Probing the vector charge of Sagittarius A* with pulsar timing

Abstract

Timing a pulsar orbiting around Sagittarius A* (Sgr A*) can provide us with a unique opportunity of testing gravity theories. We investigate the detectability of a vector charge carried by the Sgr A* black hole (BH) in the bumblebee gravity model with simulated future pulsar timing observations. The spacetime of a bumblebee BH introduces characteristic changes to the orbital dynamics of the pulsar and the light propagation of radio signals. Assuming a timing precision of 1 ms, our simulation shows that a 5-yr observation of a pulsar with an orbital period $P_b\sim 0.5\mathrm{yr}$ and an orbital eccentricity $e\sim 0.8$ can probe a vector charge-to-mass ratio as small as $Q/M\sim 10^{-3}$, which is much more stringent than the current constraint from the Event Horizon Telescope (EHT) observations, and comparable to the prospective constraint from extreme mass-ratio inspirals with the Laser Interferometer Space Antenna (LISA).

18 pages, 6 figures

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Cited by in corpus (6)

• Lorentz Symmetry Violation in Charged Black Hole Thermodynamics and Gravitational Lensing: Effects of the Kalb-Ramond Field
• Neutron stars in the bumblebee theory of gravity
• Measuring the Spin of the Galactic Center Supermassive Black Hole with Two Pulsars
• Probing a Lorentz-violating parameter from orbital precession of the S2 star around the galactic centre supermassive black hole
• Nethotrons: exploring the possibility of measuring relativistic spin precessions, from Earth's satellites to the Galactic Centre
• Testing No slip model with pulsar timing arrays: NANOGrav and IPTA