Predicting the detectability of gravitational waves from PSR J0737–3039 with the laser interferometer space antenna: A quadrupole approximation approach

Gravitational waves (GWs) are an important component of gravitational physics. In a binary system, it is emitted through orbital energy loss. In this paper, we explore the Laser Interferometer Space Antenna (LISA)’s detectability of gravitational waves from PSR J0737–3039, the first known binary pulsar system. The system is located around 1150 parsecs from Earth, with an orbital period of ∼2.45 h and an inclination angle of 87°, making it an ideal candidate for testing gravitational physics. We approximated the GW frequency of the system to be ∼2.26 × 10⁻⁴ Hz using rules of orbital frequency. We used the quadrupole formula, a part of the multipole expansion, to estimate that the calculated GW strains (h_✕ ∼ 4.8702×10⁻²³ and h₊ ∼ 4.6656×10⁻²²). The strain magnitudes fall below the detector noise curve of LISA. We offer possible explanations for this, including arm length and acceleration noise, while proposing methods to enhance LISA’s sensitivity. These methods include the Noise2Noise algorithm and possibility of the installation of resonant detectors.