In the catalogue of stars in the Calendarium of Al Achsasi Al Mouakket, this star was designated Laouiyet al Aoua, which was translated into Latin as Angulus Latratoris, meaning 'the angle of the barker'.[17] This star, along with Beta Virginis (Zavijava), Eta Virginis (Zaniah), Delta Virginis (Minelauva) and Epsilon Virginis (Vindemiatrix), were Al ʽAwwāʼ, the Barker.[14]
In Chinese, 太微左垣 (Tài Wēi Zuǒ Yuán), meaning Left Wall of Supreme Palace Enclosure, refers to an asterism consisting of Gamma Virginis, Eta Virginis, Delta Virginis, Epsilon Virginis and Alpha Comae Berenices.[18] Consequently, the Chinese name for Gamma Virginis itself is 太微左垣二 (Tài Wēi Zuǒ Yuán èr, English: the Second Star of Left Wall of Supreme Palace Enclosure.),[19] representing 東上相 (Dōngshǎngxiāng), meaning The First Eastern Minister.[20] 東上相 (Dōngshǎngxiāng), westernized into Shang Seang by R. H. Allen and the meaning is "the High Minister of State".[14]
Properties
Gamma Virginis is a binary star, consisting of two stars of nearly equal apparent magnitudes 3.65 and 3.56, and of spectral type F0V.[2] With an orbital period of 168.93 years,[5][6] it was an easy object for amateur astronomers until the beginning of the 1990s, but in 2011 the smaller apparent distance between the stars requires a larger telescope or special techniques such as speckle interferometry,[5][6]adaptive optics[21] or optical interferometry[22] to resolve the individual components. The last time they were at periapsis was in 1836. The distance became wide enough in 2020 to view with a small telescope. The star system has a combined apparent magnitude of 2.9. The system is 39 light-years away from the Sun.
Gamma Virginis is 2.8 degrees north of the ecliptic, so it can be occulted by the Moon and (rarely) by planets. In June 2011 Saturn passed a quarter of a degree south of Porrima.
Based upon X-ray emissions—an indicator of the strength of the stellar magnetic field—this system has an estimated age of 1.14 billion years.[23]
Changes of distance and position angle
This table shows the apparent distance between the two stars and their relative position angle: the first three columns show data predicted from an orbit calculated in 1937, the next two columns show in 2006,[24] the next three columns show observations reported by the Hanwell Community Observatory.[25]
^ abWhite, Jacob Aaron; Tapia-Vázquez, F.; Hughes, A. G.; Moór, A.; Matthews, B.; Wilner, D.; Aufdenberg, J.; Hughes, A. M.; De la Luz, V.; Boley, A. C. (2020-05-01), "The MESAS Project: ALMA Observations of the F-type Stars γ Lep, γ Vir A, and γ Vir B", The Astrophysical Journal, 894 (1): 76, arXiv:2003.12284, Bibcode:2020ApJ...894...76W, doi:10.3847/1538-4357/ab8467, ISSN0004-637X
^Kunitzsch, Paul; Smart, Tim (2006), A Dictionary of Modern star Names: A Short Guide to 254 Star Names and Their Derivations (2nd rev. ed.), Cambridge, Massachusetts: Sky Pub, ISBN978-1-931559-44-7
^Riddle, Reed L.; Tokovinin, Andrei; Mason, Brian D.; Hartkopf, William I.; Roberts, Lewis C. Jr.; Baranec, Christoph; Law, Nicholas M.; Bui, Khanh; Burse, Mahesh P. (2015-01-01), "A Survey of the High Order Multiplicity of Nearby Solar-type Binary Stars with Robo-AO", The Astrophysical Journal, 799 (1): 4, arXiv:1411.0682, Bibcode:2015ApJ...799....4R, doi:10.1088/0004-637X/799/1/4, ISSN0004-637X, S2CID5642378
^Hutter, D. J.; Zavala, R. T.; Tycner, C.; Benson, J. A.; Hummel, C. A.; Sanborn, J.; Franz, O. G.; Johnston, K. J. (2016-11-01), "Surveying the Bright Stars by Optical Interferometry. I. A Search for Multiplicity among Stars of Spectral Types F-K", The Astrophysical Journal Supplement Series, 227 (1): 4, arXiv:1609.05254, Bibcode:2016ApJS..227....4H, doi:10.3847/0067-0049/227/1/4, ISSN0067-0049, S2CID118803592
