1. List of Interplanetary Coronal Mass Ejections (ICMEs)
ICME list in pdf format
ICME list in excel format
The ICMEs are identified based by inspection of a combination signatures: an enhancement of total perpendicular pressure (Pt = B2/(2&mu0) + &SigmajnjkTperp,j, where j represents the three major species in the solar wind: protons, electrons and alpha particles, see Russell et al., 2005. Its gradient indicates the force), a stronger than ambient magnetic field, relatively quiet and smooth magnetic field rotations, a declining solar wind speed, a low proton temperature [Jian et al., 2006a].
At least three of the above features were required to identify an ICME. The edges of ICMEs were identified from a consensus of available features, usually delimited by sharp changes in plasma and magnetic field properties. For ambiguous events, we checked the SOHO LASCO CME catalog and STEREO SECCHI observations.
2. List of Stream Interaction Regions (SIRs)
SIR list in pdf format
SIR list in excel format
The SIRs include corotating interaction regions (CIRs) and transient stream interaction regions. The difference between a CIR and a transient SIR is only that a CIR recurs for two or more solar rotation cycle.
The SIRs are identified based on inspection of the following features: an increase of solar wind speed, a pile-up of total perpendicular pressure (Pt) with gradual decreases at both sides from the Pt peak to the edges of interaction region, velocity deflections, an increase of proton number density, an enhancement of proton temperature, an increase of the entropy defined as ln(Tp3/2/Np) [Siscoe and Intriligator, 1993; Crooker et al., 1996], a compression of the magnetic field. We require the presence of at least 5 signatures, and identify SIRs with careful consideration of the ambient solar wind. For detail, please refer to Jian et al., 2006b.
3. List of Interplanetary Shocks
Shock list in pdf format
Shock list in excel format
The forward and reverse shocks are identified using 8-Hz magnetic field data. We rotated them into shock normal coordinates to examine the existence of associated shock waves and field changes consistent with the Rankine-Hugoniot relations. The shock normal angle (&thetaBn), field change, and Mach number, are also given in this list.
To confirm, we have also checked the 1-min PLASTIC data. At forward shocks, all of solar wind speed, proton number density, proton temperature, and magnetic field should increase simultaneously. At reverse shocks, solar wind speed increases, while proton number density, proton temperature, and magnetic field all decrease. However, not all shocks have clear signatures in plasma properties. We indicate such shocks in the comments.
4. List of Solar Energetic Particle (SEP) Events Observed by both STA and STB"
5. List of PLASTIC Suprathermal Proton Events from University of New Hampshire
Crooker, N.U., M.E. Burton, G.L. Siscoe, S.W. Kahler, J.T. Gosling, and E.J. Smith (1996), Solar wind streamer belt structure, J. Geophys. Res., 101, 24331.
Jian, L., C.T. Russell, J.G. Luhmann, and R.M. Skoug (2006a), Properties of interplanetary coronal mass ejections at one AU during 1995 - 2004, Sol. Phy., 239, 393, doi: 10.1007/s11207-006-0133-2.
Jian, L., C.T. Russell, J.G. Luhmann, and R.M. Skoug (2006b), Properties of stream interaction at one AU during 1995 - 2004, Sol. Phy., 239, 337, doi: 10.1007/s11207-006-0132-3.
Russell, C.T., A.A. Shinde, and L. Jian (2005), A new parameter to define interplanetary coronal mass ejections, Adv. Space Res., 35, 2178.
Siscoe, G., and D. Intriligator (1993), Three views of two giant streams: aligned observations at 1 AU, 4.6 AU, and 5.9 AU, Geophys. Res. Lett., 20 (20), 2267.