59 Virginis

59 Virginis is known to astronomers at least from 1598, when it was catalogued by Tycho Brahe in his manuscript catalogue of 1004 fixed stars. Brahe designated it as "Parvula sequens vindemiatricem", which means in Latin "A tiny following Vindemiatrix" (that is Epsilon Virginis), and assigned it a visual magnitude 6^[12][13] (a modern value of its apparent magnitude (in band V) is 5.22). Five years later in 1603 Johann Bayer pictured it on constellation Virgo folio of his celestial atlas "Uranometria" and designated it with number 37, letter "e" (hence its Bayer designation e Virginis, or e Vir) and name "Alæ dextræ sequens", which means in Latin "Following right wing". Bayer also assigned it a visual magnitude 6.^[14]

In July 2013, Kuzuhara et al. announced the discovery of planet b orbiting this star. The discovery was made using the 8.2-meter Subaru Telescope of Mauna Kea Observatory, Hawaii.

The star is a relatively old Sun-like star with a spectral type of G0V^[4] and an effective temperature 6205±20 K (not much hotter than the Sun).^[9] It is twice as bright as the Sun in terms of luminosity.^[8] 59 Virginis appeared to be a subgiant star that has recently evolved off the main sequence stage, as its luminosity and temperature places it in the main-sequence turnoff in the Hertzsprung–Russell diagram.^[9][15], but was later found to be on the main sequence.^[3] It has a rotation period of 3.329 days.^[10] The star exhibits a Sun-like magnetic reversal cycle with the period about 12 years.^[8]

59 Virginis has an unusually high stellar rotation velocity and stellar activity, which led some astronomers to believe that it could be a young star several million years old.^[8] However, spectroscopy of the star's substellar companion, GJ 504 b, has suggested an age in the range of 3–6 Gyr.^[9] Various studies have estimated different ages for 59 Virginis: 0.16^+0.35
_−0.60 Gyr (2013),^[10] 4.5^+2.0
_−1.5 Gyr (2015),^[15] 2.5^+1.0
_−0.7 Gyr (2017),^[9] and 4.0±1.8 Gyr (2018).^[8] 2015 and 2017 studies led by Fuhrmann & Chini and D'Orazi et al. hypothesized that 59 Virginis's high activity and rotation may have been caused by the engulfment of a hot Jupiter.^[15][9][8] This was supported by, among other studies, a 2026 publication, which found that only a scenario of planet engulfment can explain the star's fast rotation, X-ray luminosity, and angular momentum.^[7]

In 2013, the discovery of a Jovian planet, b, by direct imaging of the system was announced.^[10] A later re-analysis suggested that it may actually be a brown dwarf.^[9]