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SHINE 2004 Session 41 New Radiation Belts and Other Effects of Cycle 23 SEP Events J. E. Mazur, J. B. Blake, P. L. Slocum The Aerospace Corporation M.

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Presentation on theme: "SHINE 2004 Session 41 New Radiation Belts and Other Effects of Cycle 23 SEP Events J. E. Mazur, J. B. Blake, P. L. Slocum The Aerospace Corporation M."— Presentation transcript:

1 SHINE 2004 Session 41 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.

2 SHINE 2004 Session 42 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

3 SHINE 2004 Session 43 Charged particle motion

4 SHINE 2004 Session 44 Cartoons of the inner magnetosphere Reality as viewed with a 15-month average

5 SHINE 2004 Session 45 The inner magnetosphere is host to a variety of time- dependent trapped populations and is not static.

6 SHINE 2004 Session 46 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

7 SHINE 2004 Session 47 Other glimpses of new belts Radiation belt duration from Lorentzen et al. JGR 107(A9), 1231, doi:10.1029/2001JA000276, 2002

8 SHINE 2004 Session 48 There were discontinuous changes to the outer edge of the inner proton belt in 2000 & 2001.

9 SHINE 2004 Session 49 24 March 1991 Creation of >15 MeV electron and >50 MeV proton belts - A lone spacecraft at the right place at the right time -

10 SHINE 2004 Session 410

11 SHINE 2004 Session 411 24 March 1991 shock injection as seen by CRRES The new belts lasted more than 2 years.

12 SHINE 2004 Session 412 Summary of 24 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

13 SHINE 2004 Session 413 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

14 SHINE 2004 Session 414 SAMPEX mission history

15 SHINE 2004 Session 415 New belt example: 24 Nov 2001 Clear trapping of solar particles - no other source of heavy ions possible

16 SHINE 2004 Session 416 Species-dependent injection? SAMPEX Variable composition that does not match solar particles

17 SHINE 2004 Session 417 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

18 SHINE 2004 Session 418 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

19 SHINE 2004 Session 419 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

20 SHINE 2004 Session 420 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

21 SHINE 2004 Session 421 October-November 2003

22 SHINE 2004 Session 422 Protons > 15 MeV No injection of high-energy protons

23 SHINE 2004 Session 423 Electrons >3 MeV Multi-MeV electrons at L~2.5

24 SHINE 2004 Session 424 New heavy-ion belt that lasted ~20 days

25 SHINE 2004 Session 425 Highest intensity of trapped ~0.5 MeV particles at L=2 in 11.5 years

26 SHINE 2004 Session 426 SHINE campaign events

27 SHINE 2004 Session 427 SHINE campaign events: no new ion belts

28 SHINE 2004 Session 428 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

29 SHINE 2004 Session 429 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

30 SHINE 2004 Session 430 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

31 SHINE 2004 Session 431 Backup charts

32 SHINE 2004 Session 432 SAMPEX

33 SHINE 2004 Session 433 SAMPEX

34 SHINE 2004 Session 434 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)

35 SHINE 2004 Session 435 210 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.

36 SHINE 2004 Session 436

37 SHINE 2004 Session 437 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

38 SHINE 2004 Session 438 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.

39 SHINE 2004 Session 439 Space Environment Hazards

40 SHINE 2004 Session 440 6 & 24 November 2001

41 SHINE 2004 Session 441 The inner heliosphere filled with energetic particles

42 SHINE 2004 Session 442 The CME-related shocks caused geomagnetic storms on these dates: DST data from http://swdcwww.kugi.kyoto-u.ac.jp/wdc/Sec3.html

43 SHINE 2004 Session 443 Radial Profile of 15 MeV Protons 1998 1999 2000 20012002 Nov. 2001 injections L=2.5

44 SHINE 2004 Session 444 NOVEMBER 2001

45 SHINE 2004 Session 445 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

46 SHINE 2004 Session 446 CRRES: >13 MeV electrons

47 SHINE 2004 Session 447 SAMPEX 24 March 1991 remnant

48 SHINE 2004 Session 448

49 SHINE 2004 Session 449 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

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