Gravitational Waves in Physics and Astrophysics: An artisan’s guide by M Coleman Miller and Nicolás Yunes

Author:M Coleman Miller and Nicolás Yunes
Language: eng
Format: mobi
ISBN: 9780750330510
Publisher: IOP Publishing
Published: 2021-12-17T00:00:00+00:00

5.2.3.3 Double White Dwarf Binaries

As we have mentioned before, the foreground noise produced by double white dwarf binaries in our Galaxy is expected to limit the effective sensitivity of LISA up to a few millihertz. We can motivate that in the following way. It is estimated that there are a few tens of millions of double white dwarf systems in our Galaxy that will merge in the year age of the universe, which suggests a merger rate of one per few hundred years. It is also estimated that the rate of white dwarf supernovae is one per few hundred years, so if most of these involve two white dwarfs merging rather than a white dwarf accreting matter from a nondegenerate companion, then the two rates are consistent. Let’s take as our fiducial rate 0.003 yr−1. We will also assume that the typical chirp mass is about (if we take two white dwarfs each of mass , which is average, the chirp mass is ). Finally, given that LISA’s lifetime is expected to be a few years, we will assume that the duration of the observation is , or and thus that the frequency resolution is about Hz.

Using Equation (5.5), then we have an expected number of sources in our Galaxy per Hz frequency bin of

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