that form in the inner magnetosphere during intense SEP events and CME-related shocks

• Late 2003 events and SHINE campaign events

SHINE 2004 Session 4 3

Charged particle motion

SHINE 2004 Session 4 4

Cartoons of the inner

magnetosphere

Reality as viewed with a

15-month average

SHINE 2004 Session 4 5

The inner magnetosphere is host to a variety of time-dependent trapped populations and is not static.

SHINE 2004 Session 4 6

Observations of large changes near L=2: 1960

• Explorer 7:1959-1960• GM tube: >18 MeV protons,

>1.1 MeV electrons• Pizzella, McIwain, & Van

Allen JGR 1961

SHINE 2004 Session 4 7

Other glimpses of new belts

Radiation belt duration from Lorentzen et al. JGR 107(A9), 1231, doi:10.1029/2001JA000276, 2002

0

50

100

150

200

250

300

350

400

1953 1963 1973 1983 1993 2003

Sunspotnumber

cycle 22 cycle 23

Timing & approximate lifetimes of new proton belts L~2 to 3

ftp://ftp.ngdc.noaa.gov/STP/SOLAR_DATA/SUNSPOT_NUMBERS/MONTHLY

?

continuous monitoringof inner magnetosphere

SHINE 2004 Session 4 8

There were discontinuous changes to the outer edge of the inner proton belt in 2000 & 2001.

SHINE 2004 Session 4 9

24 March 1991

Creation of >15 MeV electron and >50 MeV proton belts

- A lone spacecraft at the right place at the right time -

SHINE 2004 Session 4 10

-300

-250

-200

-150

-100

-50

0

50

100

DST

SHINE 2004 Session 4 11

24 March 1991 shock injection as seen by CRRES

The new belts lasted more than 2 years.

SHINE 2004 Session 4 12

Summary of24 March 1991 event

• Particle injection immediate – Injected particles strongly peaked in pitch angle – Successfully modeled by Li et al. GRL 20, 2423-2426, 1993– Radial transport of outer zone electrons (energy gain L-1.5)

& SEP protons (energy gain L-3)

• Both protons and electrons clearly visible in new belt– Very high electron energies for Earth’s magnetosphere

• Long lifetime: >2 years

SHINE 2004 Session 4 13

Search for new belts in cycle 23

• Potential ambiguity: protons and electrons are present throughout the magnetosphere– Is the presence of a new belt a result of a

redistribution of previously trapped particles or due to some other process?

• Use SAMPEX ion composition to search for heavy ions below L=4– Z>2 ions rare in the magnetosphere above 1

MeV/n (except for trapped ACR)– Long monitor of inner magnetosphere with well-

calibrated instruments

SHINE 2004 Session 4 14

SAMPEX mission history

SHINE 2004 Session 4 15

New belt example: 24 Nov 2001

Clear trapping of solar particles - no other source of heavy ions possible

SHINE 2004 Session 4 16

Species-dependent injection?

2

2.5

3

3.5

4

11/1/2001 12/1/2001 1/1/2002

trappedprecipitating

L shell

SEP events

1

10

100

1 10 100mass

H SFe

O

trapped ionstrapped ions

1

10

100

1 10 100mass

HHe O

MgFe

trapped ions

SAMPEX

Variable composition

that does not match

solar particles

SHINE 2004 Session 4 17

Lifetimes of new belts

• 24 Nov 2001 case• Decay rate was faster

for increasing Z• Expected trend if

energy loss in residual atmosphere was the dominant loss process

SHINE 2004 Session 4 18

New belts & SEP intensity

• What is required for creation of a new ion belt?

• SEP access to L<4 during main phase of geomagnetic storm

• Sufficient intensity of SEPs

SHINE 2004 Session 4 19

Statistics of new ion belts

• 39 SEP incursions below L=4 in 10 years

• All occurred during geomagnetic storms

• 13 of these incursions resulted in detectable new ion belts (33%)

• Creation depends upon SEP intensity and magnitude of storm

• DST related to SEP access, but high-latitude currents may also be important

SHINE 2004 Session 4 20

Statistics of new ion belts

• Locations of new belts ordered by particle Z even for differences in mean L-shells as small as 0.2 L

• Indicates rigidity-dependent access and trapping

SHINE 2004 Session 4 21

October-November 2003

SHINE 2004 Session 4 22

Protons > 15 MeV

No injection of high-energy protons

SHINE 2004 Session 4 23

Electrons >3 MeV

Multi-MeV electrons at L~2.5

SHINE 2004 Session 4 24

New heavy-ion belt that lasted ~20 days

SHINE 2004 Session 4 25

Highest intensity of trapped ~0.5 MeV particles at L=2 in 11.5 years

SHINE 2004 Session 4 26

SHINE campaign events

SHINE 2004 Session 4 27

SHINE campaign events: no new ion belts

SHINE 2004 Session 4 28

Recent History of the Radiation Belts

• SAMPEX daily averaged data mapped to a dipole

• >0.5 MeV electrons• >0.7 MeV protons• 1998 to 2004

QuickTime™ and aYUV420 codec decompressor

are needed to see this picture.

