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Gravitational redshift is a fundamental parameter that allows us to determinethe mass-to-radius ratio of compact stellar objects, such as black holes,neutron stars, and white dwarfs (WDs). In the X-ray spectra of the close binarysystem, RX J1712.6$-$2414, obtained from the Chandra High-Energy TransmissionGrating observation, we detected significant redshifts for characteristicX-rays emitted from hydrogen-like magnesium, silicon ($\Delta E/E_{\rm rest}\sim 7 \times 10^{-4}$), and sulfur ($\Delta E/E_{\rm rest} \sim 15 \times10^{-4}$) ions, which are over the instrumental absolute energy accuracy(${\Delta E/E_{\rm rest} \sim 3.3} \times 10^{-4}$). Considering some possiblefactors, such as Doppler shifts associated with the plasma flow, systemicvelocity, and optical depth, we concluded that the major contributor to theobserved redshift is the gravitational redshift of the WD harbored in thebinary system, which is the first gravitational redshift detection from amagnetic WD. Moreover, the gravitational redshift provides us with a new methodof the WD mass measurement by invoking the plasma-flow theory with strongmagnetic fields in close binaries. Regardless of large uncertainty, our newmethod estimated the WD mass to be $M_{\rm WD}> 0.9\,M_{\odot}$.

Gravitational Redshift Detection from the Magnetic White Dwarf Harbored in RX J1712.6-2414