Pi Puppis

From the Science Archives, the open-project database of science information
Jump to navigation Jump to search


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
Epoch J2000      Equinox J2000
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
Radius290[8][better source needed] R
Diameter290[8][better source needed] D
Luminosity11,825[9] L
Temperature3,990–4,055[10] K
Age20.0 ± 3.9[7] Myr
Other designations
π Pup, CPD−36° 1211, FK5 278, GC 9706, PPM=283747, HD 56855, HIP 35264, HR 2773, SAO 197795, CCDM J07171-3706A, WDS J07171-3706Aa,Ab[11]
Database references
SIMBADdata

Pi Puppis, Latinized from π Puppis, also named Ahadi,[12][13] is the second-brightest star in the southern constellation of Puppis. It has an apparent visual magnitude of 2.733,[2] 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.[1] 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.[14]

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 290 times the Sun's radius.[8] The effective temperature of the star's outer envelope is approximately 4,000 K,[10] which gives it the orange hue of a K-type star.[15] It is a semiregular variable star[4] that varies in apparent magnitude from a high of 2.70 down to 2.85.[16] Pi Puppis is the brightest star in the open cluster Collinder 135.[17]

Naming[edit]

The star has the traditional name Ahadi, which is derived from Arabic for "having much promise".[12] In Chinese, 弧矢 (Hú Shǐ), meaning Bow and Arrow,[18] 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.)[19]

References[edit]

  1. 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, arXiv:0708.1752, Bibcode 2007A&A...474..653V, doi:10.1051/0004-6361:20078357
  2. 2.0 2.1 2.2 2.3 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. Lua error in Module:Citation/CS1 at line 637: attempt to concatenate local 'chapter' (a table value).
  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. Bibcode 2001PASP..113..188P. doi:10.1086/318616.
  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, arXiv:1007.4883, Bibcode 2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x
  8. 8.0 8.1 Kaler, james B., "PI PUP (Pi Puppis)", Stars (University of Illinois), http://stars.astro.illinois.edu/sow/pipup.html, retrieved 2012-01-10
  9. McDonald, I. et al. (2012), "Fundamental Parameters and Infrared Excesses of Hipparcos Stars", Monthly Notices of the Royal Astronomical Society 427 (1): 343–57, arXiv:1208.2037, Bibcode 2012MNRAS.427..343M, doi:10.1111/j.1365-2966.2012.21873.x.
  10. 10.0 10.1 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, arXiv:1102.4832, Bibcode 2011MNRAS.414..418P, doi:10.1111/j.1365-2966.2011.18421.x
  11. "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
  12. 12.0 12.1 Poppele, Jonathan (2010), Night Sky: A Field Guide to the Constellations, Adventure Publications, p. 264, ISBN 1591932297, https://books.google.com/books?id=LbAbDQAAQBAJ&pg=PA264.
  13. http://server7.sky-map.org/starview?object_type=1&object_id=317&locale=EN
  14. 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
  15. "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
  16. 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
  17. Eggen, O. J. (February 1983), "Six clusters in Puppis-Vela", Astronomical Journal 88: 197–214, Bibcode 1983AJ.....88..197E, doi:10.1086/113306
  18. 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.
  19. (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 16 日


Add your comment
The Science Archives welcomes all comments. If you do not want to be anonymous, register or log in. It is free.


As a reminder, article comments are only for discussions on how to improve the article. Please direct other comments to a user's talk page. Please be formal and do not use excessive uppercase. Please be advised you may receive an automatic block if you break the article comments policy. For information regarding what is acceptable/not acceptable in article comments, please message Icons-flag-ru.png Joey (talk), Natalia (talk), Icons-flag-fr.png ynoss (talk), or Icons-flag-ca.png Daniel (older account/talk).


External links[edit]