Resolving the B[e] star Hen 3 1191 at 10 m with VLTI/MIDI

The models suggest that CH + is mostly located on the rim (10−13 AU) of the outer disc and at the disc surface (Fig.. CH + abundance structure in the HD 100546 disc with respect to

Astrometric and photometric star cata- logues derived from the ESA HIPPARCOS Space Astrometry Mission.

The photometry of the 236 238 objects detected in the reference images was grouped into the reference catalog (Table 3) 5 , which contains the object identifier, the right

pastoris has the ability to grow at different acceptable specific growth rates (µ) depending on the temperature of the medium (from 15ºC to 30ºC), lowering the

For samples grown at high enough substrate temperature under Cu-excess conditions, the co-evaporation process leads to the formation of a chalcopyrite phase with good

These rotating models are computed for initial masses of the host star between 1.5 and 2.5 M  , with initial surface angular velocities equal to 10 and 50% of the critical veloc-

Lacking a detailed theory for non-equilibrium polariton condensates, we test the validity of both atomic theories comparing the behavior of the temperature dependence

Therefore, the temperature is likely due to the distance from the star. Our model of the HD3003 disk gives an inner radius of 7.8 AU and a minimum grain size consistent with