Results of infrared visibility modeling.
|Star||Band||Spectral type||Ø⋆||Ø1900K||Ø||Øenv||T env||χ 2|
|U Ari||7.80−9.30 μm||M5.5 III||5.00||15.08||62.3||3300a||15.75||2800||26.98|
|W Cnc||7.80−9.30 μm||M7 III||3.90||10.29||43.4||3087a||13.00||1600||5.63|
|RX Tau||7.80−9.30 μm||M7e||5.38||14.20||69.4||3087a||13.00||1900||57.34|
|V Mon||7.80−9.30 μm||M6e||3.89||11.33||62.1||3243a||10.75||1800||0.08|
Notes. Ø⋆ is the estimated photospheric diameter with an accuracy better than 10% (except for S Ser, for which it is about 20%). Ø1900K is twice the estimated condensation radius of Al2O3. Ø is the estimated smallest possible diameter of the silicate dust shell. is thestellar effective temperature estimated from photometric measurements, and Ø⋆. Øenv and Tenv are the diameter and temperature of the envelope above the photosphere in the simple star+envelope model. Uncertaintiesof these parameters were not analyzed in this paper, the values are therefore indicative. The last column gives the reduced χ2 of the fit. No value is given for S Ser because only one baseline was measured and there are fewer data points than model parameters.
Interpolated from Perrin et al. (1998);
interpolated from Ridgway et al. (1980).
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