Alpha Arietis is the star's Bayer designation. It also bears the Flamsteed designation of 13 Arietis. The traditional name Hamal derives from the Arabic رأس الحمل rās al-ħamal "head of the ram", in turn from the name for the constellation as a whole, Al Ħamal "the ram". In 2016, the International Astronomical Union organized a Working Group on Star Names to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016 included a table of the first two batches of names approved by the WGSN; which included Hamal for this star. In Chinese, 婁宿, meaning Bond , refers to an asterism consisting of Hamal, β Arietis and γ Arietis. Consequently, the Chinese name for Hamal itself is 婁宿三
Properties
The spectrum of this star matches a stellar classification of, with the luminosity class of III indicating that it is an evolved giant star that has exhausted the supply of hydrogen at its core and is now on the red giant branch. The 'Ca-1' portion of the classification indicates that it shows weaker than normal lines of calcium in its spectrum. Since 1943, the spectrum of this star has served as one of the stable anchor points by which other stars are classified. It is estimated to have about 50% more mass than the Sun, while interferometric measurements show it to be 15 times larger in diameter. Despite its enlarged girth, this star is still spinning with a slightly faster equatorial azimuthal velocity than the Sun, having a projected rotational velocity of 3.44 km s−1. Hamal is radiating about 91 times the Sun's luminosity from its outer envelope at an effective temperature of 4,480 K. This is cooler than the surface of the Sun, giving it the orange-hued glow of a K-type star. It is suspected to be slightly variable, with an amplitude of 0.06 magnitude. The abundance of elements other than hydrogen and helium, what astronomers term the star's metallicity, is only around half that in the Sun. In 2011, the likely presence of a planet in orbit around this star was reported by Byeong-Cheol Lee et al. It was detected using the radial velocity method, based upon measurements made between 2003 and 2010 at the Bohyunsan Optical Astronomy Observatory in Korea. The object has an orbital period of 381 days and an eccentricity of 0.25. The lower bound on this object's mass is about 1.8 times the mass of Jupiter. The estimated semi-major axis of the planet's orbit is 1.2 astronomical units, which would give it a periapsis distance of 0.9 AU and an apoapsis distance of 1.5 AU. By comparison, the star has a radius of 0.07 AU.
