# Gamma Aquarii

Gamma Aquarii, or γ Aquarii, is a binary star system in the constellation of Aquarius. It has an apparent visual magnitude of 3.849, making it one of the brighter members of the constellation. Based upon parallax measurements taken during the Hipparcos mission, this star is located at a distance of approximately 164 light-years (50 parsecs) from the Sun. It is drifting closer to the Sun with a radial velocity of −16 km/s. In 1998, Olin J. Eggen included this star as a candidate member of the Hyades Supercluster.
The two components are designated Gamma Aquarii Aa, formally called Sadachbia /səˈdækbiə/, and Ab.

## Nomenclature

γ Aquarii, Latinised to Gamma Aquarii, is the system's Bayer designation. WDS J22217-0123 A is its designation in the Washington Double Star Catalog.
It bore the traditional name Sadachbia, from an Arabic expression سعد الأخبية (sa‘d al-’axbiyah), meaning "luck of the homes (tents)". In Hindi it is also called Satabhishaj (a hundred physicians); it is called Sadhayam in Tamil. In the catalogue of stars in the Calendarium of Al Achsasi Al Mouakket, this star was designated Aoul al Achbiya (أول ألأجبية - awwil al ahbiyah), which was translated into Latin as Prima Tabernaculorum, meaning the first of luck of the homes (tents). In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalogue and standardize proper names for stars. The WGSN approved the name Sadachbia for the component WDS J22217-0123 Aa on 21 August 2016, and it is now so included in the List of IAU-approved Star Names.
This star, along with Pi Aquarii (Seat), Zeta Aquarii (Sadaltager / Achr al Achbiya) and Eta Aquarii (Hydria), were al Aḣbiyah الأخبية "the Tent".
In Chinese, 墳墓 (Fén Mù), meaning Tomb, refers to an asterism consisting of Gamma Aquarii, Zeta Aquarii, Eta Aquarii and Pi Aquarii. Consequently, the Chinese name for Gamma Aquarii itself is 墳墓二 (Fén Mù èr, English: the Second Star of Tomb).

## Properties

In 1978 through 1984, H. A. McAlister listed this as a spectroscopic binary star system that is unresolved by speckle interferometry, and it is listed as such in the 1991 revision of the Bright Star Catalogue. In 2008, P. P. Eggleton and A. A. Tokovinin listed it as a single star in their catalogue of multiplicity. In 2024, the direct observation of a companion star to Gamma Aquarii was detected by interferometric observations.
The primary is an A-type main sequence star with a stellar classification of A0 V, around 2.7 times larger and more massive than the Sun. It was a candidate Lambda Boötis star, suggesting it may have accreted low-metallicity circumstellar gas some time in the past. But it has since been excluded. The star is spinning relatively rapidly with a projected rotational velocity of 80 km s$^{−1}$. This value gives a lower bound on the actual azimuthal velocity along the star's equator. The outer atmosphere of Gamma Aquarii is radiating energy at an effective temperature of 10,500 K, which is nearly double the temperature at the surface of the Sun. This heat is what gives Gamma Aquarii the white-hot glow of an A-type star.
The secondary component is a low-mass star detected via interferometry in 2024. It has around 0.56 times the mass and half the radius of the Sun. Its effective temperature of 3,900 K gives it the orange hue typical of late K-type stars. Located 1.9 astronomical units from each other, both stars take around a year to orbit the system's center of mass.