O-33: Serum Anti-M

I-28: Anti M

I-29: Menstrual Cycle Dependent Variation in Serum Levels of Anti-M

DIFFERENTIAL O AND Si ABUNDANCES IN M 33 EARLY B SUPERGIANTS

We present non-LTE analyses of four M33 early B-supergiant stars and five Galactic counterparts. This is the first time that B supergiants beyond the Magellanic Clouds are analyzed by means of detailed Non-LTE techniques. Among the M33 stars, new spectroscopic observations of B38 (ob21–108) are presented and the object is classified as B1Ia. The classification of another M33 star, B133, is chan...

O + + H 2 O „ + M ... \ H 5 O 2 + „ + M ...

8 C / O white dwarfs of very low mass : 0 . 33 - 0 . 5 M ⊙

The standard lower limit for the mass of white dwarfs (WDs) with a C/O core is roughly 0.5 M⊙. In the present work we investigated the possibility to form C/O WDs with mass as low as 0.33 M⊙. Both the pre-WD and the cooling evolution of such nonstandard models will be described.

Mo ð W Þ n O m ( n = 1 – 33 ; m = 2 – 75 ) clusters in the gas phase

H2MoO4 and H2WO4 upon direct laser desorption produce small clusters in the gas phase, extending up to 4500 and 7200 Da, respectively. The clustering patterns are quite similar for the two systems. The mass difference between successive peaks differ with increasing mass number as different kinds of structures become possible. A distinct planar to three-dimensional structural cross over is obser...