  Heartbeat stars (HBSs) are ideal astrophysical laboratories to study the
formation and evolution of binary stars in eccentric orbits and the internal
structural changes of their components under strong tidal action. We discover
23 new HBSs based on TESS photometric data. The orbital parameters, including
orbital period, eccentricity, orbital inclination, argument of periastron, and
epoch of periastron passage of these HBSs are derived by using a corrected
version of Kumar et al.'s model based on the Markov Chain Monte Carlo (MCMC)
method. The preliminary results show that these HBSs have orbital periods in
the range from 2.7 to 20 days and eccentricities in the range from 0.08 to
0.70. The eccentricity-period relation of these objects shows a positive
correlation between eccentricity and period, and also shows the existence of
orbital circularization. The Hertzsprung-Russell diagram shows that the HBSs
are not all located in a particular area. The distribution of the derived
parameters suggests a selection bias within the TESS survey towards massive
HBSs with shorter orbital periods, higher temperatures and luminosities. These
objects are a very useful source to study the structure and evolution of
eccentricity orbit binaries and to extend the TESS HBS catalog.
