Pi Puppis

Short description: Second-brightest star in the constellation of Puppis

For the meteor shower, see Astronomy:Pi Puppids.

π Puppis

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) | 2.69 - 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[1] mas
Distance| 810 ± 70 ly
(250 ± 20 pc)
Absolute magnitude (MV)| −4.5[7]
Details
Mass| 11.7±0.2[8] M☉
Radius| 235[9] R☉
Luminosity| 11,378[9] L☉
Surface gravity (log g)| 0.13[9] cgs
Temperature| 3,990–4,055[10] K
Age| 20.0±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
SIMBAD| data

Pi Puppis, Latinized from π Puppis, also named Ahadi,[12][11] 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.[13]

## Contents

* 1 Description
* 2 Nomenclature
* 3 Observation
* 4 References

## Description

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,[10] which gives it the orange hue of a K-type star.[16] 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.[17] Pi Puppis is the brightest star in the open cluster Collinder 135.[18]

## Nomenclature

This star does not seem to have had a traditional proper name,[19] but some 21st-century sources use the name Ahadi, which is derived from Arabic for "having much promise".[12] This name appears in the SIMBAD database[11] and at least one academic paper.[20]

In Chinese, 弧矢 (Hú Shǐ), meaning Bow and Arrow,[21] 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).[22]

## Observation

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.[23] 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.[18]

About every five years, the Pi Puppids, a meteor shower associated with the comet 26P/Grigg–Skjellerup, appears near the star in late April.[18] The Pi Puppids are a variable meteor shower, with varying maximums each year.[24]

## 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 "zeta Pup". AAVSO. https://www.aavso.org/vsx/index.php?view=detail.top&oid=27176.
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 4.2 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
5. ↑ 5.0 5.1 5.2 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). "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.
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. doi:10.1086/318616. Bibcode: 2001PASP..113..188P.
8. ↑ 8.0 8.1 8.2 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
9. ↑ 9.0 9.1 9.2 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.
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, doi:10.1111/j.1365-2966.2011.18421.x, Bibcode: 2011MNRAS.414..418P
11. ↑ 11.0 11.1 11.2 "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 978-1591932291, https://books.google.com/books?id=LbAbDQAAQBAJ&pg=PA264.
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. ↑ 18.0 18.1 18.2 Eggen, O. J. (February 1983), "Six clusters in Puppis-Vela", Astronomical Journal 88: 197–214, doi:10.1086/113306, Bibcode: 1983AJ.....88..197E
19. ↑ Kaler, Jim. "Pi Pup". http://stars.astro.illinois.edu/sow/pipup.html.
20. ↑ Neuhäuser, R.; Torres, G. (October 2022). "Colour evolution of Betelgeuse and Antares over two millennia, derived from historical records, as a new constraint on mass and age". Monthly Notices of the Royal Astronomical Society 516 (1): 693-719. doi:10.1093/mnras/stac1969. Bibcode: 2022MNRAS.516..693N.
21. ↑ 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 .
22. ↑ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 16 日
23. ↑ Celis S., L. (1982). "Red variable stars. I — UBVRI photometry and photometric properties". Astronomical Journal 87: 1791–1802. doi:10.1086/113268. Bibcode: 1982AJ.....87.1791C.
24. ↑ "Meteor Data Center: 137 PPU". International Astronomical Union (IAU). https://www.ta3.sk/IAUC22DB/MDC2022/Roje/pojedynczy_obiekt.php?lporz=00350&kodstrumienia=00137. Retrieved 2023-10-09.

