Table 1.
Back mapping polarity measure for the spherical source surface at 2.5 R⊙.
Spacecraft | Solar wind | Period 1 (declining) | Period 2 (minimum) | Period 3 (maximum) | ||||||
---|---|---|---|---|---|---|---|---|---|---|
type | CR2041−CR2055 |
CR2066−CR2075 |
CR2133−CR2142 |
|||||||
n | pm, s/pm, e | σs/σe | n | pm, s/pm, e | σs/σe | n | pm, s/pm, e | σs/σe | ||
(%) | (%) | (%) | (%) | (%) | (%) | |||||
ACE | Ejecta | 969 | 79/79 | 2.9/3.0 | 485 | 73/75 | 2.4/2.6 | 1644 | 72/71 | 1.7/1.7 |
Coronal hole | 8464 | 94/93 | 0.2/0.3 | 11 097 | 94/94 | 0.2/0.2 | 5364 | 89/85 | 1.2/1.8 | |
Sector reversal | 10 646 | 60/60 | 1.2/1.3 | 7570 | 65/69 | 1.9/1.6 | 7822 | 59/57 | 0.8/0.9 | |
Streamer belt | 11 494 | 79/77 | 0.7/0.9 | 13 284 | 81/82 | 0.5/0.7 | 14 076 | 76/70 | 1.4/1.9 | |
Overall | 31 573 | 76/75 | 0.7/0.8 | 32 436 | 82/83 | 0.5/0.5 | 28 906 | 74/69 | 1.0/1.2 | |
STEREO-A | Ejecta | 15 048 | 87/86 | 1.6/1.9 | 40 060 | 74/72 | 1.1/1.4 | |||
Coronal hole | 123 548 | 89/90 | 0.5/0.3 | 61 216 | 90/88 | 0.4/0.6 | ||||
Sector reversal | 66 893 | 61/68 | 2.0/1.2 | 46 468 | 51/53 | 1.9/1.8 | ||||
Streamer belt | 163 059 | 83/84 | 0.6/0.6 | 155 228 | 75/72 | 1.1/1.3 | ||||
Overall | 368 548 | 81/83 | 0.6/0.4 | 302 972 | 74/72 | 0.7/0.9 | ||||
STEREO-B | Ejecta | 8421 | 81/85 | 4.0/2.0 | 10 325 | 76/79 | 1.5/1.3 | |||
Coronal hole | 91 748 | 93/93 | 0.4/0.5 | 8003 | 87/71 | 2.8/8.1 | ||||
Sector reversal | 58 988 | 67/72 | 1.2/1.2 | 7956 | 64/64 | 1.5/2.3 | ||||
Streamer belt | 108 680 | 83/82 | 0.9/1.2 | 30 247 | 74/73 | 1.3/1.9 | ||||
Overall | 267 837 | 83/84 | 0.7/0.7 | 56 531 | 75/73 | 1.2/1.6 |
Notes. The first column lists the spacecraft, the second column lists the solar wind types, and Cols. 3−5 show the data for three different periods. Also shown are the sample count (n) and the correctly predicted magnetic field polarity fractions (pm, s/e) and standard deviations (σs/e) of the evaluation procedure for the standard rss = 2.5 R⊙ spherical PFSS model (subscript s) and the elliptic model with parameters rss = 2.5 R⊙ and eo = 1.667 (subscript e). Data samples were partitioned according to the Xu & Borovsky (2015) scheme into four classes of solar wind types for three periods (columns) and three spacecraft (rows). Analyzing streamer belt wind on the ACE during solar activity minimum shows that there were n = 13 284 data samples available, 80.8% (= pm, s) of which mapped to correctly predicted magnetic field polarities on the source surface with a standard deviation of σs = 0.5% in the spherical model.
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