Table 4.
First intersection between the coronal shock and magnetic field lines connecting the spacecraft.
| s/c | Estimated first | Shock height from | θBn at the | Cobpoint | ||||
|---|---|---|---|---|---|---|---|---|
| intersection time (UT) (a) | sun centre (R⊙) | cobpoint (deg) (b) | ||||||
| Parker | ENLIL | Parker | ENLIL | Parker | ENLIL | Parker | ENLIL | |
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) |
| (STA | 22:41 ± 10 min | 22:42 ± 10 min | 2.6 ± 0.3 | 2.8 ± 0.3 | 37 ± 2 | 24 ± 2 | E157S04 | E164S05) |
| (MESS | 22:38 ± 10 min | 22:42 ± 10 min | 2.5 ± 0.3 | 3.0 ± 0.3 | 5 ± 1 | 9 ± 1 | W179N01 | W174N01) |
| STA | 22:55 ± 10 min | 22:55 ± 10 min | 3.3 ± 0.3 | 3.2 ± 0.3 | 17 ± 2 | 22 ± 2 | E157S04 | E164S05 |
| MESS | 22:55 ± 10 min | 22:55 ± 10 min | 3.5 ± 0.3 | 3.5 ± 0.3 | 4 ± 1 | 7 ± 1 | W179N01 | W174N01 |
Notes. As the estimated first intersection times occur in the first step of the coronal shock reconstruction using coronagraph data from both STEREO and LASCO (last two lines), we also present the first intersection results calculated using EUVI/COR1 data from both STEREO instruments (first two lines in brackets). Details given in main text.
Angle between the shock normal and the upstream magnetic field line at the cobpoint. The given uncertainties are rounded to one degree. They are based on the shock height deviation due to the coronagraph images cadence (the fluctuations in the magnetic field lines, due to waves and turbulence, or in the shock front geometry are not considered).
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