* v
* t
* e

Stars of Puppis

Bayer|

* ζ (Naos)
* ν
* ξ (Azmidi)
* ο
* π
* ρ (Tureis)
* σ
* τ
* χ
* L2

Flamsteed|

* 1
* 2
* 3 (l)
* 4
* 5
* 6
* 8
* 9
* 10
* 11 (j)
* 12
* 14
* 16
* 18
* 19
* 20
* 21
* 22

Variable|

* R
* T (not variable)
* V
* Z
* RS
* RX
* ST
* TY
* UY
* UZ
* VV
* VX
* VZ
* WW
* AQ
* AR
* AU
* BB
* BN
* BV
* CP
* HH
* HZ
* KQ
* MX (r)
* MY (y3)
* MZ
* NO
* NP
* NS (h1)
* NV (υ1)
* NW (υ2)
* NX
* OU (L1)
* OS
* OW (z)
* OX
* PQ
* PR
* PT
* PU (m)
* PV
* PX
* PY
* QS
* QU
* QW (I)
* QY
* QZ (b)
* V336
* V338
* V339
* V347
* V348
* V351
* V363
* V368
* V376
* V378
* V390
* V392
* V397
* V420
* V436
* V438
* V443
* V445
* V468 (d4)
* V510
* V574
* V575
* V596
* V597
* V598

HR|

* 2157
* 2158
* 2178
* 2187
* 2204
* 2211
* 2348 (G)
* 2384
* 2462 (V)
* 2475
* 2482
* 2488
* 2518 (x)
* 2548 (X)
* 2549
* 2558
* 2563
* 2579
* 2594
* 2604
* 2608
* 2612
* 2619 (t)
* 2626
* 2641
* 2658
* 2666 (C)
* 2667
* 2672 (H)
* 2677
* 2685
* 2687
* 2691 (D)
* 2702 (A)
* 2719
* 2727 (E)
* 2759
* 2762
* 2769
* 2770
* 2771
* 2789 (M)
* 2791 (F)
* 2794
* 2829
* 2856
* 2860
* 2863
* 2868
* 2870
* 2873
* 2874
* 2875 (y)
* 2881
* 2895
* 2897
* 2899
* 2900
* 2906
* 2909 (n)
* 2910 (n)
* 2913
* 2916
* 2922 (p)
* 2923
* 2933
* 2937 (f)
* 2940 (y2)
* 2945
* 2948 (k1)
* 2949 (k2)
* 2954 (e)
* 2955
* 2956
* 2959
* 2960
* 2961 (d1)
* 2963 (d2)
* 2964 (d3)
* 2976
* 2981
* 2984
* 2988
* 2994
* 2998
* 3001
* 3002 (W)
* 3007
* 3011
* 3017 (c)
* 3018
* 3019
* 3020
* 3023
* 3027
* 3035
* 3037
* 3042
* 3043
* 3046 (Q)
* 3051
* 3052
* 3055 (P)
* 3057
* 3060
* 3068
* 3069
* 3071
* 3074
* 3079
* 3080 (a)
* 3085
* 3089
* 3090 (J)
* 3091
* 3092
* 3096
* 3101
* 3111
* 3114
* 3116 (N)
* 3118
* 3121 (O)
* 3131
* 3137
* 3140
* 3142
* 3143
* 3148
* 3154
* 3155
* 3160
* 3166
* 3177
* 3183
* 3190
* 3194
* 3199
* 3205
* 3219
* 3226
* 3233
* 3238
* 3239
* 3241
* 3242
* 3243 (h2)
* 3251
* 3253
* 3259
* 3261
* 3266
* 3270 (q)
* 3273
* 3276
* 3279
* 3281
* 3282 (w)
* 3283
* 3286
* 3291
* 3308
* 3315
* 3316
* 3317
* 3320
* 3324
* 3326

HD|

* 44594
* 48265 (Nosaxa)
* 49798
* 50499
* 53680
* 53706
* 59235
* 61005
* 61589
* 61750
* 62542
* 63291
* 63399
* 63696
* 63734
* 65638
* 66885
* 67408
* 69904
* 70642

Gliese|

* Gliese 257
* Gliese 283
* Gliese 300

Other|

* 171 G. Puppis
* Bran 76
* L 745-46A
* 2MASS 0729−39
* NGC 2423-3
* OH 231.8+4.2
* PSR B0740−28
* PSR B0808−13
* PSR J0737−3039
* PSR J0738−4042
* RX J0812.4−3114
* RX J0822−4300
* SCR J0740−4257
* SWIFT J0732.5−1331
* 4U 0728-25
* WASP-121

* List

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