Beta Piscis Austrini, Latinized from β Piscis Austrini, is catalogued as a binary star system in the southern constellation of Piscis Austrinus. It is visible to the naked eye with an apparent visual magnitude of +4.29. Based upon an annual parallax shift of 22.84 mas as seen from the Earth, the star is located 143 light years from the Sun. These coordinates are a source of X-ray emission with a luminosity of 8,850,000,000,000,000,000,000 W, which is most likely coming from a source other than the A-type stars. Oblak (1978) identified this as a triple star system, although subsequent sources list it as a binary. The magnitude 4.29 primary, component A, is a white-hued A-type main sequence star with a stellar classification of A1 V. It has an estimated 2.3 times the mass of the Sun and 2.1 times the Sun's radius. The star is radiating 37 times the solar luminosity from its photosphere at an effective temperature of 9,638 K. There is evidence for an infrared excess, indicating the presence of an orbiting debris disk. This has an estimated temperature of 188 K, indicating an orbital distance of 12 AU from the host star. The magnitude 7.8 secondary, component B, has a class of A2 V and lies at an angular separation of 30.3 arc seconds. Beta Piscis Austrini is moving through the Galaxy at a speed of 14.4 km/s relative to the Sun. Its projected Galactic orbit carries it between 7328 pc and 8697 pc from the center of the Galaxy. With Delta and Zeta it constituted Tien Kang ("heavenly rope") in China.