Editing Beta Arietis (section)

==Properties==
Beta Arietis has an [[Apparent magnitude|apparent visual magnitude]] of 2.65. Based on dynamical [[parallax]] measurements, it is located at a distance of {{Convert|58.4|ly|pc|abbr=off|lk=on}} from Earth.<ref name=sb2/> This is a [[spectroscopic binary]] star system consisting of a pair of stars orbiting around each other with a separation that can not currently be resolved with a conventional telescope. However, the pair have been resolved using the [[Mark III Stellar Interferometer]] at the [[Mount Wilson Observatory]]. This allows the [[orbital elements]] to be computed, as well as the individual masses of the two stars. The stars complete their highly [[Elliptic orbit|elliptical orbit]] every 107 days.<ref name=apj356_641/>

The primary star has a [[stellar classification]] of A3&nbsp;V,<ref name=sb2/> which means it is an [[A-type main-sequence star]] that is generating energy through the [[thermonuclear fusion]] of hydrogen in its core region. The [[NStars]] project gives the star a spectral type of kA4&nbsp;hA5&nbsp;mA5&nbsp;Va under the revised [[MK spectral classification]] system.<ref name=aj126_4_2048/> The secondary star is a [[G-type main-sequence star]], with a [[stellar classification]] of G2V.<ref name=sb2/> It is about four magnitudes fainter than the primary; hence the energy output from the system is dominated by the primary star.<ref name=apj356_641/> In a few million years, as the primary evolves toward a [[red giant]], significant amounts of mass transfer to the secondary component is expected.<ref name=mnras384_1_173/>

The primary has been classified as a rapid rotator, with a [[stellar rotation|projected rotational velocity]] of 73&nbsp;km/s providing a lower bound on the [[azimuth]]al rotational velocity along the equator.<ref name=aaa463_2_671/> It may also be a mildly [[Am star]], which is a class of stars that show a peculiar spectrum with strong [[Spectral line|absorption lines]] from various elements and deficiencies in others. In β Arietis, these absorption lines are broadened because of the [[Doppler effect]] from the rotation, making analysis of the abundance patterns difficult.<ref name=aaass27_35/>

This system has been examined with the [[Spitzer Space Telescope]] for the presence of an [[infrared excess|excess emission of infrared]], which would indicate a disk of dust. However, no significant excess was detected.<ref name=aj126_4_2048/>