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Extra resources for Astrophysics. Part B: Radio Telescopes
Example text
Such systems can be expected to have large mass functions, and they do indeed give four of the eleven largest values in the figure. It is quite likely that more SBs, particularly at the upper margin of f , are in fact triple, but have not been recognised as such. 10 is a similar plot to Fig. 6 – sampled in a way somewhat similar to the way in which real stars are sampled. Random inclinations were also included. We believe that the best way to assess the reliability of a model of the distribution of Q, which can be expected to depend on P and M1 , is to compare a theoretical figure like Fig.
Several of the shorter-period systems, say with P < ∼ 10 days, will be resident in wider triples. The surface density of massive stars is, of course, to be modified according to their short lifetimes (Chapter 2). Stars above a mass ∼5 M only live for < ∼100 megayears, so that their abundance is reduced to ∼1% of what is predicted above. 7 Conclusion 29 white dwarfs, neutron stars or black holes, but they may nevertheless have companions of initially lower mass that are still normal stars. We should not suppose that all parts of the Galaxy, including its collection of satellite globular clusters, would conform to a single distribution.
Rough observational limits are indicated by straight lines, as in Fig. 9a. Those of too long a period or too small a velocity amplitude to be readily measurable are indicated by a cross. The stars might be late B/A/F dwarfs, or, if evolved, G/K giants as in Fig. 9a. Unlike in Fig. 9a, no triples were included. cases only the G/K giant has had its radial velocity curve measured. The fact that ∗2 is seen at all suggests that it is only moderately less massive than ∗1. 2–4 M . 5 We believe that a slight trend can be seen in Fig.
