Table 2
Stellar sample.
| Star | VY CMa | VX Sgr | W Hya | U Her | R Aql |
|
|
|||||
| RA | 07:22:58.33 | 18:08:04.05 | 13:49:02.00 | 16:25:47.47 | 19:06:22.25 |
| Dec | −25:46:03.2 | −22:13:26.6 | −28:22:03.5 | +18:53:32.9 | +08:13:48.0 |
| Distancea | 1.2 kpc | 1.6 kpc | 104 pc | 266 pc | 422 pc |
| Typeb | RSG | RSG | Mira/SRa | Mira | Mira |
| Spectral typeb | M5 | M4−M10 | M7−M9 | M6.5−M9.5 | M5e−M9e |
| Current period (days)b | 1600 | 732 | 390 | 404 | 270.5 |
| Magnitude rangeb | 6.5−9.6 V | 6.5−14 V | 5.6−9.6 V | 6.4−13.4 V | 5.5−12 V |
| Masers | SiO, H2O, OH | SiO, H2O, OH | SiO, H2O, OH | SiO, H2O, OH | SiO, H2O, OH |
| Mass loss ratesc (M⊙ yr-1) | 1.8 × 10-4 | 6.3 × 10-5 | 1.4 × 10-7 | 1.6 × 10-7 | 2–14 × 10-6 |
Notes.
Distances are from: W Hya and R Aql (Hipparcos, van Leeuwen 2007), VY CMa (Choi et al. 2008; Zhang et al. 2012), VX Sgr (Chen et al. 2007) and U Her (Vlemmings & van Langevelde 2007).
From the AAVSO, except for the period of VY CMa which is from Kiss et al. (2006).
Mass loss rates, scaled to the distances used here, are from De Beck et al. (2010) for VY CMa, VX Sgr and W Hya. For U Her and R Aql, these are from Yates et al. (1995) and Zhao-Geisler et al. (2012), respectively.
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