79 Ceti, also known as HD 16141, is a binary star system located 123 light-years from the Sun in the southern constellation of Cetus. It has an apparent visual magnitude of +6.83, which puts it below the normal limit for visibility with the average naked eye. The star is drifting closer to the Earth with a heliocentric radial velocity of −51 km/s.
Harlan (1974) assigned this star a stellar classification of G2V, matching an ordinary G-type main-sequence star that is undergoing core hydrogen fusion. However, Houk and Swift (1999) found a class of G8IV, which suggests it has exhausted the supply of hydrogen at its core and begun to evolve off the main sequence. Eventually the outer layers of the star will expand and cool and the star will become a red giant. Estimates of the star's age range from 6.0 to 9.4 billion years old. It has an estimated 1.06 times the mass of the Sun and 1.48 times the Sun's radius. The star is radiating twice luminosity of the Sun from its photosphere at an effective temperature of 5,806 K. The discrepancy was later found to be due to an additional red dwarf star in the system at a projected separation 220 AUs.
On March 29, 2000, a planet orbiting primary star was announced, it was discovered using the radial velocity method. This object has a minimum 0.26 times the mass of Jupiter and is orbiting its host star every 75.5 days.