The GWs from the S-stars revolving around the SMBH at Sgr A*

TL;DR

This paper estimates gravitational waves from S-stars orbiting Sgr A* and finds their signals are below current detection sensitivity, suggesting future technological advances are needed for detection.

Contribution

It provides the first estimation of GWs from S-stars around Sgr A* using post-Newtonian methods, highlighting the challenges for future detection.

Findings

GW signals are below current PTA sensitivity.

Future technology may enable detection of these GWs.

Estimates are based on observed S-star orbits and eccentricity.

Abstract

A preliminary estimation of gravitational waves (GWs) from the extreme-mass-ratio-inspirals (EMRIs) system in the Galactic Centre (GC) is given for the 37 observed S-stars revolving around the supermassive black hole (SMBH) at Sagittarius (Sgr) A*. Within this century, the total strain of the gravitational waveform calculated from the post-Newtonian (PN) method with eccentricity is well below the current planned sensitivity of pulsar-timing-array (PTA). New technology might be required in order to extract GW signal from this EMRIs system for future PTA detections.