Prospects of constraining <math display="inline"><mi>f</mi><mo stretchy="false">(</mo><mi>T</mi><mo stretchy="false">)</mo></math> gravity with the third-generation gravitational-wave detectors

Mergers of binary compact objects, accompanied with electromagnetic (EM) counterparts, offer excellent opportunities to explore varied cosmological models, since gravitational waves (GWs) and EM counterparts always carry the information of luminosity distance and redshift, respectively.

f (T)

gravity, which alters the background evolution and provides a friction term in the propagation of GWs, can be tested by comparing the modified GW luminosity distance with the EM luminosity distance. Considering the third-generation gravitational-wave detectors, Einstein Telescope and two cosmic explorers, we simulate a series of GW events of binary neutron stars and neutron-star–black-hole binaries with EM counterparts. These simulations can be used to constrain

f (T)

gravity [especially the power-law model

f (T) = T + α (- T)^{β}

in this work] and other cosmological parameters, such as

β

and the Hubble constant. In addition, combining simulations with current observations of type Ia supernovae and baryon acoustic oscillations, we obtain tighter limitations for

f (T)

gravity. We find that the estimated precision significantly improved when all three datasets are combined (

Δ β \sim 0.03

), compared to analyzing the current observations alone (

Δ β \sim 0.3

). Simultaneously, the uncertainty of the Hubble constant can be reduced to approximately 1%.

Note:

12 pages, 6 figures, 3 tables

family: 3
binary: compact
neutron star: binary
binary: coalescence
baryon: oscillation: acoustic
gravitation: f(T)
gravitational radiation detector
Hubble constant
luminosity: redshift
radiation: electromagnetic

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Figures(7)

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