Table 2
Modeling parameters and figures in which they have been used.
| Case study | 1P/Halley (Giotto flyby) | 67P/C-G (low activity) | 67P/C-G (high activity, perihelion) | General case (this work) |
|---|---|---|---|---|
| Cometary radius (km) | ~ 5.5 (d) | ~ 2 (d) | ~2 (d) | 2 |
| Heliocentric distance (au) | 0.89 | 3.2 (b) | 1.24 | ⋯ |
| Local photoionization frequency (s−1) | 8.6 × 10−7 | 6.8 × 10−8 | 4.5 × 10−7 | ⋯ |
| Local outgassing rate (s−1) | 6.9 × 1029 (a) | 6 × 1025 (b) | 6 × 1028 (c) | 1025–1030 |
| Neutral velocity (m⋅s−1) | 900 (a) | 600 (a),(c) | 900 (c) | 600 |
| Electron temperature (K) | [150-1000] | 150 | 150 | 150 |
| Photoabsorption cross section (m2) | ⋯ | ⋯ | ⋯ | 7.82 × 10−22 |
| Cases shown in figures | 1, 11, 12 | 1, 11, 12 | 1, 11, 12 | 2–5, 8 |
Notes. Three cases have been considered: 1P during the Giotto flyby, 67P at perihelion, and 67P at the beginning of the escort phase. The photoionization frequency is that of water for averaged conditions during the Rosetta escort phase (7 × 10−7 s−1 at 1 au, Heritier et al. 2018) and has been corrected for the heliocentric distance.
References. (a) Krankowsky et al. (1986); (b)Galand et al. (2016); (c)Hansen et al. (2016); (d)Lamy et al. (2004).
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