Titlebook: Birth and Evolution of Massive Stars and Stellar Groups; Proceedings of a Sym Wilfried Boland,Hugo Woerden Conference proceedings 1985 D. R

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Rustproof

The Nearest Molecular Cloudsare correlated with the infrared “cirrus” found by IRAS. The mean distance to the clouds is about 100 pc; they are thus the nearest clouds to the Sun and are the small molecular-cloud component of the interstellar medium. The large internal velocity dispersions indicate that the clouds are not gravi

BRINK

季雨

Distribution and Motion of Young Nearby Stars as a Function of Agetial distribution of stars younger than 30·10. years along the inclined plane of Gould’s Belt shows a rather abrupt jump back to the galactic plane at distances coinciding with a discontinuity in the velocity gradients. Table 1 gives velocity parameters for different age groups, and the difficulty t

corn732

悠然

Near-Infrared Spectra of 11 T Tauri Starstriplet behaviour. The stars we have observed fall into three groups according to the values of the equivalent widths of the Ca IIλ 8498 line. Our results are in good agreement with recently proposed chromospheric models.

來就得意

The Turn-On Point of the Pleiades Clusterituated near to spectral type K2, corresponding to a mass of 0.75 to 0.8 M.. This is very close to the expected position based on the cluster age, as derived from the B and early A-star members of the Pleiades, and stellar contraction times. This also means, however, that the pre-main-sequence stars

危機

Two AOV Stars on the Zero-Age Main-Sequence in the Association Cha I HD 97048 and HD 97300 in the Cha I association. The MK spectral classification and apparent visual magnitude for these stars are: B9.5 Ve and V = 8.4; B9V and V = 9.0, respectively. Both objects are presumably ZAMS stars; although HD 97300 has no emission features, it does have many of the properti

安裝

Evolution of Massive Stars: Observational Evidenceith evolutionary models, the observations suggest a galactic gradient in the initial mass function of these stars. Differences in the massive stellar population between the Large and Small Magellanic Cloud are starting to appear. Understanding these differences will provide important insight into th

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