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Antevorta
Antevorta
Antevorta
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In ancient Roman religion, Antevorta was a goddess of the future, also known as Porrima or Prorsa (a contracted form of Proversa). She and her sister Postverta (or Postvorta) were described as companions or siblings of the goddess Carmenta, sometimes referred to as "the Carmentae".[1] They may have originally been two aspects of Carmenta, namely those of her knowledge of the future and the past (compare the two-faced Janus).

Antevorta and Postvorta had two altars in Rome and were invoked by pregnant women as protectors against the dangers of childbirth.[2] Antevorta was said to be present at the birth when the baby was born head-first; Postverta, when the feet of the baby came first.

Star name

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Antevorta is an alternative star name for Gamma Virginis, officially named Porrima.

See also

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References

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Antevorta

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Antevorta, also known as Porrima, is the traditional name of the system Gamma Virginis (γ Virginis) in the constellation of Virgo. It consists of two nearly identical Sun-like stars orbiting each other with a period of about 169 years, at an average separation of 38 light-years from the Solar System. The name Antevorta derives from , where Antevorta (or Prorsa) was a of and the future, one of the and sister to Postvorta. The system is visible to the as a magnitude 2.74 star, located near the , making it observable from both hemispheres.

Nomenclature

Bayer designation

The system, introduced by in his 1603 star atlas Uranometria, assigns Greek letters (starting with alpha for the brightest) followed by the Latin genitive of the constellation name to identify stars in order of approximate decreasing brightness within each constellation. Porrima holds the Bayer designation γ Virginis (Gamma Virginis), marking it as the star assigned the Greek letter gamma in the constellation Virgo; although Bayer's ordering was not always strictly by brightness, γ Virginis ranks as the second-brightest star in Virgo after α Virginis (). It also carries the Flamsteed designation 29 Virginis, introduced by in his 1725 Historia Coelestis Britannica as a numerical catalog based on within constellations, providing an alternative identifier for precise reference. These designations enable accurate location and cross-referencing of Porrima in major astronomical databases, such as the Catalogue (where it is HIP 61941) and the Gaia Data Release 3 (Gaia DR3 3683687763520080384), facilitating astrometric measurements and observational studies.

Traditional names

The primary traditional name for the star system is Porrima, derived from the Roman goddess of who foretold the future. This goddess, also known as Antevorta—meaning "facing forward" in reference to her prophetic gaze toward future events—was one of the , a group of four prophetic water nymphs associated with , fountains, and in . Her sister deity, Postvorta (or Postverta), represented the past by "facing backward," and both were companions to the goddess , embodying complementary aspects of time and foresight. Historically, the star has borne other cultural designations, including the Arabic name Laouiyet al Aoua, meaning "the angle of the barker," as recorded by the 17th-century Egyptian Al Achsasi al Mouakket in his star catalog; this term alluded to the star's position in an asterism resembling a barking figure. In Chinese astronomy, it was designated 太微左垣二 (Tài Wēi Zuǒ Yuán èr), translating to "the Second Star of the Left Wall" within the Supreme Palace Enclosure, a key asterism in the representing imperial guards. The (IAU) officially adopted Porrima as the proper name for the star ( γ Virginis) on July 20, 2016, through its on Star Names, following proposals from the 2015 contest that emphasized cultural and mythological significance. The name applies to the as a whole.

Location and visibility

Position in the sky

Antevorta, known astronomically as γ Virginis or Porrima, occupies a position in the constellation Virgo, situated near the border with Libra and about 3.7° northwest of the prominent star (α Virginis). This placement situates it within the northern portion of Virgo, a large zodiacal constellation spanning 657 square degrees. The star's equatorial coordinates at epoch J2000.0 are right ascension 12ʰ 41ᵐ 39.628ʲ and declination −01° 26′ 57.85″, positioning it just south of the celestial equator. In galactic coordinates, Antevorta lies at longitude l = 297.83° and latitude b = 61.33°, placing it well above the galactic plane in the direction of the constellation. Relative to the ecliptic, it is located 2.8° north, a proximity that occasionally allows for occultations by the Moon or, more rarely, planets such as Venus or Mercury. Based on astrometric data from the mission Data Release 3 (2022), Antevorta is at a distance of 39.2 ± 0.2 light-years (12.02 ± 0.07 parsecs) from , corresponding to a of 83.19 ± 0.51 mas. The star demonstrates measurable , with annual components of approximately −0.605 arcseconds in and +0.086 arcseconds in , reflecting its gradual shift across the sky over time.

