Solar Physics

, Volume 239, Issue 1, pp 337–392

Properties of Stream Interactions at One AU During 1995 – 2004

  • L. Jian
  • C. T. Russell
  • J. G. Luhmann
  • R. M. Skoug
Article

DOI: 10.1007/s11207-006-0132-3

Cite this article as:
Jian, L., Russell, C.T., Luhmann, J.G. et al. Sol Phys (2006) 239: 337. doi:10.1007/s11207-006-0132-3

Abstract

A stream interaction region (SIR) forms when a fast solar stream overtakes a slow stream, leading to structure that evolves as an SIR moves away from the Sun. Based on Wind (1995 – 2004) and ACE (1998 – 2004) in situ observations, we have conducted a comprehensive survey of SIRs at one AU, including a separate assessment of the longer-lasting corotating interaction regions (CIRs) that recur on more than one solar rotation. In all there are 196 CIRs, accounting for about 54% of the 365 SIRs. The largest proportion of CIRs to SIRs (64%) appears in 1999, and the smallest proportion (49%) is in 2002. Over the ten years, the annual number of SIR events varies little, from 32 up to 45. On average, the occurrence rate of shocks at SIRs at one AU is about 24%. Seventy percent of the SIRs with shocks have only forward shocks, more than twice the percentage of SIRs with only reverse shocks. This preponderance of forward shocks is consistent with the deflections of forward and reverse shocks relative to the ecliptic plane. In order to help address the effect of SIRs and CIRs on geomagnetic activity, we determine the solar-cycle variation of the event duration, scale size, the change in velocity from slow stream to fast stream, and the solar-cycle variation of the maximum magnetic field, peak total perpendicular pressure, and other properties. These statistics also provide a baseline for future studies at other heliocentric distances and for validating heliospheric models.

Supplementary material

Copyright information

© Springer Science + Business Media, Inc. 2006

Authors and Affiliations

  • L. Jian
    • 1
  • C. T. Russell
    • 2
  • J. G. Luhmann
    • 3
  • R. M. Skoug
    • 4
  1. 1.Institute of Geophysics and Planetary PhysicsUniversity of California, Los AngelesLos AngelesU.S.A.
  2. 2.Institute of Geophysics and Planetary PhysicsUniversity of California, Los AngelesLos AngelesU.S.A.
  3. 3.Space Sciences LaboratoryUniversity of CaliforniaBerkeleyU.S.A.
  4. 4.Los Alamos National LaboratoryLos AlamosU.S.A.

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