Coronal and interplanetary radio emission as a tracer of solar energetic particle propagation


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Coronal and interplanetary radio emission as a tracer of solar energetic particle propagation

  • Karl-Ludwig Klein




The coronal magnetic field and SEP transport

  • Radio observations and magnetic field extrapolations.



Type III bursts and PFSS extrapolations as tracers of open flux tubes in the corona

  • Solar release time of energetic particles (p 5-55 MeV, SoHO/COSTEP; e 30-500 keV, Wind/3DP) from energy dispersion of onset times.

  • Events accompanied by type III bursts (e- beams 10 keV)

    • Track radio emission to 1 AU (ground + Wind/WAVES)
    • m- maps at several  - sections of open flux tube at several altitudes in the corona (Nançay Radioheliograph).
  • Compare with potential magnetic field extrapolations (SolarSoft; Schrijver & DeRosa).







Type III emitting electrons travel to high latitude in the corona, but are in the ecliptic at 1 AU  IP field line curves down to the ecliptic before reaching 1 AU ( Parker).

  • Type III emitting electrons travel to high latitude in the corona, but are in the ecliptic at 1 AU  IP field line curves down to the ecliptic before reaching 1 AU ( Parker).

  • The failure is due to the Parker model, not to the PFSS extrapolation !





2008 November 4

  • SEP event: 2 electron injections at all three s/c

  • SWAVES/STEREO: two successive DH III

  • Weak impulsive SEP

    • SXR burst, peak 03:17 (after Mason et al. 2009; is this consistent with the following ???)
    • H flare: SF, start 03:26, max 03:29, N35 W38 (LEAR/SGD)
    • Type III 03:22-03:36, 160 MHz (different obs / SGD)
    • Weak microwave burst (NoRP 2 GHz)
  • No imaging observations (NRH), but SWAVES shows similar radio events later on Nov 04



2008 November 4





2008 November 3 & 4: noise storm sources



2008 November 4: PFSS and radio sources



2008 November 4: PFSS and radio sources









Radio astronomical constraints on energetic particle propagation in the corona

  • The radio emission of electron beams (« type III bursts ») can be used as tracer of open coronal magnetic flux tubes.

  • Type III bursts and magnetic field extrapolations show that

    • open magnetic field lines rooted in small parts of AR diverge rapidly with height and can easily cover 90° in solar longitude;
    • strongly curved open field lines connect solar active regions to the nominal Earth-connected Parker spiral even when the parent active region is several tens of degrees away in longitude.
  • Type III bursts and Langmuir waves in situ imply that the interplanetary field lines may curve downward (Parker)

  • 2008 November 04 and 2009 May 01:

    • Type III bursts at long m-; from high coronal sources;
    • 2008 Nov 04: noise storm at shorter m-, closed coronal structures at that height (within 0.5 R)
    • Type III at greater altitude; open flux tubes, streamer-like configuration
    • Similar 2009 May 01 ?



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