Corotating interaction regions at high latitudes: Report of Working Group 3

H. Kunow, M. A. Lee, L. A. Fisk, R. J. Forsyth, B. Heber, T. S. Horbury, E. Keppler, J. Kóta, Y. Q. Lou, R. B. McKibben, C. Paizis, M. S. Potgieter, E. C. Roelof, T. R. Sanderson, G. M. Simnett, R. Von Steiger, B. T. Tsurutani, R. F. Wimmer-Schweingruber, J. R. Jokipii

Research output: Contribution to journalArticle

20 Scopus citations

Abstract

Ulysses observed a stable strong CIR from early 1992 through 1994 during its first journey into the southern hemisphere. After the rapid latitude scan in early 1995, Ulysses observed a weaker CIR from early 1996 to mid-1997 in the northern hemisphere as it traveled back to the ecliptic at the orbit of Jupiter. These two CIRs are the observational basis of the investigation into the latitudinal structure of CIRs. The first CIR was caused by an extension of the northern coronal hole into the southern hemisphere during declining solar activity, whereas the second CIR near solar minimum activity was caused by small warps in the streamer belt. The latitudinal structure is described through the presentation of three 26-day periods during the southern CIR. The first at ∼24°S shows the full plasma interaction region including fast and slow wind streams, the compressed shocked flows with embedded stream interface and heliospheric current sheet (HCS), and the forward and reverse shocks with associated accelerated ions and electrons. The second at 40°S exhibits only the reverse shock, accelerated particles, and the 26-day modulation of cosmic rays. The third at 60°S shows only the accelerated particles and modulated cosmic rays. The possible mechanisms for the access of the accelerated particles and the CIR-modulated cosmic rays to high latitudes above the plasma interaction region are presented. They include direct magnetic field connection across latitude due to stochastic field line weaving or to systematic weaving caused by solar differential rotation combined with non-radial expansion of the fast wind. Another possible mechanism is particle diffusion across the average magnetic field, which includes stochastic field line weaving. A constraint on connection to a distant portion of the CIR is energy loss in the solar wind, which is substantial for the relatively slow-moving accelerated ions. Finally, the weaker northern CIR is compared with the southern CIR. It is weak because the inclination of the streamer belt and HCS decreased as Ulysses traveled to lower latitudes so that the spacecraft remained at about the maximum latitudinal extent of the HCS.

Original languageEnglish (US)
Pages (from-to)221-268
Number of pages48
JournalSpace Science Reviews
Volume89
Issue number1-2
DOIs
StatePublished - 1999

Keywords

  • CIRs
  • High latitude heliosphere
  • Interplanetary medium
  • Solar wind

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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    Kunow, H., Lee, M. A., Fisk, L. A., Forsyth, R. J., Heber, B., Horbury, T. S., Keppler, E., Kóta, J., Lou, Y. Q., McKibben, R. B., Paizis, C., Potgieter, M. S., Roelof, E. C., Sanderson, T. R., Simnett, G. M., Von Steiger, R., Tsurutani, B. T., Wimmer-Schweingruber, R. F., & Jokipii, J. R. (1999). Corotating interaction regions at high latitudes: Report of Working Group 3. Space Science Reviews, 89(1-2), 221-268. https://doi.org/10.1023/a:1005218010508