| Reference | Description |
| Bell et al. 1997 Super storms JGR 102, 14189-14198. | Top 2% of storms identified as superstorms. Examined auroral energy input to the inner magnetosphere. |
| Bothmer, V. 2004 The solar and interplanetary causes of space storms in solar cycle 23 | Fractions of storms (Ap>20) caused by Slow Wind, CIR/CH, CME/CIR, CME, multiple CMEs. |
| Bothmer, V. 2003 Sources of Magnetic Helicity Over the Solar Cycle ISCS Conference Proceedings | In-situ inclinations of cloud axes in agreement w/inclinations of polarity inversion lines of the source regions. |
| Burlaga, L.F. et al. 2001 Fast ejecta during the ascending phase of solar cycle 23: ACE observations, 1998-1999 JGR 106, 20957-20977. | Magnetic cloud properties vs complex ejecta properties. |
| Cane, H.V. and Richardson, I.G. 2003 Interplanetary coronal mass ejections in the near-Earth solar wind during 1996-2002 JGR 108, 1156. | ICME source identifications 1996-2002. |
| Canto, J. et al 2005 "The dynamics of velocity fluctuations in the solar wind - I. Coronal Mass Ejections" MNRAS 357, 572. | Analytic model for the dynamical evolution of supersonic velocity fluctuations at the base of the ambient solar wind, applied to CME propogation times from Sun to Earth. |
| Cremades, H. and Bothmer, V. 2004 On the three-dimensional configuration of coronal mass ejections A&A 422, 307-322. | Source region identifications and characteristics of many CMEs from 05 Nov 1996 through 28 Dec 2002. |
| Gonzalez, W.D. 2004 Prediction of peak-Dst from halo CME/magnetic cloud-speed observations JASTP 66, 161-165. | Analytic description of peak Dst values from CME expansion speed. |
| Gopalswamy, N. et al. 2005 Solar source of the largest geomagnetic storm of cycle 23 | 2003 Nov 20 geomagnetic storm source identification. |
| Hoeksema, J.T. and Zhao, X. 1992 "Prediction of Magnetic Orientation in Driver Gas Associated - Bz Events", JGR, 97, 3151-3157. | Compared PFSS model results at source location (at 1.03Rs) to ISEE-3 mag data for 5 events, with favorable result for predicting Bz in 3 flare-related CME's, but not for 1 erupting prominence result. |
| Huttunen, K.E.J. et al 2005 Properties and geoeffectiveness of magnetic clouds in the rising, maximum and early declining phases of solar cycle 23 Ann. Geo. 23, 1-17. | Bi-polar clouds in rising phase of Cycle 23 rotated S-N. Switched to N-S at Solar Max. Separated effects of sheath from magnetic cloud. |
| Huttunen, K.E.J. and Koskinen, H.E.J. 2004 Importance of post-shock streams and sheath region as drivers of intense magnetic storms and high-latitude activity Ann. Geo. 22, 1729-1738. | Storm caused by MC different from storm caused by sheath or post-shock stream. Sheath and post-shock stream caused storms tend to favor high-latitude activity. |
| Kahler, S. 1993 "A Search for Geomagnetic Storm Evidence of the Reversal of the Solar Dipole Magnetic Field and Interplanetary Bz" JGR 98, 3485-3489. | No evidence solar dipole preserved in coronal ejecta. No solar cycle dependence for Bz. |
| Mac-Mahon, R.M. and Gonzalez, W.D. 1997 Energetics during the main phase of geomagnetic superstorms JGR 102, 14199-14207. | Global energetics: calculation of solar wind energy budget and the energy transfer into the magnetosphere. |
| Mulligan, T. et al 1998 Solar cycle evolution of the structure of magnetic clouds in the inner heliosphere GRL 25 2959-2962. | Leading mag field in clouds is controlled by polarity of suns global field. Inclination of coronal streamer belt controls axis of symmetry of clouds. Helicity not ordered by solar cycle. |
| Vilmer, N. 2003 On the solar origin of interplanetary disturbances observed in the vicinity of the Earth Ann. Geo. 21, 847-862. | Source identification for 40 interplanetary disturbances. |
| Webb, D.F. et al 2000 Relationship of halo coronal mass ejections, magnetic clouds, and magnetic storms JGR 105, 7491-7508. | Not all clouds had LASCO counterparts. Some geoactivity source identification. |
| Wu, C.-C. et al 2004 Relationships between magnetic clouds, CMEs and geomagnetic storms, Proc. of IAU Symp. 226. | Magnetic Clouds + Magnetic Cloud-like events correlate highly with CME rate, whereas MCs alone do not. |
| Xie, H. et al 2004 CMEs and long-lived geomagnetic storms: A case study Proc. IAU Symp 226. | The 1998 May 2-7 Geomagnetic Storm. |
| Yermolaev, Y.I. and Yermolaev, M.Y. 2002 Statistical Relationships between Solar, Interplanetary, and Geomagnetic Disturbances, 1976-2000 Cosmic Res. 40, 1-14. | Source identifications for many events from 1976-2000. Fraction of storms from MC and CIR as a function of storm strength. |
| Yermolaev, Y.I. and Yermolaev, M.Y. 2003 "Statistical Relationships between Solar, Interplanetary, and Geomagnetic Disturbances, 1976-2000: 2" Cosmic Res. 41, 105-109. | Continuation of the previous study, considering flares > M5 and halo CMEs. Correlations of these phenomena with geomagnetic storms as a function of Dst. |
| Yermolaev, Y.I. et al. 2005 "Statistical studies of geomagnetic storm dependencies on solar and interplanetary events: a review" P&SS 53, 189-196. | A survey of the methods used to correlate events at the Sun with storms at the Earth. |
| Zhang, J. et al 2003 Identification of Solar Sources of Major Geomagnetic Storms Between 1996 and 2000 AJ 582, 520-533. | Source identifications from 1996-2000. A CME transit time formula. |
| Zhao, X.P. and Hoeksema, J.T. 1997 Is the geoeffectiveness of the 6 January 1997 CME predictable from solar observations? GRL 24, 2965-2968. | January 6, 1997 CME Bz prediction
DSF central axis orientation Impact parameter |
| Zhao, X.P. and Webb, D.F. 2003 Source regions and storm effectiveness of frontside full halo coronal mass ejections JGR 108, 1234. | CME fractions from bi-polar and uni-polar sources through rise in solar cycle. Streamer belt inclination change lowers rate of ecliptic CMEs. |
| Zhukov, A. 2004 Solar sources of geoeffective CMEs: a SOHO/EIT view Proc. of IAU Symp. 226. | Identification of very weak halo CME in LASCO. Consider using EUV signatures as a CME proxy. Some sigmoid discussion. |