The distance to Maia has been measured by the
Gaia spacecraft using the
annual parallax method. In
Gaia Data Release 2, the parallax is given as , corresponding to a distance of . The 2007 new
Hipparcos reduction gives a statistically more accurate parallax of , indicating a distance of . while
VLBI measurements of multiple members give a distance of . Maia's
visual magnitude is 3.87, requiring darker skies to be seen. Its
bolometric luminosity is 501 times that of the sun, mostly in the
ultraviolet, thus suggesting a radius of 3.6 times that of the Sun and a mass of 3.8 solar masses. for Maia, adapted from White
et al. (2017) Maia was thought to be a
variable star by astronomer
Otto Struve. He proposed a class of stars known as Maia variables, which included
Gamma Ursae Minoris. Examination of the
Hipparcos data for Maia and some others in the class found no evidence of variability. On the other hand, White
et al. found low amplitude, but unambiguous, variability in Maia's brightness as seen by
Kepler/K2, with a period of 10.3 days, which they attribute to the rotation of a
starspot. It is now thought Maia is not a Maia variable, but a
rotating variable. It is the only member of the
New General Catalogue discovered photographically. ==Mythology==