SHINE 2004 Session 4 29

Summary• Inner magnetosphere is a dynamic place

and a reservoir of interplanetary and interstellar material

• Previous best example of SEP-related new belts: March 1991

• This survey used heavy-ions as tracers of solar particle material that becomes trapped in the inner magnetosphere during intense SEP events with geomagnetic storms– One-third of the SEP incursions below L=4

resulted in new belts– Belt creation dependent on SEP intensity

and size of storm– Not clear what determines belt location

• Heavy-ion belt decay consistent with energy loss

SHINE 2004 Session 4 30

The way ahead

• Modeling of shock events– what solar wind characteristics lead to the fast risetime in ground-

based magnetometer observations of storm commencements?– what is the temporal cadence of solar wind measurements needed

for modeling ssc risetimes of a minute or less?

• High-duty cycle measurements in the slot region: – ion composition sensors– electron sensors with good energy resolution and dynamic range to

more than 10 MeV– comprehensive field investigations

SHINE 2004 Session 4 31

Backup charts

SHINE 2004 Session 4 32

SAMPEX

SHINE 2004 Session 4 33

SAMPEX

SHINE 2004 Session 4 34

31 October 2003

• No energetic protons injected

• Multi-MeV electrons appear at L = 2.5– direct shock association unclear

• 10-20 MeV electrons among solar population– First time seen by SAMPEX (launch July 1992)

SHINE 2004 Session 4 35

210 Magnetometer Chain

• Timing of the SSCs associated with energetic particle injection events determined using the 210 Magnetometer chain.

• Allows comparisons of the state of the Earth’s magnetic field at high time resolution.

SHINE 2004 Session 4 36

-100

0

100

200

300

-500 0 500 1000 1500

031031011106000714980504910324000406980826011124

H

Time after ssc onset, sec

210 Magnetometer Chain

SHINE 2004 Session 4 37

Upsets and Anomalies Caused by the Space Environment

•Loss of data•Spurious signals

–False alarms, noise strobes, erroneous telemetry values•Phantom commands

–For example gain changes and attitude sensor errors •Mission or sensor degradation•Solar array degradation•Safeholds•Latchups•Subsystem failure

–Loss of a redundant system•Mission Loss

SHINE 2004 Session 4 38

•Survey of spacecraft anomaly databases (Space Architect Study: Koons et al. 1999)

•This study quantified the impact of the space environment by looking at how long it took to solve the problem

•Difficulties: many spacecraft operators do not want their troubles to be known

•Few radiation damage records probably due to conservative limits in the models & conservative designs

How can one assess the impact of the environment? Examples from one or two missions are not sufficient.

SHINE 2004 Session 4 39

Space Environment Hazardsspacehazard

spacecraftcharging:

single event effects total radiationdose

surfacedegradation

plasmainterference with

spacecraftcommunication

specificcause

surface internal galacticcosmic

rays

trappedradia-tion

solarparticle

trappedradia-tion

solarparticle

ionsputter-

ing

O+erosion

scintilla-tion

waverefract-

ion

LEOi<60

1 1 notapplic-

able

2 notapplic-

able

2 1 1 2 2 2

LEOi>60

1 1 2 2 2 2 1 1 2 2 2

MEO 2 2 2 2 2 2 2 1 2 2 2

GPSi~55

2 2 2 notapplic-

able

2 2 2 1 2 2 2

GTO 2 2 2 2 2 2 2 1 1 2 2

GEO 2 2 2 notapplic-

able

2 2 2 1 1 2 2

HEO 2 2 2 2 2 2 2 1 1 2 2

Inter-planet-

ary

notapplic-

able

notapplic-

able

2 notapplic-

able

2 notapplic-

able

2 1 notapplic-

able

1 1

Table key:2 important1 relevant

SHINE 2004 Session 4 40

6 & 24 November 2001

SHINE 2004 Session 4 41

The inner heliosphere filled with energetic particles

SHINE 2004 Session 4 42

The CME-related shocks caused geomagnetic storms on these

dates:

-300-250-200-150-100-50

050

100

11/1/2001 11/11/2001 11/21/2001 12/1/2001

DsT (nT)

11/6/2001 11/24/2001

DST data from http://swdcwww.kugi.kyoto-u.ac.jp/wdc/Sec3.html

SHINE 2004 Session 4 43

Radial Profile of 15 MeV Protons

1998 1999 2000 2001 2002

Nov. 2001 injections

L=2.5

SHINE 2004 Session 4 44

NOVEMBER 2001

SHINE 2004 Session 4 45

6 and 24 November 2001 Events

• 6 Nov injection may have been prompt, certainly occurred within few hours

• 24 Nov injection partially obscured by 6 Nov, also may have been prompt

• Injection of heavy ions, including Fe observed

• No electrons clearly associated with ion injections

SHINE 2004 Session 4 46

CRRES: >13 MeV electrons

SHINE 2004 Session 4 47

SAMPEX

24 March 1991 remnant

SHINE 2004 Session 4 48

1

10

100

0 500 1000 1500 2000 2500 3000

HEO1 (1994-026)

Day Number (940101=1)

Ee > 1.5 MeVE

e > 3.5 MeVE

e > 6.5 MeV

SHINE 2004 Session 4 49

Particle Lifetimes in New Belts

• Proton livetimes in inner zone determined by energy loss in residual atmosphere and inelastic nuclear collisions

• At 50 MeV, lifetime is ~ 3 years