Observational details

Antevorta, known scientifically as γ Virginis, exhibits a combined apparent visual magnitude of 2.74, allowing it to be observed with the in moderately dark skies without optical aid. The system's two components, designated γ¹ Vir and γ² Vir, possess individual magnitudes of 3.65 and 3.56, respectively, contributing to the overall while appearing nearly equal in to the unaided eye. This non-variable nature ensures stable illumination, making Antevorta a reliable target for consistent observational tracking over time. The binary pair is currently resolvable using small telescopes, with an angular separation of about 3.5 arcseconds as of 2025, a configuration that has progressively widened since the most recent periapsis passage in 1836. With an of approximately 169 years, the components continue to separate, enhancing accessibility for visual observation in modest equipment. Antevorta is visible from both Northern and Southern hemispheres due to its equatorial position, reaching during spring evenings for northern observers and proving optimal for detailed viewing in and May when it transits high in the sky. Its proximity to the facilitates occasional lunar occultations, with historical events documented and future passages anticipated, though no recent occultations by planets have been recorded.

Stellar properties

Physical characteristics

The Antevorta system consists of two nearly identical main-sequence stars, both classified as spectral type F0 V, characteristic of hot, white stars that fuse hydrogen in their cores. This classification reflects their position on the main sequence, where they exhibit stable luminosity over billions of years. Each component has a mass of approximately 1.4 ± 0.05 solar masses (M⊙), determined through orbital analysis combined with parallax measurements. Their radii are estimated at about 1.45 solar radii (R⊙) per star, contributing to their overall physical similarity. The surface temperatures of both stars are around 6,900 K, imparting a white appearance to the system when observed visually. This temperature range aligns with their F-type classification and supports luminosities of roughly 4.4 times the Sun's luminosity (L⊙) for each component. The system is estimated to be approximately 1.46 billion years old, derived from isochrone fitting and gyrochronology methods applied to the stars' rotational and evolutionary properties. Metallicity is slightly subsolar, with [Fe/H] ≈ -0.08 and no significant abundance peculiarities noted.

Binary system

Antevorta is a visual comprising two nearly identical F0 V main-sequence that their common . The components, designated Antevorta A and Antevorta B, exhibit very similar spectral types and luminosities, with each having a mass of approximately 1.4 solar masses. This close resemblance in physical properties makes Antevorta a valuable system for studying the dynamics of twin-like in wide binaries. The of the system is 169.104 ± 0.011 years, during which the complete one full revolution around each other. The is highly elliptical, characterized by an eccentricity of 0.8815 ± 0.00018, which results in significant variations in separation over the cycle. The semi-major axis spans 3.639 ± 0.008 arcseconds, equivalent to a physical distance of about 42.5 AU given the system's distance of 38.1 light-years. The relative to the is 149.46° ± 0.16°, rendering the system nearly edge-on and theoretically capable of producing eclipses, though none have been detected owing to the orbital geometry at conjunctions. The most recent periastron was in 2005. As of 2025, the stellar separation is approximately 3.47 arcseconds and increasing along their elliptical path. The next closest approach is anticipated around 2174, when the components will again draw nearer before separating once more. These long-term orbital variations highlight the stability of the system over human timescales while underscoring the challenges in resolving such wide binaries with ground-based telescopes. Looking to the future, both stars in Antevorta are expected to exhaust their core reserves and ascend the as subgiants in approximately 2–3 billion years, based on models of intermediate-mass . This post-main-sequence expansion could influence the binary orbit through asymmetric mass loss or enhanced tidal forces, potentially leading to orbital widening or circularization, though the exact outcome depends on the stars' synchronized .

