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Beta Pavonis, Latinised from β Pavonis, is a single,[9] white-hued star in the southern constellation of Pavo. It can be seen with the naked eye, having an apparent visual magnitude of 3.42.[2] Based upon an annual parallax shift of 24.14 mas as seen from Earth, it is located 135 light-years from the Sun. It is moving away from the Sun with a radial velocity of +4 km/s.[6] Beta Pavonis is a member of the Ursa Major Moving Group, a set of stars that share a similar motion through space.[10]

β Pavonis
Location of β Pavonis (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Pavo
Right ascension 20h 44m 57.49399s[1]
Declination −66° 12′ 11.5708″[1]
Apparent magnitude (V) 3.42[2]
Characteristics
Spectral type A5 IV[3] or A7 III[4]
U−B color index +0.12[5]
B−V color index +0.16[5]
Astrometry
Radial velocity (Rv)+3.7±0.5[6] km/s
Proper motion (μ) RA: −42.67[1] mas/yr
Dec.: +9.94[1] mas/yr
Parallax (π)24.14 ± 0.16 mas[1]
Distance135.1 ± 0.9 ly
(41.4 ± 0.3 pc)
Absolute magnitude (MV)+0.33[2]
Details
Mass2.51[3] M☉
Radius2.3[7] R☉
Luminosity66[3] L☉
Surface gravity (log g)3.84[8] cgs
Temperature8,184±278[8] K
Rotational velocity (v sin i)75[3] km/s
Age305[8] Myr
Other designations
β Pav, CPD−66° 3501, FK5 775, GC 28862, HD 197051, HIP 102395, HR 7913, SAO 254862
Database references
SIMBADdata

Zorec and Royer (2012) list a stellar classification for this star of A5 IV,[3] indicating it is an evolving subgiant star that has consumed the hydrogen at its core and has begun to expand onto the red giant branch. However, Houk (1979) listed a more evolved class of A7 III,[4] suggesting it is already a giant star. It has about 2.3[7] times the Sun's radius and 2.51[3] times the mass of the Sun. At the estimated age of 305[8] million years, the star still has a relatively high rate of spin, having a projected rotational velocity of 75 km/s.[3] Beta Pavonis is radiating 66[3] times the Sun's luminosity from its photosphere at an effective temperature of about 8,184 K.[8]


References


  1. Van Leeuwen, F. (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. Vizier catalog entry
  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. Vizier catalog entry
  3. Zorec, J.; Royer, F. (2012). "Rotational velocities of A-type stars". Astronomy & Astrophysics. 537: A120. arXiv:1201.2052. Bibcode:2012A&A...537A.120Z. doi:10.1051/0004-6361/201117691. S2CID 55586789. Vizier catalog entry
  4. Houk, Nancy (1979). Michigan catalogue of two-dimensional spectral types for the HD stars. Vol. 1. Ann Arbor, Michigan: Department of Astronomy, University of Michigan. Bibcode:1978mcts.book.....H.
  5. Mallama, A. (2014). "Sloan Magnitudes for the Brightest Stars". The Journal of the American Association of Variable Star Observers. 42 (2): 443. Bibcode:2014JAVSO..42..443M.Vizier catalog entry
  6. Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv:1606.08053. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. S2CID 119231169.
  7. Pasinetti Fracassini, L. E.; et al. (February 2001). "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)". Astronomy and Astrophysics (Third ed.). 367: 521–524. arXiv:astro-ph/0012289. Bibcode:2001A&A...367..521P. doi:10.1051/0004-6361:20000451. S2CID 425754.
  8. David, Trevor J.; Hillenbrand, Lynne A. (2015). "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets". The Astrophysical Journal. 804 (2): 146. arXiv:1501.03154. Bibcode:2015ApJ...804..146D. doi:10.1088/0004-637X/804/2/146. S2CID 33401607. Vizier catalog entry
  9. 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.
  10. Chupina, N. V.; et al. (June 2006). "Kinematic structure of the corona of the Ursa Major flow found using proper motions and radial velocities of single stars". Astronomy and Astrophysics. 451 (3): 909–916. Bibcode:2006A&A...451..909C. doi:10.1051/0004-6361:20054009.

На других языках

- [en] Beta Pavonis

[ru] Бета Павлина

Бета Павлина (лат. Beta Pavonis) — одиночная[10] белая звезда в южном созвездии Павлина. Доступна для наблюдения невооружённым глазом, обладает видимой звёздной величиной 3,42[2]. Годичный параллакс составляет 24,14 мсд при наблюдении с Земли. Звезда расположена на расстоянии 135 световых лет от Солнца. Бета Павлина удаляется от Солнца с лучевой скоростью +4 км/с[3]. Бета Павлина входит в состав движущейся группы звёзд Большой Медведицы, множества звёзд с похожими кинематическими свойствами[11].


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