Table 3.
Computation parameters and effect on the wind speed determination.
| Computation input | Source | Adopted values | Effect on wind speed |
|---|---|---|---|
| parameters | determination | ||
| Lya disk irradiance | Machol et al. (2019) | 7 days averaged | < 5% |
| (LASP) | |||
| Lya disk profile | Auchère (2005) | Analytical | < 10% |
| (SUMER) | Capuano et al. (2021) | ||
| Electron temperature | Gibson et al. (1999) | G99 profile | ∼40% (slow wind) |
| Vásquez et al. (2003) | V03 profiles | ∼20% (fast wind) | |
| See Fig. 7 | [0.4, ...1.6] MK | See Figs. 10, 11 | |
| Kinetic temperature | Cranmer et al. (1999) | [1.0, ..., 3.0] MK | ∼10% (slow wind) |
| Antonucci et al. (2000) | ∼18% (fast wind)(1) | ||
| Dolei et al. (2016) | See Fig. 12 | ||
| (UVCS) | |||
| Anisotropy | Susino et al. (2008) | [1, 2] | ∼5% (slow wind) |
| Cranmer (2020) | ∼15% (fast wind) | ||
| (UVCS) | See Fig. 13 | ||
| He abundance | Moses et al. (2020) | [2.5, 10]% | < 5% |
| (SCORE) | |||
Notes. (1)The kinetic temperature was varied between 1 and 3 MK in the parameter grids, resulting in an overall wind speed uncertainty of approximately 30%. Kinetic temperatures exceeding 2 MK are not physically expected in coronal holes, however. By restricting the kinetic temperature range to 1−2 MK, we reduced the wind speed uncertainty to about 18%.
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