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Henny J.G.L.M. Lamers 《Astrophysics and Space Science》1998,260(1-2):63-80
The different methods for the study of stellar winds are discussed: (1) P Cygni profiles (2) atomic emission lines (3) infrared
and radio free-free emission (4) molecular emission lines (5) infrared radiation by dust. For each of these methods we describe
some characteristic observations and we discuss the way in which these data can be used to derive the mass loss rate and the
velocity distribution of the wind. We discuss these from the basic physical point of view in order to obtain an understanding
of the basic physical processes involved.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
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Henny J. G. L. M. Lamers 《Astrophysics and Space Science》2009,324(2-4):183-186
The analysis of the age distributions of star cluster samples of different galaxies has resulted in two very different empirical models for the dissolution of star clusters: the Baltimore model and the Utrecht model. I describe these two models and their differences. The Baltimore model implies that the dissolution of star clusters is mass independent and that about 90% of the clusters are destroyed each age dex, up to an age of about a Gyr, after which point mass-dependent dissolution from two-body relaxation becomes the dominant mechanism. In the Utrecht model, cluster dissolution occurs in three stages: (i) mass-independent infant mortality due to the expulsion of gas up to about 107 yr; (ii) a phase of slow dynamical evolution with strong evolutionary fading of the clusters lasting up to about a Gyr; and (iii) a phase dominated by mass-dependent dissolution, as predicted by dynamical models. I describe the cluster age distributions for mass-limited and magnitude-limited cluster samples for both models. I refrain from judging the correctness of these models. 相似文献
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Henny J. G. L. M. Lamers 《Astrophysics and Space Science》1994,221(1-2):489-490
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