Table 1
Best-fit parameters from DUSTY models.
| Source | T* | Tinn | n | τ550 | log(Y) | L | Rinn | Rout | Mdust | Ṁdust | δ |
|---|---|---|---|---|---|---|---|---|---|---|---|
| (K) | (K) | (L⊙) | (1013cm) | (1016cm) | (10−6 M⊙) | (10−10 M⊙ yr−1) | |||||
| EY Hya | ![]() |
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5200±800 | 7.9 | 50 | 29 | 19 | 310 |
| FH Vir | ![]() |
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2100±300 | 3.3 | 83 | 13 | – | – |
| IN Hya | ![]() |
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1700±200 | 3.3 | 33 | 2.4 | – | – |
| R LMi | ![]() |
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3300±500 | 4.8 | 190 | 48 | 5.2 | 810 |
| R UMa | ![]() |
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5000±900 | 26 | 260 | 30 | 1.7 | 760 |
| RR Eri | ![]() |
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4700±900 | 20 | 20 | 3.2 | 6.0 | 680 |
| RT Cnc | ![]() |
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2100±300 | 4.2 | 42 | 5.5 | 3.0 | 230 |
| RU Her* | <2700 | ![]() |
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20 000±5000 | 50 | 130 | 72 | 13 | 1230 |
| RW Boo | ![]() |
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2200±300 | 6.6 | 66 | 3.5 | 2.1 | 1670 |
| RZ UMa | ![]() |
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5100±1000 | 7.4 | 19 | 21 | 17 | 70 |
| ST UMa | ![]() |
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2900±500 | 7.5 | 30 | 4.0 | – | – |
| SV Peg | ![]() |
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10 000±2000 | 21 | 21 | 41 | 45 | 330 |
| T Dra | ![]() |
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13 000±3000 | 19 | 1200 | 1200 | 37 | 780 |
| TU And | ![]() |
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7500±1700 | 5.9 | 150 | 127 | – | – |
| UY Leo | ![]() |
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2000±300 | 4.0 | 64 | 23 | – | – |
| V Eri | ![]() |
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5100±1000 | 8.1 | 13 | 26 | 65 | 90 |
| VY UMa | ![]() |
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4700±900 | 6.1 | 24 | 0.15 | 0.050 | 40 000 |
| VY UMa** | – | – | – | – | – | – | – | – | 5.5 | – | – |
| W Peg | ![]() |
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5300±1000 | 15 | 150 | 26 | 4.1 | 1100 |
| Y CrB | ![]() |
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4500±800 | 6.4 | 64 | 7.5 | 8.1 | 160 |
| Y Gem | ![]() |
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8500±1800 | 9.2 | 5.8 | 1.0 | – | – |
| Z Cnc | ![]() |
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4200±600 | 12 | 1.2 | 1.1 | 11 | 55 |
Notes. Column 1: name of the source; Col. 2: stellar effective temperature; Col. 3: dust shell inner radius temperature; Col. 4: dust shell density power-law index; Col. 5: dust shell radial optical depth at 550 nm (from Rinn to Rout); Col. 6: logarithm of the dust shell outer-to-inner radii ratio; Col. 7: bolometric luminosity; Col. 8: dust shell inner radius; Col. 9: dust shell outer radius; Col. 10: dust shell mass; Col. 11: dust mas-loss rate; and Col. 12: gas-to-dust ratio. *In the case of RU Her, the sensitivity study indicates T* <2700K, although we noted that 2600 K fits the SED correctly (see Fig. 1). **In the case of VY UMa, the dust mass estimated for the detached shell is included separately.
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