Table 2
Envelope parameters.
| Source | Rinner (cm) | Tinner (K) | τ UV | LUV (erg s−1 | XISRF | LX (erg s−1) | L (L⊙) | α | (Ṁ (M⊙ yr−1 | β | Vexp (km s−1) | r1/2 (cm) |
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| T Dra(a) | 1.5×1014 | 1200 | 7.2 | 1.8×1034 | 2.1×108 | 4.1e×1031 | 9000 | 2.65 | 4.1×10−6 | 1.00 | 14.0 | 2×1017 |
| T Dra(b) | 1.5×1014 | 1200 | 7.2 | 1.8×1034 | 2.1×108 | 4.1e×1031 | 9000 | 2.65 | 2.3×10−6 | 0.75 | 14.0 | 2×1017 |
| EY Hya | 7.0×1013 | 1350 | 1.0 | 3.3×1031 | 3.9×105 | 1.1×1031 | 6400 | 2.35 | 2.8×10−7 | 0.35 | 10.0 | 3×1016 |
| VY Uma | 6.0×1013 | 1450 | 0.5 | 1.6×1031 | 1.9×105 | – | 5300 | 2.40 | 1.0×10−7 | 0.80 | 5.5 | 3×1016 |
| V Eri | 8.0×1013 | 1250 | 1.0 | 1.4×1031 | 1.7×105 | – | 5800 | 2.35 | 2.8×10−7 | 0.30 | 10.0 | 3×1016 |
Notes. Column (1): source, Col. (2-4): inner radius, temperature at inner radius and opacity estimated at UV wavelengths (200 nm) from SED modelling (Alonso-Hernández, in prep.), Col. (5): UV luminosity from the time-average GALEX NUV and FUV fluxes corrected from extinction with τUV, Col. (6): ISRF scaling factor at r = 5 × 1013 cm, as an indicative value for AGB stellar radii, according to the UV luminosity (see Sect. 6.1), Col. (7): X-ray luminosity from the X-ray fluxes (only for X-AGBs), Col. (8): stellar luminosity from Alonso-Hernández et al. (2024), Col. (9): α parameter as defined by Groenewegen (2017), Col. (10-13): mass-loss rate, temperature power-law index, expansion velocity and photodissociation radius from best-fit CO radiative transfer model. As discussed in Sect. 5, there are two CO radiative transfer models for T Dra: (a) assuming a standard CO radial abundance and (b) assuming a centrally depleted CO abundance in the innermost regions ofT Dra, likely caused by CO photodissociation driven by X-ray radiation (see Sect. 5).
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