Constraining the range of Yukawa gravity interaction from S2 star orbits III: improvement expectations for graviton mass bounds

Abstract

Recently, the LIGO-Virgo collaboration discovered gravitational waves and in their first publication on the subject the authors also presented a graviton mass constraint as m g < 1.2 × 10 −22 eV [1] (see also more details in a complimentary paper [2]). In our previous papers we considered constraints on Yukawa gravity parameters [3] and on graviton mass from analysis of the trajectory of S2 star near the Galactic Center [4]. In the paper we analyze a potential to reduce upper bounds for graviton mass with future observational data on trajectories of bright stars near the Galactic Center. Since gravitational potentials are different for these two cases, expressions for relativistic advance for general relativity and Yukawa potential are different functions on eccentricity and semimajor axis, it gives an opportunity to improve current estimates of graviton mass with future observational facilities. In our considerations of an improvement potential for a graviton mass estimate we adopt a conservative strategy and assume that trajectories of bright stars and their apocenter advance will be described with general relativity expressions and it gives opportunities to improve graviton mass constraints. In contrast with our previous studies, where we present current constraints on parameters of Yukawa gravity [3] and graviton mass [4] from observations of S2 star, in the paper we express expectations to improve current constraints for graviton mass, assuming the GR predictions about apocenter shifts will be confirmed with future observations. We concluded that if future observations of bright star orbits during around fifty years will confirm GR predictions about apocenter shifts of bright star orbits it give an opportunity to constrain a graviton mass at a level around 5 × 10 −23 eV or slightly better than current estimates obtained with LIGO observations.

Weak field limit and gravitational waves in f(T, B) teleparallel gravity

“…Being dynamically equivalent to f (R) gravity, it is possible to show that, in the post-Newtonian limit, a Yukawalike correction emerges in general [56]. This correction can be considered to put upper bound on the graviton mass as discussed in [57][58][59]. Being f (R) gravity not excluded by observations [15][16][17], this could be a pathway to test also f (T, B) gravity by a possible massive mode.…”

Constraints on tidal charge of the supermassive black hole at the Galactic Center with trajectories of bright stars

“…One could also check predictions of general relativity or alternative theories of gravity. For instance, one could evaluate constraints on parameters of theory, Yukawa gravity and graviton masses with trajectories of bright stars at the Galactic Center because in the case of alternative theories of gravity a weak gravitational field limit differs from Newtonian one, so trajectories of bright stars differ from elliptical ones and analyzing observational data with theoretical fits obtained in the framework of alternative theories of gravity one constrains parameters of such theories [37–42] (see, also discussion of observational ways to investigate opportunities to find possible deviations from general relativity with observations of bright stars at the Galactic Center [1, 43]).…”

Constraining Yukawa gravity from planetary motion in the solar system

“…where Λ is the range of interaction and δ is a new universal constant (for δ = 0, Φ (r) reduces to the Newtonian potential). Orbital precession per orbital period induced by this potential is given by Zakharov et al (2018):…”

“…In our previous work we performed such tests of different gravity theories in order to constrain their parameters at galactic Borka, Jovanović, Borka Jovanović, & Zakharov, 2012Capozziello et al, 2014;Dialektopoulos, Borka, Capozziello, Borka Jovanović, & Jovanović, 2019;Zakharov, Borka, Borka Jovanović, & Jovanović, 2014) and extragalactic scales Capozziello, Jovanović, Borka Jovanović, & Borka, 2017). Among these theories, a special attention has been given to the gravity theories with Yukawa-like correction term (Fischbach, Sudarsky, Szafer, Talmadge, & Aronson, 1986;Fischbach & *Corresponding author, e-mail: pjovanovic@aob.rs Talmadge, 1992;Hoyle et al, 2001;Iorio, 2007), and in our previous research we constrained parameters of Yukawa gravity at galactic scales (Borka et al, 2013;Zakharov et al, 2016Zakharov et al, , 2018.…”

“…On the other hand, the results of present high precision observational techniques and theories of planetary motions enable one to accurately study a variety of small effects in the Solar System, such as the presence of dark matter (Pitjeva & Pitjev, 2013) or possible deviations from Newtonian gravity (Adelberger, Gundlach, Heckel, Hoedl, & Schlamminger, 2009;Borka et al, 2013, Zakharov et al, 2016, 2018. Recently, discrepancies from the Newtonian potential in the form of Yukawa correction term have been tested at laboratory, geophysical and different astrophysical scales (Adelberger et al, 2009, Borka et al, 2013, Zakharov et al, 2016, 2018).…”