Table 1
Sample of AGB envelopes and associated parameters.
| Source | Vsys (a) | D(b) | L⋆ | T* | τ10 | Td(rc) | Ṁ(c) | δ | υ∞ (a) | Ψ | |
|---|---|---|---|---|---|---|---|---|---|---|---|
| (km s−1) | (pc) | (L⊙) | (K) | (K) | (cm) | (M⊙ yr−1) | (km s−1) | ||||
| O-rich | |||||||||||
| R Leo | +0.1 | 111 ± 17(d) | 7000 | 2803(i) | 0.032 | 1000 | 1.8 × 1014 | 1.3 × 10−7 | 0.30 | 5 | 420 |
| R Cas | +26.5 | 174 ± 6 | 6800 | 3129(j) | 0.20 | 1400 | 9.3 × 1013 | 9.5 × 10−7 | 0.60 | 7.5 | 640 |
| TX Cam | + 11.5 | 287±14 | 4600 | 2778(k) | 0.63 | 1300 | 9.3 × 1013 | 3.9 × 10−6 | 0.50 | 17.5 | 360 |
| IK Tau | +34.5 | 261 ± 19 | 7900 | 2234(l) | 1.0 | 1000 | 2.0 × 1014 | 4.8 × 10−6 | 0.65 | 17.5 | 130 |
| V1111 Oph | −31 | 502 ± 31 | 5000 | 2667(k) | 1.3 | 1100 | 1.5 × 1014 | 8.5 × 10−6 | 0.70 | 15.5 | 260 |
| GX Mon | −9.5 | 569 ± 53 | 6300 | 2173(m) | 1.0 | 900 | 2.2 × 1014 | 1.6 × 10−5 | 0.70 | 18 | 380 |
| NV Aur | +3 | 1360 | 10700(g) | 2500(j) | 2.5 | 1000 | 2.8 × 1014 | 2.0 × 10−5 | 0.65 | 17.5 | 150 |
| C-rich | |||||||||||
| Y CVn | +22 | 310 ± 17 | 8500 | 2760(n) | 0.0063 | 1000 | 1.9 × 1014 | 2.1 × 10−7 | 0.50 | 7 | 1360 |
| R Lep | +11.5 | 456±13 | 7800 | 2290(n) | 0.079 | 1300 | 8.9 × 1013 | 2.1 × 10−6 | 0.60 | 17.5 | 900 |
| LP And | −17 | 526 ± 131(e) | 3700 | 2040(n) | 0.79 | 1200 | 9.9 × 1013 | 5.3 × 10−6 | 0.70 | 14.5 | 250 |
| IRC+20370 | −0.8 | 753 ± 113 | 11 300 | 2200(j) | 0.40 | 1300 | 1.3 × 1014 | 5.8 × 10−6 | 0.65 | 14 | 420 |
| IRC+30374 | −12.5 | 823 ± 51 | 6300 | 2500(o) | 0.79 | 1500 | 8.9 × 1013 | 9.9 × 10−6 | 0.75 | 25 | 300 |
| IRC+ 10216 | −26.5 | 123 ± 14(f) | 7800 | 2330(p) | 0.79 | 900 | 2.8 × 1014 | 2.4 × 10−5(q) | 0.95(q) | 14.5 | 390 |
| CRL 190 | −39.5 | 3370 | 16700(h) | 2500(o) | 5.0 | 1400 | 3.1 × 1014 | 3.9 × 10−5 | 1.05 | 17 | 80 |
Notes. Unless otherwise stated, the parameters L⋆, τ10, Td(rc), rc, Ṁ, δ, and Ψ are determined in this study. (a) From Massalkhi et al. (2020) for O-rich stars and Massalkhi et al. (2018) for C-rich stars. (b) From Gaia DR3 (Gaia Collaboration 2023) unless otherwise stated. Uncertainties in the distances from Gaia DR3 are likely underestimated (Andriantsaralaza et al. 2022). The distances of NV Aur and CRL 190 are derived in this study from the luminosity and a fit to the SED. (c) The estimated uncertainty in the mass-loss rate is 20% (see Sect. 3.2). (d) From combined parallax measured by Allegheny Observatory and HIPPARCOS (Whitelock et al. 2008). (e) Value from Nearby Evolved Stars Survey (https://evolvedstars.space; Scicluna et al. 2022) is preferred over Gaia DR3 value (413 ± 41) because the resulting luminosity agrees better with the period-luminosity relation (Groenewegen & Whitelock 1996). (f) Groenewegen et al. (2012).(g) From the period-luminosity relation (Olivier et al. 2001). (h) From the period-luminosity relation (Groenewegen et al. 2002). (i) Perrin et al. (1999). (j) De Beck et al. (2010). (k) van Loon et al. (2005). (l) Adam & Ohnaka (2019). (m) Karovicova et al. (2013). (n) Bergeat et al. (2001). (o) Rough estimate by Groenewegen et al. (1998). (p) Ridgway & Keady (1988).(q) Mass-loss rate for IRC +10216 fixed to 2.4 × 10−5 M⊙ yr−1 (Fonfría et al. 2022). The gas temperature radial profile adopted consists of three components with δ = 1.00 between 1015 and 1016 cm, δ = 0.45 inward of 1015 cm, and δ = 1.55 beyond 1016 cm.
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