By Harry van der Laan (auth.), Wilfried Boland, Hugo van Woerden (eds.)
Read or Download Birth and Evolution of Massive Stars and Stellar Groups: Proceedings of a Symposium held in Dwingeloo, The Netherlands, 24–26 September 1984 PDF
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Additional resources for Birth and Evolution of Massive Stars and Stellar Groups: Proceedings of a Symposium held in Dwingeloo, The Netherlands, 24–26 September 1984
E. that seen by a distant observer in our own or another galaxy, is likely to be negligible. BLITZ: I disagree. 2 ~ pc- 2 , taking account of the incompleteness of our catalogue and using the same CO/H 2 conversion factor as for GMC's. The small high-latitude molecular clouds have 20-30% of the total molecular mass. There are a number of effects which may be misleading you in the log N - log S plots. BLAAUW: Is it correct to say that we do not know yet whether this population of small clouds also permeates the large molecular-cloud structures we saw from Thaddeus' plots of the Orion-Monoceros-Taurus clouds?
Might it look like the blue populous clusters in the Large Magellanic Cloud? You noted that the central density in the Trapezium Cluster is similar to that in globular clusters. HERBIG HERBIG: I presume that the star density in the Trapezium Cluster is high enough that the cluster will remain bound after the gas has been dissipated. After 10 6 years, then, all its low-mass members will have descended to the main sequence, the OB stars will have disappeared, and from 400 pc distance it might not be a very striking object.
Projected velocity in the center-anticenter direction as a function of ~rojected distance on the same direction for stars younger than 30 • 10 years. 35 DISTRIBUTION AND MOTION OF YOUNG NEARBY STARS 500 pc in the direction of the anticentre and 200 pc in the direction of the galactic centre. The total extension of this inclined plane in the direction of galactic rotation is of the order of 1 kpc. A least-squares solution for the orientation of the plane of Gould's Belt for stars younger than 20 10 6 years gives an inclination of 190 ±1° with a line of nodes directed towards £~930±3° The line of nodes thus lies almost exactly at right angles to the direction to the galactic centre.