Exploring the sensitivity of gravitational wave detectors to neutron star physics

Kavli Affiliate: Rana Adhikari

| First 5 Authors: Denis Martynov, Haixing Miao, Huan Yang, Francisco Hernandez Vivanco, Eric Thrane

| Summary:

The physics of neutron stars can be studied with gravitational waves emitted
from coalescing binary systems. Tidal effects become significant during the
last few orbits and can be visible in the gravitational-wave spectrum above 500
Hz. After the merger, the neutron star remnant oscillates at frequencies above
1 kHz and can collapse into a black hole. Gravitational-wave detectors with a
sensitivity of ~10^{-24} strain/sqHz at 2-4 kHz can observe these oscillations
from a source which is ~100 Mpc away. The current observatories, such as LIGO
and Virgo, are limited by shot noise at high frequencies and have a sensitivity
of > 2 * 10^{-23} strain/sqHz at 3 kHz. In this paper, we propose an optical
configuration of gravitational-wave detectors which can be set up in present
facilities using the current interferometer topology. This scheme has a
potential to reach 7 * 10^{-25} strain/sqHz at 2.5 kHz without compromising the
detector sensitivity to black hole binaries. We argue that the proposed
instruments have a potential to detect similar amount of post-merger neutron
star oscillations as the next generation detectors, such as Cosmic Explorer and
Einstein Telescope. We also optimise the arm length of the future detectors for
neutron star physics and find that the optimal arm length is ~20 km. These
instruments have the potential to observe neutron star post-merger oscillations
at a rate of ~30 events per year with a signal-to-noise ratio of 5 or more.

| Search Query: ArXiv Query: search_query=au:”Rana Adhikari”&id_list=&start=0&max_results=10

Read More

Leave a Reply