IR arcs around candidate weak-wind stars.
|Star||Sp. T||d||N H||n H||n||v ⋆||v ∞||Ṁ weak||Ṁ Vink||r obs||r s,weak||r s,Vink||r min|
|(kpc)||(cm-2)||(cm-3)||(cm-3)||(km s-1)||(km s-1)||(M⊙ yr-1)||(M⊙ yr-1)||(pc)||(pc)||(pc)||(pc)|
|σ Ori AB||O9.5V||0.3||...||...||10||50||1500||2.0e-10(9)||8.0e-8⋆⋆⋆||0.1||6e-3||0.13||0.10–0.40|
Notes. Column definitions: d is the distance; NH and nH are the total column density and average number density of atomic hydrogen along of sight; n is a directly measured local ISM number density (see below); Ṁweak and ṀVink are the weak-wind values as given in the corresponding references and the mass-loss as predicted by the theoretical recipe described in Vink et al. (2000); robs is the observed projected distance where the emission peaks in the WISE 22 μm images (assuming the listed d); rs,weak, rs,Vink are the calculated stand-off distance using Ṁweak, ṀVink and v∞; rmin is the predicted location of the dust wave in the model described in this work. rmin calculated through spectral type, density, velocity, and listed for 3000 Å and 300 Å grains, respectively.
HD 34078 is a fast runaway star which has recently encountered a molecular cloud or core not along the line of sight, therefore the average density along the line of sight is not representable in calculating the stand-off distance.
There is no column density of atomic hydrogen measured for HD 216898; the listed column density (and the derived average density) is for molecular hydrogen.
For consistency, we list Ṁ from Howarth & Prinja (1989), value used throughout this work. This value is consistent with the Vink et al. (2000) prediction, seen by comparison with the other O9.5V stars HD 34078 and HD 149757.
Reference. (1) Martins et al. (2005a); (2) Martins et al. (2012); (3) Boissé et al. (2009); (4) Brown & Bomans (2005); (5) Peri et al. (2012); (6) Gvaramadze et al. (2012b); (7) Gvaramadze et al. (2012a); (8) Marcolino et al. (2009); (9) Najarro et al. (2011). Distances and (average) column densities from Gudennavar et al. (2012) (for HD 216898 d was not listed and is calculated through the measured Hipparcos parallax from van Leeuwen 2007).
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