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Solar Physics

, Volume 285, Issue 1–2, pp 251–267 | Cite as

Initial Fe/O Enhancements in Large, Gradual, Solar Energetic Particle Events: Observations from Wind and Ulysses

  • Allan J. TylkaEmail author
  • Olga E. Malandraki
  • Gareth Dorrian
  • Yuan-Kuen Ko
  • Richard G. Marsden
  • Chee K. Ng
  • Cecil Tranquille
OBSERVATIONS AND MODELLING OF THE INNER HELIOSPHERE

Abstract

Shocks driven by fast coronal mass ejections (CMEs) are the dominant particle accelerators in large, “gradual” solar energetic particle (SEP) events. In these events, the event-integrated value of the iron-to-oxygen ratio (Fe/O) is typically ∼ 0.1, at least at energies of a few MeV/nucleon. However, at the start of some gradual events, when intensities are low and growing, initially Fe/O is ∼ 1. This value is also characteristic of small, “impulsive” SEP events, in which particle acceleration is due to magnetic reconnection. These observations suggested that SEPs in gradual events also include a direct contribution from the flare that accompanied the CME launch. If correct, this interpretation is of critical importance: it indicates a clear path to interplanetary space for particles from the reconnection region beneath the CME. A key issue for the flare origin is “magnetic connectedness”, i.e., proximity of the flare site to the solar footpoint of the observer’s magnetic field line.

We present two large gradual events observed in 2001 by Wind at L1 and by Ulysses, when it was located at > 60 heliolatitude and beyond 1.6 AU. In these events, transient Fe/O enhancements at 5 – 10 MeV/nucleon were seen at both spacecraft, even though one or both is not “well-connected” to the flare. These observations demonstrate that an initial Fe/O enhancement cannot be cited as evidence for a direct flare component. Instead, initial Fe/O enhancements are better understood as a transport effect, driven by the different mass-to-charge ratios of Fe and O.

We further demonstrate that the time-constant of the roughly exponential decay of the Fe/O ratio scales as R 2, where R is the observer’s radial distance from the Sun. This behavior is consistent with radial diffusion. These observations thus also provide a potential constraint on models in which SEPs reach high heliolatitudes by cross-field diffusion.

Keywords

Solar Energetic Particles (SEPs) Solar flares Coronal mass ejections Ulysses Wind 

Notes

Acknowledgements

The authors thank Dr. Y.M. Wang for providing the PFSS model results, Dr. Donald V. Reames for the Wind/EPACT/LEMT data, and Prof. Bruce McKibben for the Ulysses/HET data. This work has been supported by the NASA Heliophysics Guest Investigator Program under DPR NNH09AK79I and by the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement number 263252 [COMESEP].

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Copyright information

© Springer Science+Business Media B.V. (outside the USA)  2012

Authors and Affiliations

  • Allan J. Tylka
    • 1
    Email author
  • Olga E. Malandraki
    • 2
  • Gareth Dorrian
    • 2
  • Yuan-Kuen Ko
    • 1
  • Richard G. Marsden
    • 3
  • Chee K. Ng
    • 4
  • Cecil Tranquille
    • 3
  1. 1.Code 7680, Space Science DivisionNaval Research LaboratoryWashingtonUSA
  2. 2.Institute of Astronomy, Astrophysics, Space Applications and Remote SensingNational Observatory of AthensAthensGreece
  3. 3.European Space Agency (SRE-SM)ESTECNoordwijkThe Netherlands
  4. 4.College of ScienceGeorge Mason UniversityFairfaxUSA

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