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Pi Puppis

From Wikipedia - Reading time: 8 min

For the meteor shower, see Pi Puppids.
π Puppis
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) 2.69 – 2.76[2]
Characteristics
Spectral type K3 Ib[3]
U−B color index +1.238[4]
B−V color index +1.608[4]
Variable type SRd[5]
Astrometry
Radial velocity (Rv)+15.8[6] km/s
Proper motion (μ) RA: −10.05[1] mas/yr
Dec.: +6.47[1] mas/yr
Parallax (π)4.04±0.33 mas[1]
Distance810 ± 70 ly
(250 ± 20 pc)
Absolute magnitude (MV)−4.5[7]
Details
Mass11.7±0.2[8] M☉
Radius235[9] R☉
Luminosity11,378[9] L☉
Surface gravity (log g)0.13[9] cgs
Temperature3,990–4,055[10] K
Age20.0±3.9[8] 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[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 about 2.7, 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.[14]

A light curve for Pi Puppis, plotted from Hipparcos data,[15] folded with the period derived by Koen and Eyer (2002)[16]

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,[10] which gives it the orange hue of a K-type star.[17] With a mass 11.7 times that of the Sun, this is a short-lived star with an estimated age of 20 million years.[8]

It is a semiregular variable star[5] that varies in apparent magnitude from a high of 2.70 down to 2.85.[18] Pi Puppis is the brightest star in the open cluster Collinder 135.[19]

Nomenclature

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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,[20] 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.)[21]

Observation

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Collinder 135

Pi Puppis is a semiregular variable star[5] with an apparent magnitude of 2.733.[4] It appears slightly orange in color with a B-V color index of +1.608, similar to that of the famous Mira.[22] It is typically the second brightest star in Puppis, only behind the blue supergiant Naos,[2] and the brightest star in the open cluster Collinder 135.[19]

About every five years, the Pi Puppids, a meteor shower associated with the comet 26P/Grigg–Skjellerup, appears near the star in late April.[19] The Pi Puppids are a variable meteor shower, with varying maximums each year.[23]

References

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  1. ^ a b c d e 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, S2CID 18759600
  2. ^ a b "zeta Pup". International Variable Star Index. AAVSO. Retrieved 2022-06-15.
  3. ^ a b 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, 3, Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan, Bibcode:1982mcts.book.....H
  4. ^ a b c Gutierrez-Moreno, Adelina; et al. (1966), "A System of photometric standards", Publ. Dept. Astron. Univ. Chile, 1, Publicaciones Universidad de Chile, Department de Astronomy: 1–17, Bibcode:1966PDAUC...1....1G
  5. ^ a b c 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
  6. ^ Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". In Batten, Alan Henry; Heard, John Frederick (eds.). Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30. Determination of Radial Velocities and Their Applications. Vol. 30. University of Toronto: International Astronomical Union. p. 57. Bibcode:1967IAUS...30...57E.
  7. ^ 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. Bibcode:2001PASP..113..188P. doi:10.1086/318616.
  8. ^ a b c 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, S2CID 118629873
  9. ^ a b c 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. arXiv:1706.02208. Bibcode:2017MNRAS.471..770M. doi:10.1093/mnras/stx1433. eISSN 1365-2966. ISSN 0035-8711.
  10. ^ a b 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, S2CID 59268230
  11. ^ "CCDM J07171-3706A -- Double or multiple star", SIMBAD, Centre de Données astronomiques de Strasbourg
  12. ^ a b Poppele, Jonathan (2010), Night Sky: A Field Guide to the Constellations, Adventure Publications, p. 264, ISBN 978-1591932291.[permanent dead link]
  13. ^ "π Pup (Ahadi) - Star - SKY-MAP".
  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. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  16. ^ 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. arXiv:astro-ph/0112194. Bibcode:2002MNRAS.331...45K. doi:10.1046/j.1365-8711.2002.05150.x.
  17. ^ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on March 18, 2012, retrieved 2012-01-16
  18. ^ Burnham, Robert (1978), Burnham's celestial handbook: an observer's guide to the universe beyond the solar system, Dover books explaining science, vol. 3 (2nd ed.), Courier Dover Publications, p. 1499, ISBN 0-486-23673-0
  19. ^ a b c Eggen, O. J. (February 1983), "Six clusters in Puppis-Vela", Astronomical Journal, 88: 197–214, Bibcode:1983AJ.....88..197E, doi:10.1086/113306
  20. ^ 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 Archived 2012-02-04 at the Wayback Machine.
  21. ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 16 日 Archived 2011-08-22 at the Wayback Machine
  22. ^ Celis S., L. (1982). "Red variable stars. I — UBVRI photometry and photometric properties". Astronomical Journal. 87: 1791–1802. Bibcode:1982AJ.....87.1791C. doi:10.1086/113268.
  23. ^ "Meteor Data Center: 137 PPU". International Astronomical Union (IAU). Retrieved 2023-10-09.
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