Astronomy:Pi Puppis

From HandWiki
Short description: Second-brightest star in the constellation of Puppis
Pi Puppis
Diagram showing star positions and boundaries of the Puppis constellation and its surroundings
Cercle rouge 100%.svg
Location of π Puppis (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Puppis
Right ascension  07h 17m 08.55678s[1]
Declination −37° 05′ 50.8962″[1]
Apparent magnitude (V) 2.733[2]
Characteristics
Spectral type K3 Ib[3]
U−B color index +1.238[2]
B−V color index +1.608[2]
Variable type SRd[4]
Astrometry
Radial velocity (Rv)+15.8[5] km/s
Proper motion (μ) RA: −10.05[1] mas/yr
Dec.: +6.47[1] mas/yr
Parallax (π)4.04 ± 0.33[1] mas
Distance810 ± 70 ly
(250 ± 20 pc)
Absolute magnitude (MV)−4.5[6]
Details
Mass11.7±0.2[7] M☉
Radius235[8] R☉
Luminosity11,378[8] L☉
Surface gravity (log g)0.13[8] cgs
Temperature3,990–4,055[9] K
Age20.0±3.9[7] Myr
Other designations
π Pup, CPD−36°1211, FK5 278, GC 9706, HD 56855, HIP 35264, HR 2773, SAO 197795, PPM 283747, CCDM J07171-3706A, WDS J07171-3706A[10]
Database references
SIMBADdata

Pi Puppis, Latinized from π Puppis, also named Ahadi,[11][12] is the second-brightest star in the southern constellation of Puppis. It has an apparent visual magnitude of 2.733, so it can be viewed with the naked eye at night. Parallax measurements yield an estimated distance of roughly 810 light-years (250 parsecs) from the Earth. This is a double star with a magnitude 6.86 companion at an angular separation of 0.72 arcsecond and a position angle of 148° from the brighter primary.[13]

A light curve for Pi Puppis, plotted from Hipparcos data,[14] folded with the period derived by Koen and Eyer (2002)[15]

The spectrum of Pi Puppis matches a stellar classification of K3 Ib.[3] The Ib luminosity class indicates this a lower luminosity supergiant star that has consumed the hydrogen fuel at its core, evolved away from the main sequence, and expanded to about 235 times the Sun's radius. The effective temperature of the star's outer envelope is approximately 4,000 K,[9] which gives it the orange hue of a K-type star.[16] It is a semiregular variable star[4] that varies in apparent magnitude from a high of 2.70 down to 2.85.[17] Pi Puppis is the brightest star in the open cluster Collinder 135.[18]

