Table 1
Stellar properties of Proxima.
| Parameter | Proxima | Ref. |
|---|---|---|
| RA (J2000) | 14:29:42.95 | 1 |
| Dec (J2000) | −62:40:46.17 | 1 |
| μα (mas yr−1) | −3781.306 | 1 |
| μδ (mas yr−1) | 769.766 | 1 |
| Parallax (mas) | 768.50 ± 0.20 | 1 |
| Distance (pc) | 1.3012 ± 0.0003 | 1 |
| mB (mag) | 12.95 ± 0.03 | 2 |
| mV (mag) | 11.13 ± 0.01 | 2 |
| mKs (mag) | 4.384 ± 0.0033 | 9 |
| MKs (mag) | 8.813 ± 0.0033 | 10 |
| Spectral type | M 5.5V | 3 |
| L*/L⊙ | 0.0016 ± 0.0006 | 4 |
| Teff (K) | 2900 ± 100 | 5 |
| [Fe/H] (dex) | 0.0 ± 0.1 | 5 |
| M* D00 (M⊙) | 0.120 ± 0.015 | 6 |
| M* M 15 (M⊙) | 0.1221 ± 0.0022 | 7 |
| R* (R⊙) | 0.141 ± 0.021 | 4 |
| Prot (days) | ~83.2 | 8 |
| log g (cgs) | 5.0 ± 0.25 | 5 |
log10 (R |
– 4.98 ± 0.13 | 0 |
Notes. Most works on Proxima b have relied on the stellar mass derived from Delfosse et al. (2000).The measurement derived using Mann et al. (2015) is more precise, so we will use it as our primary measurement, but we also continue to calculate the planetary mass using Delfosse et al. (2000) to allow for a direct comparison with previous measurements.
References. (0) This work – based on Suárez Mascareño et al. (2016), (1) Gaia Collaboration (2016), (2) Jao et al. (2014), (3) Bessell (1991), (4) Boyajian et al. (2012), (5) Pavlenko et al. (2017), (6) estimated using Delfosse et al. (2000, D00), (7) estimated using Mann et al. (2015, M 15), (8) Suárez Mascareño et al. (2016), (9) Cutri et al. (2003), (10) Kervella et al. (2017).
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