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Pi Piscis Austrini, Latinized from π Piscis Austrini, is binary star[5] system in the southern constellation of Piscis Austrinus, near the eastern constellation border with Sculptor. It has a yellow-white hue and is visible to the naked eye as a dim point of light with an apparent visual magnitude of 5.12.[2] The system is located at a distance of 92 light-years from the Sun based on parallax.[1] Its radial velocity is poorly constrained, but it appears to be drifting closer at a rate of around −6 km/s.[2] Pi Piscis Austrini is moving through the galaxy at a velocity of 16.3 km/s relative to the Sun. Its projected galactic orbit carries it between 24,000 and 37,500 light-years from the center of the galaxy.[2]

Pi Piscis Austrini
Location of π Piscis Austrini (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Piscis Austrinus
Right ascension 23h 03m 29.81653s[1]
Declination −34° 44′ 57.8827″[1]
Apparent magnitude (V) 5.12[2]
Characteristics
Spectral type F1 V Fe-0.8[3] + F3 V[4][5]
U−B color index +0.00[6]
B−V color index +0.29[6]
Astrometry
Radial velocity (Rv)−6.0±4.2[2] km/s
Proper motion (μ) RA: +72.789[1] mas/yr
Dec.: +83.569[1] mas/yr
Parallax (π)35.3691 ± 0.2124 mas[1]
Distance92.2 ± 0.6 ly
(28.3 ± 0.2 pc)
Absolute magnitude (MV)+2.78[2]
Orbit[7]
Period (P)178.3177±0.0038 d
Semi-major axis (a)≥ 0.296 AU
Eccentricity (e)0.5286±0.0041
Periastron epoch (T)2,435,319.73±0.25
Argument of periastron (ω)
(secondary)		2.62±0.81°
Semi-amplitude (K1)
(primary)		21.28±0.16 km/s
Details
A
Mass1.51[3] M☉
Radius1.64+0.11
−0.08[1] R☉
Luminosity5.85±0.04[1] L☉
Surface gravity (log g)4.30±0.14[3] cgs
Temperature7,003+195
−216[1] K
Metallicity [Fe/H]+0.12[2] dex
Age474[3] Myr
Other designations
π PsA, CD−35° 15630, GC 32122, GJ 886.2, (Wo) 9807, HD 217792, HIP 113860, HR 8767, SAO 214275[8]
Database references
SIMBADdata

This is a single-lined spectroscopic binary system with an orbital period of 178.3 days and an eccentricity of 0.53.[7] The primary component is an F-type main-sequence star with a stellar classification of F1 V Fe-0.8.[3] In 1965 it was designated a classical Cepheid variable star with a brightness that ranged from 5.10 to 5.12, but is now considered to be (most likely) constant.[4][9] It displays an infrared excess, suggesting a circumstellar disk is orbiting at a radius of 23 AU with a mean temperature of 90 K.[10] The cooler secondary companion has a class of F3 V.[5] The system appears to be a source of X-ray emission.[11]


References


  1. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
  3. Gray, R. O.; et al. (July 2006). "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample". The Astronomical Journal. 132 (1): 161–170. arXiv:astro-ph/0603770. Bibcode:2006AJ....132..161G. doi:10.1086/504637. S2CID 119476992.
  4. Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, GCVS 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID 125853869.
  5. Eggleton, P. P.; Tokovinin, A. A. (September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society. 389 (2): 869–879. arXiv:0806.2878. Bibcode:2008MNRAS.389..869E. doi:10.1111/j.1365-2966.2008.13596.x. S2CID 14878976.
  6. Cousins, A. W. J. (1973). "UBV Photometry of Some Southern Stars (Second List)". Monthly Notes of the Astron. Soc. Southern Africa. 32: 11. Bibcode:1973MNSSA..32...11C.
  7. Bopp, B. W.; et al. (1970). "Orbital elements of six spectroscopic binary stars". Monthly Notices of the Royal Astronomical Society. 147 (4): 355–366. Bibcode:1970MNRAS.147..355B. doi:10.1093/mnras/147.4.355.
  8. "* pi. PsA". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 7 January 2017.
  9. Janot-Pacheco, E. (August 1974). "On the cepheid nature of pi PsA". Astronomy and Astrophysics. 34: 325–326. Bibcode:1974A&A....34..325J.
  10. Cotten, Tara H.; Song, Inseok (July 2016). "A Comprehensive Census of Nearby Infrared Excess Stars". The Astrophysical Journal Supplement Series. 225 (1): 24. arXiv:1606.01134. Bibcode:2016ApJS..225...15C. doi:10.3847/0067-0049/225/1/15. S2CID 118438871. 15.
  11. Haakonsen, Christian Bernt; Rutledge, Robert E. (September 2009). "XID II: Statistical Cross-Association of ROSAT Bright Source Catalog X-ray Sources with 2MASS Point Source Catalog Near-Infrared Sources". The Astrophysical Journal Supplement. 184 (1): 138–151. arXiv:0910.3229. Bibcode:2009ApJS..184..138H. doi:10.1088/0067-0049/184/1/138. S2CID 119267456.



На других языках

- [en] Pi Piscis Austrini

[es] Pi Piscis Austrini

Pi Piscis Austrini (π PsA / HD 217792 / HR 8767) es una estrella en la constelación de Piscis Austrinus de magnitud aparente +5,14[1] que se encuentra a 93 años luz del Sistema Solar. Es una estrella de la secuencia principal de tipo espectral F1V con una temperatura efectiva de 7143 K.[2] Su velocidad de rotación proyectada —límite inferior de la misma—, es de 28 km/s, unas 14 veces más rápida que la del Sol.[3] Posee una metalicidad significativamente menor que la de nuestra estrella ([M/H] = -0,30) y su edad se estima en 900 millones de años.[4]

[ru] Пи Южной Рыбы

Pi Piscis Austrini (Pi PsA, π Piscis Austrini, π PsA) — звезда в созвездии Южной Рыбы. Видимая звёздная величина +5.12 (видна невооружённым глазом). Находится на расстоянии 93 световых года от Солнца.


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