Kavli Affiliate: Xian Chen
| First 5 Authors: Zeyuan Xuan, Smadar Naoz, Xian Chen, ,
| Summary:
Many gravitational wave (GW) sources in the LISA band are expected to have
non-negligible eccentricity. Furthermore, many of them can undergo acceleration
because they reside in the presence of a tertiary. Here we develop analytical
and numerical methods to quantify how the compact binary’s eccentricity
enhances the detection of its peculiar acceleration. We show that the general
relativistic precession pattern can disentangle the binary’s
acceleration-induced frequency shift from the chirp-mass-induced frequency
shift in GW template fitting, thus relaxing the signal-to-noise ratio
requirement for distinguishing the acceleration by a factor of $10sim100$.
Moreover, by adopting the GW templates of the accelerating eccentric compact
binaries, we can enhance the acceleration measurement accuracy by a factor of
$sim100$, compared to the zero-eccentricity case, and detect the source’s
acceleration even if it does not change during the observational time. For
example, a stellar-mass binary black hole (BBH) with moderate eccentricity in
the LISA band yields an error of the acceleration measurement
$sim10^{-7}mcdot s^{-2}$ for $rm{SNR}=20$ and observational time of $4$ yrs.
In this example, we can measure the BBHs’ peculiar acceleration even when it is
$sim1rm pc$ away from a $4times 10^{6}rm M_{odot}$ SMBH. Our results
highlight the importance of eccentricity to the LISA-band sources and show the
necessity of developing GW templates for accelerating eccentric compact
binaries.
| Search Query: ArXiv Query: search_query=au:”Xian Chen”&id_list=&start=0&max_results=10