WZ Doradus

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WZ Doradus
Dorado constellation map.svg
Red circle.svg
Location of WZ Doradus on the map (circled)
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Dorado
Right ascension 05h 07m 34.02686s [1]
Declination −63° 23′ 58.8474″ [1]
Apparent magnitude  (V)5.20 - 5.32 [2]
Characteristics
Evolutionary stage AGB [3]
Spectral type M3 III [4]
U−B color index +1.85 [5]
B−V color index +1.65 [5]
Variable type SRb [2]
Astrometry
Radial velocity (Rv)19.3±2.8 [6]  km/s
Proper motion (μ)RA: +13.210  mas/yr [1]
Dec.: −44.813  mas/yr [1]
Parallax (π)5.6282 ± 0.1116  mas [1]
Distance 580 ± 10  ly
(178 ± 4  pc)
Absolute magnitude  (MV)−1.00 [7]
Details
Mass 1.4 [8]   M☉
Radius 88.3+6.6
−10.0 [9]   R☉
Luminosity 1,248±47 [9]   L☉
Surface gravity (log g)0.50 [10]   cgs
Temperature 3,603±125 [10]   K
Other designations
21 G. Doradus [11] , WZ Dor, CD−63°188, CPD−63°420, FK5  2389, GC  6314, HD  33684, HIP  23840, HR  1695, SAO  249198, TIC  55298910 [12]
Database references
SIMBAD data

WZ Doradus (HD 33684; HR 1695; 21 G. Doradus) is a solitary red-hued variable star [13] located in the southern constellation Dorado. It has an average apparent magnitude of 5.21, [14] making it faintly visible to the naked eye under ideal conditions. Gaia DR3 parallax measurements imply a distance of 580 light-years [1] and it is currently receding with a heliocentric radial velocity of 19.3  km/s . [6] At its current distance, WZ Doradus is diminished by two-tenths of a magnitude due to interstellar extinction and it has an absolute magnitude of −1.00. [7]

HD 33684 was first observed to vary in brightness by astronomer P. M. Corben in 1971. [15] It was said to have an amplitude of 0.18 magnitudes. A year later, HD 33684 was given the variable star designation WZ Doradus. [16] It was again observed in 1973 by Olin J. Eggen and he noticed that it varied within 40 days. [17] A 1998 survey found no strong emissions indicating dust around the star. [18] Another survey also found no technetium in its spectrum. [19] WZ Doradus is a semiregular variable of subtype SRb that varies between 5.2 and 5.32 within an average period of 40 days. [2] Tabur et al. (2009) found two periods for the star after it was widely believed to only have one period. [20]

WZ Doradus variability periods [20]
Amplitude (mag)Period (days)
0.04226.0
0.02644.6
A light curve for WZ Doradus, plotted from data published by Tabur et al. WZDorLightCurve.png
A light curve for WZ Doradus, plotted from data published by Tabur et al.

WZ Doradus has a stellar classification of M3 III, [4] indicating that it is an evolved red giant. It is currently on the asymptotic giant branch, [3] generating energy via the fusion of hydrogen and helium shells around an inert carbon core. As a result of its evolved state, it has expanded to 88.3 times the radius of the Sun [9] and it now radiates 1,248 times the luminosity of the Sun [9] from its enlarged photosphere at an effective temperature of 3,603  K . [10]

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References

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  4. 1 2 Houk, N.; Cowley, A. P. (1975). University of Michigan Catalogue of two-dimensional spectral types for the HD stars: Declinations −90° to −53°. Vol. 1. Bibcode:1975mcts.book.....H.
  5. 1 2 Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data. SIMBAD, Bibcode:1986EgUBV........0M
  6. 1 2 Gontcharov, G. A. (November 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. eISSN   1562-6873. ISSN   1063-7737. S2CID   119231169.
  7. 1 2 Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331–346. arXiv: 1108.4971 . Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. eISSN   1562-6873. ISSN   1063-7737. S2CID   119257644.
  8. ↑ Kervella, Pierre; et al. (March 2019). "Stellar and substellar companions of nearby stars from Gaia DR2. Binarity from proper motion anomaly". Astronomy & Astrophysics. 623: 23. arXiv: 1811.08902 . Bibcode:2019A&A...623A..72K. doi:10.1051/0004-6361/201834371. S2CID   119491061. A72.
  9. 1 2 3 4 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
  10. 1 2 3 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. S2CID   73594365.
  11. ↑ Gould, Benjamin Apthorp (1878). "Uranometria Argentina : brillantez y posicion de las estrellas fijas, hasta la septima magnitud, comprendidas dentro de cien grados del polo austral : con atlas". Resultados del Observatorio Nacional Argentino. 1. Bibcode:1879RNAO....1.....G.
  12. ↑ "V* WZ Dor". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved August 30, 2023.
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  14. ↑ Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H. ISSN   0004-6361. S2CID   17128864.
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  16. ↑ Kukarkin, B. V.; Kholopov, P. N.; Kukarkina, N. P.; Perova, N. B. (1 September 1972). "58th Name-List of Variable Stars". Information Bulletin on Variable Stars. 717: 1. Bibcode:1972IBVS..717....1K. ISSN   0374-0676.
  17. ↑ Eggen, O. J. (September 1973). "The classification of intrinsic variables. IV. Very-small-amplitude, very-short-period red variables". The Astrophysical Journal. 184: 793. Bibcode:1973ApJ...184..793E. doi: 10.1086/152371 . eISSN   1538-4357. ISSN   0004-637X. S2CID   120021304.
  18. ↑ Sloan, G. C.; Price, S. D. (December 1998). "The Infrared Spectral Classification of Oxygen-rich Dust Shells". The Astrophysical Journal Supplement Series. 119 (2). American Astronomical Society: 141–158. Bibcode:1998ApJS..119..141S. doi:10.1086/313156. ISSN   0067-0049. S2CID   53469543.
  19. ↑ Lebzelter, Th.; Hron, J. (November 1999). "A search for Technetium in semiregular variables". Astronomy and Astrophysics. 351: 533–542. Bibcode:1999A&A...351..533L. ISSN   0004-6361. S2CID   17019103.
  20. 1 2 3 Tabur, V.; Bedding, T. R.; Kiss, L. L.; Moon, T. T.; Szeidl, B.; Kjeldsen, H. (21 December 2009). "Long-term photometry and periods for 261 nearby pulsating M giants". Monthly Notices of the Royal Astronomical Society. 400 (4): 1945–1961. arXiv: 0908.3228 . Bibcode:2009MNRAS.400.1945T. doi: 10.1111/j.1365-2966.2009.15588.x . eISSN   1365-2966. ISSN   0035-8711. S2CID   15358380.
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