Naming

The star has the traditional name Ahadi, which is derived from Arabic for "having much promise".[11] In Chinese, 弧矢 (Hú Shǐ), meaning Bow and Arrow,[19] refers to an asterism consisting of π Puppis, δ Canis Majoris, η Canis Majoris, HD 63032, HD 65456, ο Puppis, k Puppis, ε Canis Majoris and κ Canis Majoris. Consequently, π Puppis itself is known as 弧矢九 (Hú Shǐ jiǔ, English: the Ninth Star of Bow and Arrow.)[20]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V 
  2. ↑ 2.0 2.1 2.2 Gutierrez-Moreno, Adelina et al. (1966), "A System of photometric standards", Publ. Dept. Astron. Univ. Chile (Publicaciones Universidad de Chile, Department de Astronomy) 1: 1–17, Bibcode: 1966PDAUC...1....1G 
  3. ↑ 3.0 3.1 Houk, Nancy (1979), "Michigan catalogue of two-dimensional spectral types for the HD stars", Michigan Catalogue of Two-dimensional Spectral Types for the HD stars. Volume_3. Declinations -40_ƒ0 to -26_ƒ0 (Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan) 3, Bibcode: 1982mcts.book.....H 
  4. ↑ 4.0 4.1 Kazarovets, E. V. et al. (January 1999), "The 74th Special Name-list of Variable Stars", Information Bulletin on Variable Stars 4659: 1, Bibcode: 1999IBVS.4659....1K 
  5. ↑ Evans, D. S. (June 20–24, 1966). "Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30". in Batten, Alan Henry; Heard, John Frederick. 30. University of Toronto: International Astronomical Union. 57. Bibcode: 1967IAUS...30...57E. 
  6. ↑ Parsons, Sidney B. (2001). "A Large Spectral Class Dependence of the Wilson-Bappu Effect among Luminous Stars". The Publications of the Astronomical Society of the Pacific 113 (780): 188–194. doi:10.1086/318616. Bibcode: 2001PASP..113..188P. 
  7. ↑ 7.0 7.1 Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society 410 (1): 190–200, doi:10.1111/j.1365-2966.2010.17434.x, Bibcode: 2011MNRAS.410..190T 
  8. ↑ 8.0 8.1 8.2 McDonald, I.; Zijlstra, A. A.; Watson, R. A. (15 June 2017). "Fundamental parameters and infrared excesses of Tycho–Gaia stars". Monthly Notices of the Royal Astronomical Society 471 (1): 770–791. doi:10.1093/mnras/stx1433. ISSN 0035-8711. Bibcode: 2017MNRAS.471..770M. 
  9. ↑ 9.0 9.1 Pérez Martínez, M. Isabel; Schröder, K.-P.; Cuntz, M. (June 2011), "The basal chromospheric Mg II h+k flux of evolved stars: probing the energy dissipation of giant chromospheres", Monthly Notices of the Royal Astronomical Society 414 (1): 418–427, doi:10.1111/j.1365-2966.2011.18421.x, Bibcode: 2011MNRAS.414..418P 
  10. ↑ "CCDM J07171-3706A -- Double or multiple star", SIMBAD (Centre de Données astronomiques de Strasbourg), http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Pi+Puppis 
  11. ↑ 11.0 11.1 Poppele, Jonathan (2010), Night Sky: A Field Guide to the Constellations, Adventure Publications, p. 264, ISBN 978-1591932291, https://books.google.com/books?id=LbAbDQAAQBAJ&pg=PA264. [yes|permanent dead link|dead link}}]
  12. ↑ "π Pup (Ahadi) - Star - SKY-MAP". http://server7.sky-map.org/starview?object_type=1&object_id=317&locale=EN. 
  13. ↑ Fabricius, C.; Makarov, V. V. (April 2000), "Two-colour photometry for 9473 components of close Hipparcos double and multiple stars", Astronomy and Astrophysics 356: 141–145, Bibcode: 2000A&A...356..141F 
  14. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html. 
  15. ↑ Koen, Chris; Eyer, Laurent (March 2002). "New periodic variables from the Hipparcos epoch photometry". Monthly Notices of the Royal Astronomical Society 331 (1): 45–59. doi:10.1046/j.1365-8711.2002.05150.x. Bibcode: 2002MNRAS.331...45K. 
  16. ↑ "The Colour of Stars", Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004, http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html, retrieved 2012-01-16 
  17. ↑ Burnham, Robert (1978), Burnham's celestial handbook: an observer's guide to the universe beyond the solar system, Dover books explaining science, 3 (2nd ed.), Courier Dover Publications, p. 1499, ISBN 0-486-23673-0, https://books.google.com/books?id=PJzIt3SIlkUC&pg=PA1499 
  18. ↑ Eggen, O. J. (February 1983), "Six clusters in Puppis-Vela", Astronomical Journal 88: 197–214, doi:10.1086/113306, Bibcode: 1983AJ.....88..197E 
  19. ↑ 弧矢 (Hú Shǐ) is westernized into Koo She. R.H. Allen had opinion that Koo She refers to the asterism including δ Velorum and ω Velorum. AEEA opinion is, δ Velorum is member of 天社 (Tiān Shè), meaning Celestial Earth God's Temple asterism and ω Velorum is not member of any asterisms. 天社 (Tiān Shè)is westernized into Tseen She and R.H.Allen used the term Tseen She for Chinese name of η Carinae. See Richard Hinckley Allen: Star Names — Their Lore and Meaning: Argo Navis and (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 17 日.
  20. ↑ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 16 日

External links



Retrieved from "https://handwiki.org/wiki/index.php?title=Astronomy:Pi_Puppis&oldid=3428223"