(center)|thumb|left|upright Gamma Aquilae is a relatively young star with an age of about 270 million years. Nevertheless, it has reached a stage of its
evolution where it has consumed the hydrogen at its core and expanded into what is termed a
bright giant star, with a
stellar classification of K3 II. The star is now burning
helium into
carbon in its core. After it has finished generating energy through nuclear fusion, Gamma Aquilae will become a
white dwarf. The star has an estimated 3.5 times the
mass of the Sun and has expanded to 92 times the
Sun's radius. It is radiating over 2,100 times the luminosity of the Sun. An
effective temperature of in its outer envelope gives it the orange hue typical of K-type stars. A 1991 catalogue of
photometry reported that Gamma Aquilae showed some variation in its brightness, but this has not been confirmed. It is a known
source of X-ray emission, which is most likely being emitted by a hot
corona. Gamma Aquilae is located just 7' from the center of an
emission nebula, which has been first reported in 2023 by Stefan Ziegenbalg. The star is unlikely to be the ionization source of this nebula. ==Nomenclature==