Historical observations

Name origin and early records

The name Antevorta for the star γ Virginis derives from the Roman goddess Antevorta, also known as Porrima, one of the or Carmentes—ancient water nymphs associated with and ; Antevorta specifically foretold the future, while her Postverta predicted the past. This mythological connection reflects the star's placement in the constellation Virgo, often linked to themes of foresight and divine order in classical lore. The star first appears in historical astronomical records in Ptolemy's (2nd century CE), where it is described as the third star in the left wing of Virgo, cataloged among the 29 stars outlining the constellation's figure. In Arabic astronomy, it was incorporated into medieval catalogs as part of the asterism Al ʽAwwāʾ ("the Barker" or "barking dog"), with the specific designation Zāwiat al ʽAwwāʾ meaning "the angle of the barker," later rendered as Laouiyet al Aoua in some texts, referring to its position forming a bend or angle in the stellar pattern. During the , assigned it the designation γ Virginis in his influential atlas Uranometria (1603), standardizing its position as the second-brightest star in Virgo. The traditional name Porrima gained prominence in 19th-century astronomical literature, as documented in Richard Hinckley Allen's Star Names: Their Lore and Meaning (1899), which preserved classical and medieval etymologies. In ancient , the star held no specific prophetic associations but was positioned within the Supreme Palace Enclosure asterism (Tài Wēi Yuán), particularly as the second star of the Left Wall (Tài Wēi Zuǒ Yuán èr), symbolizing an imperial advisor in the cosmic representation of the emperor's court. The formalized the proper name Porrima (encompassing Antevorta as an variant) in 2016.

Modern studies

The binary nature of Antevorta (γ Virginis) was first noted by Father J. Richaud in 1689. resolved it further in 1783 using his 6.2-inch aperture telescope, measuring a separation of approximately 5.7 arcseconds and marking one of the early systematic observations of visual binaries. This observation highlighted the system's orbital motion, setting the stage for subsequent studies of . Orbital elements for the binary system were progressively refined beginning in the 19th century, building on earlier positional data from observers like Tycho Brahe in the late 16th century; significant updates came from Robert Grant's analysis in 1853, which incorporated historical measures to improve eccentricity and period estimates. Modern refinements draw from astrometric missions, including the Hipparcos satellite's 1997 data yielding a parallax of 0.0845 arcseconds and orbital period of about 169 years, and the Gaia mission's Data Release 3 (2022), which confirmed the distance at 38.1 light-years with higher precision and updated the semi-major axis to 3.64 arcseconds. These elements indicate an eccentricity of 0.88 and a binary separation briefly reaching 0.4 arcseconds at periapsis. The system's periapsis passage in 1836, observed notably by at the , provided critical data on its high eccentricity when the components approached within 0.3 arcseconds, nearly merging visually. This event allowed for direct assessment of orbital parameters, with predictions for the next close approach around 2005 (actual minimum separation 0.37 arcseconds) and a subsequent passage near 2174. Spectroscopic analysis through measurements has confirmed the individual masses of the components at approximately 1.4 solar masses each, derived from combined visual orbit and astrometric data, while showing no significant variability indicative of additional companions or pulsations. These studies underscore the stability of the F0 V main-sequence pair, with velocities varying predictably over the 169-year orbit. Recent contributions include the International Astronomical Union's formal approval of the name "Porrima" (with Antevorta as an alias) for the primary component in 2016, reflecting its mythological roots. Gaia's DR3 has solidified the distance estimate, enabling refined calculations of about 4 solar luminosities per star. Although no have been detected, preliminary studies have explored the potential zone around 2–3 AU, noting the system's youth (approximately 1.5 billion years) and moderate as conducive but unconfirmed factors. Future prospects involve continued monitoring for subtle orbital perturbations via high-resolution and , potentially revealing any long-term changes or rare events given the 31-degree inclination to the .
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