Optical study of F, G and K stars in the ROSAT All-Sky Survey

I analyze a sample of 107 southern stars of spectral types A to K, which were identified as the optical counterparts of X-ray sources detected by ROSAT during its All-Sky Survey. The study is conducted using optical observations, photometric as well as spectroscopic (high-resolution). Various parameters are determined for the sample objects, mainly spectral types and luminosity classes, absolute magnitudes, distances, radial velocities, projected rotational velocities, effective temperatures, Lithium abundances. I compare the X-ray parameters of my sample stars with those of a similar sample, detected by the Einstein Observatory during its Medium Sensitivity Survey (EMSS). I also look for correlations between the different stellar parameters determined for my sample, and compare those results to those obtained for the EMSS sample, and also to some results obtained from other, earlier studies

Engineering polymer informatics: Towards the computer-aided design of polymers

The computer-aided design of polymers is one of the holy grails of modern chemical informatics and of significant interest for a number of communities in polymer science. The paper outlines a vision for the in silico design of polymers and presents an information model for polymers based on modern semantic web technologies, thus laying the foundations for achieving the vision

Formation and Evolution of Planetary Systems: Upper Limits the Gas Mass in HD105

We report infrared spectroscopic observations of HD 105, a nearby ($\sim 40$ pc) and relatively young ($\sim 30$ Myr) G0 star with excess infrared continuum emission, which has been modeled as arising from an optically thin circumstellar dust disk with an inner hole of size $\gtrsim 13$ AU. We have used the high spectral resolution mode of the Infrared Spectrometer (IRS) on the Spitzer Space Telescope to search for gas emission lines from the disk. The observations reported here provide upper limits to the fluxes of H$_2$ S(0) 28$\mu$m, H$_2$ S(1) 17$\mu$m, H$_2$ S(2) 12 $\mu$m, [FeII] 26$\mu$m, [SiII] 35$\mu$m, and [SI] 25$\mu$m infrared emission lines. The H$_2$ line upper limits directly place constraints on the mass of warm molecular gas in the disk: $M({\rm H_2})< 4.6$, 3.8$\times 10^{-2}$, and $3.0\times 10^{-3}$ M$_J$ at $T= 50$, 100, and 200 K, respectively. We also compare the line flux upper limits to predictions from detailed thermal/chemical models of various gas distributions in the disk. These comparisons indicate that if the gas distribution has an inner hole with radius $r_{i,gas}$, the surface density at that inner radius is limited to values ranging from $\lesssim 3$ gm cm$^{-2}$ at $r_{i,gas}=0.5$ AU to 0.1 gm cm$^{-2}$ at $r_{i,gas}= 5-20$ AU. These values are considerably below the value for a minimum mass solar nebula, and suggest that less than 1 M$_J$ of gas (at any temperature) exists in the 1-40 AU planet-forming region. Therefore, it is unlikely that there is sufficient gas for gas giant planet formation to occur in HD 105 at this time.Comment: To appear in the Astrophysical Journa

Definitions of basic terms relating to polymer liquid crystals (IUPAC Recommendations 2001)

The document first gives definitions of basic terms related to liquid-crystalline and mesomorphic states of matter and then terms specific to the classification of liquid-crystal polymers. The terms have been restricted to those most commonly encountered in the structural description of the latter class of materials. The terms have been selected from the recently published comprehensive document "Definitions of basic terms relating to low-molar-mass and polymer liquid crystals" [Pure and Applied Chemistry 73 (5), 845-895 (2001)] and are intended to form a readily usable guide for the reader interested in the structural description of polymer liquid crystals. The more comprehensive document should be used for terminology associated with types of mesophases and the optical and physical characteristics of liquid-crystalline materials. The advice given by representatives of the International Liquid Crystal Society for the preparation of this document is gratefully acknowledged.Fil:Barón, M. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina