Periastron precession effect of f-mode dynamical tides on gravitational waves from eccentric double white dwarfs
arxiv(2022)
摘要
The dynamical tide can play an important role in the orbital motion of close
eccentric double white dwarf binaries. As the launching of the space-based
gravitational-wave detector, the Laser Interferometer Space Antenna (LISA), is
just around the corner, detection of gravitational wave signals from such
systems is anticipated. In this paper, we discuss the influence of the
dynamical tide on eccentric orbits, focusing on the effect on orbital
precession. We show that in orbits with a high eccentricity, resonance can
cause a large precession when a harmonic of the orbital frequency matches the
natural frequencies of the normal modes of the star. In contrast to the case
with circular orbits, each mode can encounter multiple resonances with
different harmonics and these resonant regions can cover about 10
frequency space for orbits with close separations. In this case, the tidal
precession effect is distinct from the other contributions and can be
identified with LISA if the signal-to-noise ratio is high enough. However,
within the highly eccentric-small separation region, the dynamical tide causes
chaotic motion and the gravitational wave signal becomes unpredictable. Even
not at resonance, the dynamical tide can contribute up to 20
for orbits close to Roche-lobe filling separation with low eccentricities and
LISA can resolve these off-resonant dynamical tide effects within the low
eccentricity-small orbital separation region of the parameter space. For lower
mass systems, the dynamical tide effect can degenerate with the uncertainties
of the eccentricity, making it unmeasurable from the precession rate alone. For
higher mass systems, the radiation reaction effect becomes significant enough
to constrain the eccentricity, allowing the measurement of the dynamical tide.
更多查看译文
AI 理解论文
溯源树
样例
生成溯源树,研究论文发展脉络
Chat Paper
正在生成论文摘要