Beta Cassiopeiae
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Beta Cassiopeiae (β Cassiopeiae, abbreviated Beta Cas or β Cas), officially named Caph Template:IPAc-en,<ref name=Kunitzsch>Template:Cite book</ref><ref name="IAU-CSN">{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> is a Delta Scuti variable star in the constellation of Cassiopeia. It is a giant star belonging to the spectral class F2. The white star of second magnitude (+2.28 mag, variable) has an absolute magnitude of +1.3 mag.
NomenclatureEdit
Beta Cassiopeiae is the star's Bayer designation. It also bore the traditional names Caph (from the Arabic word {{#invoke:Lang|lang}} Template:Transliteration, "palm" – i.e. reaching from the Pleiades), Chaph and Kaff, as well as al-Sanam al-Nakah "the Camel's Hump".<ref name=allen/> In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)<ref name="WGSN">{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016<ref name="WGSN1">{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> included a table of the first two batches of names approved by the WGSN; which included Caph for this star.
Originally, the pre-Islamic Arabic term al-Kaff al-Khadib "the stained hand" referred to the five stars comprising the 'W' of the constellation Cassiopeia, and depicted a hand stained with henna. The term was abbreviated and somehow came to signify β Cassiopeiae alone. The old "stained hand" was part of an asterism called Thuraya stretching from the Pleiades, which signified the "head" through Taurus and Perseus and into Cassiopeia, while the other "hand" was in Cetus.<ref name=kunitzsch_smart2006/>
In Chinese, {{#invoke:Lang|lang}} ({{#invoke:Lang|lang}}), in the Legs (Chinese constellation),<ref>Wang Liang was a famous charioteer during the Spring and Autumn period</ref> refers to an asterism consisting of β Cassiopeiae, κ Cassiopeiae, η Cassiopeiae, α Cassiopeiae and λ Cassiopeiae.<ref>Template:In lang 中國星座神話, written by 陳久金. Published by 台灣書房出版有限公司, 2005, Template:ISBN.</ref> Consequently, the Chinese name for β Cassiopeiae itself is {{#invoke:Lang|lang}} ({{#invoke:Lang|lang}}, Template:Langx.)<ref>Template:In lang 香港太空館 - 研究資源 - 亮星中英對照表 Template:Webarchive, Hong Kong Space Museum. Accessed on line November 23, 2010.</ref>
Together with Alpha Andromedae (Alpheratz) and Gamma Pegasi (Algenib), Beta Cassiopeiae was one of three bright stars known as the "Three Guides" marking the equinoctial colure.<ref name=allen/> This is an imaginary line running due south from Beta Cassiopeiae through Alpha Andromedae to the celestial equator, at a point where the Sun's path (the ecliptic) crosses it each autumn and spring equinox.<ref name=kaler2002/>
VisibilityEdit
With a mean apparent magnitude (V-band) of +2.28, it is one of the five stars which make up the 'W' of Cassiopeia, adjacent to the just brighter Schedar (Alpha Cassiopeiae). SN 1572, traditionally known as Tycho's Star, appeared about 5 degrees to the northwest of Caph in 1572.<ref name=allen/>
As a star in the deep northern hemisphere of the sky, Beta Cassiopeiae is prominent to viewers in the northern hemisphere but not often seen by those in the southern hemisphere. The constellation of Cassiopeia does not rise above the horizon to viewers in Tasmania, and only low if one were in Cairns.<ref name ="southern">Template:Cite book</ref>
SystemEdit
Beta Cassiopeiae is a yellow-white hued giant of stellar class F2 III.<ref name=gray/> More than three times the size of and 21 times brighter than the Sun, Caph has an absolute magnitude of +1.3. It was once an A-type star with about double the Sun's mass.<ref name=apj732_2/> It is now in the process of cooling and expanding to become a red giant. Its core is likely to have used up its hydrogen and is shrinking and heating, while its outer envelope of hydrogen is expanding and cooling. Stars do not spend much time in this state and are relatively uncommon. Caph's corona is unusually weak.<ref name=kaler2002/>
Beta Cassiopeiae is a variable star of the Delta Scuti type; in fact, the fourth brightest of such stars in the sky after Denebola, Vega and Altair.<ref name=apj619_2_1072/> It is a monoperiodic pulsator,<ref name=poretti2000/> with a brightness that ranges from magnitude +2.25 to +2.31 with a period of 2.5 hours.<ref name=kaler2002/> This type of variable includes subgiant or main-sequence stars of spectral classes F5–A0, having masses between 1.5–2.5 solar masses and nearing the end of their core hydrogen fusion lifetime.<ref name=poretti2000/> Their pulsations are related to the same helium instability strip on the Hertzsprung–Russell diagram as that of classical Cepheids. Delta Scuti stars are located at the intersection of the strip with the main sequence.<ref name=percy2007/>
This star is rotating at about 92% of its critical velocity, completing 1.12 rotations every day. This is giving the star an oblate spheroid shape with an equatorial bulge that is 24% larger than the polar radius. This shape is causing the polar region to have a higher temperature than the equator: the temperature difference is about 1,000 K. The star is being viewed nearly pole-on, the stellar axis is inclined about 20 degrees to the line of sight from the Earth.<ref name=apj732_2/>
Beta Cassiopeiae was once considered to be a spectroscopic binary with a faint companion in a 27-day orbit, but it is now thought to be a single star.<ref>Template:Cite journal</ref>