2023/02/28 by Tanmay Kumar Poddar, Anish Ghoshal, Poddar, Tanmay Kumar +3 · 1 citation
Physics and Astronomy · #Cosmology and Gravitation Theories #Cosmology and Nongalactic Astrophysics (astro-ph.CO) #Dark Matter and Cosmic Phenomena #FOS: Physical sciences #General Relativity and Quantum Cosmology (gr-qc) #High Energy Physics - Phenomenology (hep-ph) #Pulsars and Gravitational Waves Research
paper · pdf · doi:10.48550/arxiv.2302.14513
openalex publication_date 2023/02/28 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We derive in detail the orbital period loss of a compact binary system in presence of a fifth force and radiation of ultralight particles for a general eccentric Keplerian orbit. We obtain constraints on fifth force strength α\lesssim 1.11× 10-3 from the orbital period decay of compact binary systems. We derive constraints on the gauge coupling of ultralight scalar (gS\lesssim 3.06× 10-20) and vector (gV\lesssim 2.29× 10-20) particles from orbital period loss and the constraints get stronger in presence of a fifth force (α=0.9). In addition, we also obtain constraints on the axion decay constant (7.94× 1010~\rmGeV\lesssim fa\lesssim 3.16× 1017~\rmGeV, α=0.9) if the orbital period decays due to the combined effects of axionic fifth force and axion radiation. We also achieve constraints on the strengths of the fifth force (α\lesssim 0.025) and radiation (β\lesssim 10-3) from GW170817. The constraints on new force parameters depend on the choice of the initial eccentricity which we include in our analysis (ε0=10-6, 0.1). We do the model independent estimate of the capture of dark matter mass fraction by a binary system. Lastly, we obtain constraints on fifth force strength due to Brans-Dicke mediated scalar between two compact stars in a binary system (ω_\rmBD>266) and from the Nordtvedt effect (ω_\rmBD>75858). The bound on Brans-Dicke coupling gets stronger if one includes the effect of eccentricity. Our constraints can be generalized to any alternative theories of gravity and will be within the reach of second and third generation gravitational wave detectors.