...[*]
Hubble Fellow.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
... wave[*]
For circular orbits this equation is identical to Eq. (5) of Evans et al. (1987). It is different by a factor of $\sqrt{8}$ from Eq. (20) of Press & Thorne (1972), who use a factor $\sqrt{2}$ larger definition of h and possibly confuse $\omega_{\rm g}$ in Eq. (3) with the orbital angular frequency. It differs by a factor 25/3 from Eq. (3.14) of Douglas & Braginsky (1979) because they confuse the orbital frequency in their Eq. (3.13), with the frequency of the wave (twice the orbital frequency) in their Eq. (3.4).
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
...1999)[*]
Note that Portegies Zwart & Yungelson (1999) consider only a subset of the (ns, wd) population, namely the systems that are eccentric and contain a white dwarf more massive than 1.1 ${M}_{\odot}$. For this subset they find a birth rate that is comparable to the birth rate of double neutron stars.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
Copyright ESO 2001