Table 1
Relevant parameters of the 16 C-rich stars selected for this study.
| Source name | RA J2000 | Dec J2000 | Distance (pc) | VLSR (km s−1) | Ṁ (M⊙ yr−1) | 2V* (km s−1) | Observation time (h) | Period (days) | L⋆ (L⊙) |
|---|---|---|---|---|---|---|---|---|---|
| W Ori(e) | 05:05:23.72 | +01:10:39.5 | 490 | −1.0 | 3.1 × 10−7 | 22 | 19.33 | 212 | 11600 |
| S Aur(e) | 05:27:07.45 | +34:08:58.6 | 1099 | −17.0 | 5.9 × 10−6 | 51 | 7.08 | 590.1 | 24000 |
| V636 Mon(c) | 06:25:01.43 | −09:07:15.9 | 880 | +10.0 | 5.8 × 10−6 | 40 | 11.06 | 543 | 8472 |
| R Vol(b) | 07:05:36.20 | −73:00:52.02 |  |
−11.0 | (2.9 ± 0.68) × 10−6 | 36 | 16.02 | 453 | 8252 |
| IRC+10216(a) | 09:47:57.4 | +13:16:44 | 140 | −26.5 | 2−4 × 10−5 | 36 | 3.56 | 630 | 8750(c) |
| RAFGL 4211(a) | 15:11:41.9 | −48:20:01 | 950 | −3.0 | 0.93 × 10−5 | 42 | 14.11 | 632 | |
| II Lup(a) | 15:23:05.7 | −51:25:59 | 640 | −15.0 | 1 × 10−5 | 46 | 13.21 | 576 | 8900(d) |
| IRC +20370(c) | 18:41:54.39 | +17:41:08.5 | 600 | −0.8 | 3.0 × 10−6 | 28 | 7.07 | 524 | 7900 |
| V Aql(c) | 19:04:24.15 | −05:41:05.4 | 330 | +53.5 | 1.4 × 10−7 | 16 | 4.11 | 407 | 6500 |
| IRC +30374(c) | 19:34:09.87 | +28:04:06.3 | 1200 | −12.5 | 1.0 × 10−5 | 50 | 3.37 | − | 9800 |
| AQ Sgr(b) | 19:34:18.99 | −16:22:27.04 |  |
+20.0 | 2.5 × 10−6 | 25 | 7.59 | 199.6 | 2490 |
| CRL 2477(c) | 19:56:48.43 | +30:43:59.9 | 3380 | +5.0 | 1.1 × 10−4 | 40 | 2.40 | − | 13200 |
| CRL 2513(c) | 20:09:14.25 | +31:25:44.9 | 1760 | +17.5 | 2.0 × 10−5 | 51 | 2.57 | 706 | 8300 |
| RV Aqr(c) | 21:05:51.74 | −00:12:42.0 | 670 | +0.5 | 2.3 × 10−6 | 30 | 10.7 | 453 | 6800 |
| Y Pav(b) | 21:24:16.74 | −69:44:01.96 |  |
0.0 | (2.8 ± 0.96) × 10−6 | 22 | 12.08 | 449 | 5076 |
| CRL 3068(c) | 23:19:12.24 | +17:11:33.4 | 1300 | −31.5 | 2.5 × 10−5 | 29 | 16.11 | 696 | 10900 |
Notes. This table gives information about the parameters of the sample of the carbon-rich stars. (a)Menten et al. (2018) – distance considered here is DPLR, where the distance is derived from the Mira period-luminosity relation; (b)Rau et al. (2017) (Mass-loss rate from Loup et al. 1993); (c)Massalkhi et al. (2018). (d)Ramstedt & Olofsson (2014); (e) Schöier & Olofsson (2001). The distances for W Ori (220 pc) and S Aur (820 pc) were derived from the Hipparcos measurements and the period-luminosity relation in Schöier & Olofsson (2001), respectively. The distances are updated by the more accurate Gaia parallax measurements (Gaia Collaboration 2018). Their mass-loss rates and luminosities are also updated by scaling the new distances. All periods are from the American Association of Variable Star Observers (AAVSO) (https://www.aavso.org/) with the exception of CRL 2513 and IRC+10216 (Kerschbaum et al. 2006; Menten et al. 2012; Pardo et al. 2018).
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