Table 1
Summary of the studied relativistic events.
| Column 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | ||
| # GLE / date | tonset(UT) | Max. % | Active region | PS | V SW | Connection | Interplanetary | ||
| increase | location | footpoints | (km s-1) | structure | |||||
|
|
|||||||||
| 59 / 2000-Jul.-14 | 10:31 | 59 | N22, W07 | W43 | 500 | poorly | back region | ||
| 60 / 2001-Apr.-15⋆ | 13:55 | 237 | S20, W85 | W33 | 640 | poorly | disturbed solar wind | ||
| 61 / 2001-Apr.-18⋆ | 02:36 | 26 | behind limb | W60 | 360 | poorly | ICME sheath | ||
| 63 / 2001-Dec.-26⋆ | 05:40 | 13 | N08, W54 | W51 | 420 | well | slow solar wind | ||
| 64 / 2002-Aug.-24⋆ | 01:24 | 14 | S02, W81 | W54 | 400 | well | slow solar wind | ||
| 65 / 2003-Oct.-28⋆ | 11:12 | 47 | S16, E08 | W48 | 450 | poorly | back region | ||
| 66 / 2003-Oct.-29 | 21:01 | 35 | S15, W02 | W48 | 450 | poorly | magnetic cloud | ||
| 67 / 2003-Nov.-02⋆ | 17:30 | 39 | S14, W56 | W36 | 600 | well | back region | ||
| 69 / 2005-Jan.-20 | 06:49 | 5400 | N14, W55 | W39 | 550 | well | disturbed solar wind | ||
| 70 / 2006-Dec.-13⋆ | 02:50 | 92 | S06, W23 | W33 | 660 | well | fast solar wind | ||
Notes. Results obtained from independent studies are synthesized in this table. Column 1: the number and the date of the GLEs. Column 2: the onset time of the first responding neutron monitor. Column 3: maximum percentage increase of the GLE (Belov et al. 2010). Column 4: the location of the parent active region. Column 5: the solar longitude of the Parker spiral footpoint. Column 6: the mean velocity of the solar wind computed on a half-day time interval for a quiet region of the IMF immediately preceding any transient magnetic structures transiting through the Earth during the GLE. Column 7: the nature of connection between the parent active region and the Parker spiral footpoint. Column 8: results of the identification of the magnetic topology of the interplanetary medium. The stars to the right of Col. 1 indicate the GLEs where interplanetary length and solar release time could be estimated (Table 2).
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