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HD 33579
	; A light curve for HD 33579, plotted from Hipparcos data
Observation data; Epoch J2000.0 Equinox J2000.0
Constellation	Dorado
Right ascension	5h 5m 55.51147s
Declination	−67° 53′ 10.9330″
Apparent magnitude (V)	8.99 - 9.22
Characteristics
Spectral type	A3Ia+
U−B color index	−0.29
B−V color index	+0.14
Variable type	α Cygni
Astrometry
Radial velocity (Rv)	255.959 km/s
Proper motion (μ)	RA: +1.810 mas/yr ; Dec.: +0.146 mas/yr
Parallax (π)	0.0178 ± 0.0137 mas
Distance	148,700 ly ; (45,600 pc)
Absolute magnitude (MV)	−9.57
Details
Mass	20–30 M☉
Radius	419; 471 R☉
Luminosity	575,400 L☉
Surface gravity (log g)	0.82±0.21 cgs
Temperature	7,763 K
Metallicity [Fe/H]	−0.38±0.14 dex
Other designations
	HD 33579, CD−68 258, HIP 23718, R76, SK −67 44, AAVSO 0506-68
Database references
SIMBAD	data

HD 33579 is a white/yellow hypergiant and one of the brightest stars in the Large Magellanic Cloud (LMC). It is a suspected variable star.

HD 33579 lies in a part of the Hertzsprung–Russell diagram referred to as the Yellow Evolutionary Void because stars with that combination of luminosity and temperature are extremely unstable. They either expand to become cooler or shed their outer layers completely to become hotter. Yet HD 33579 is relatively stable, hardly even variable. This is thought to be due to its higher mass compared to most stars with similar temperature and luminosity.^[4] It has a radius of approximately 650 solar radii, comparable to Betelgeuse and larger than the orbit of Mars.^[11]

HD 33579 is an extremely rare type of star currently evolving for the first time through the yellow evolutionary void from being a blue hypergiant to becoming a red hypergiant. This means the star is often referred to as a yellow hypergiant although the spectral type of A3 means it is also described as a white hypergiant.^[4]

Although HD 33579 has not been formally listed in the General Catalogue of Variable Stars, analysis of Hipparcos photometry confirmed small amplitude variations in its brightness that had been reported in earlier research.^[13]^[14]^[15] Periods of 620 days and 105 days are found, plus other possible shorter periods. The total amplitude is only around 0.1 magnitudes.^[6] A statistical analysis of Hipparcos photometry showed a possible period of 27 days.^[16]

Notes

^ Applying the Stefan–Boltzmann law with a nominal solar effective temperature of 5,772 K:
${\sqrt {{\biggl (}{\frac {5,772}{7,763}}{\biggr )}^{4}\cdot 10^{5.76}}}=419.37\ R_{\odot }$ .
^ Applying the Stefan–Boltzmann law with a nominal solar effective temperature of 5,772 K:
${\sqrt {{\biggl (}{\frac {5,772}{7,145}}{\biggr )}^{4}\cdot 10^{5.716}}}=470.6\ R_{\odot }$ .

References

^ "Hipparcos Tools Interactive Data Access". Hipparcos. ESA. Retrieved 8 December 2021.
^ ^a ^b ^c ^d ^e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
^ "LMC V1006". International Variable Star Index. AAVSO. Retrieved 2022-08-12.
^ ^a ^b ^c ^d ^e Nieuwenhuijzen, H.; De Jager, C. (2000). "Checking the yellow evolutionary void. Three evolutionary critical Hypergiants: HD 33579, HR 8752 & IRC +10420". Astronomy and Astrophysics. 353: 163–176 (2000). Bibcode:2000A&A...353..163N.
^ ^a ^b Mavridis, L. N, ed. (1974). Proceedings of the First European Astronomical Meeting Athens, September 4–9, 1972. doi:10.1007/978-3-642-65666-8. ISBN 978-3-642-65668-2.
^ ^a ^b Van Leeuwen, F.; Van Genderen, A. M.; Zegelaar, I. (1998). "Hipparcos photometry of 24 variable massive stars (α Cygni variables)". Astronomy and Astrophysics Supplement Series. 128: 117–129. Bibcode:1998A&AS..128..117V. doi:10.1051/aas:1998129.
^ Kordopatis, G.; Gilmore, G.; Steinmetz, M.; Boeche, C.; Seabroke, G. M.; Siebert, A.; Zwitter, T.; Binney, J.; De Laverny, P.; Recio-Blanco, A.; Williams, M. E. K.; Piffl, T.; Enke, H.; Roeser, S.; Bijaoui, A.; Wyse, R. F. G.; Freeman, K.; Munari, U.; Carrillo, I.; Anguiano, B.; Burton, D.; Campbell, R.; Cass, C. J. P.; Fiegert, K.; Hartley, M.; Parker, Q. A.; Reid, W.; Ritter, A.; Russell, K. S.; et al. (2013). "The Radial Velocity Experiment (RAVE): Fourth Data Release". The Astronomical Journal. 146 (5): 134. arXiv:1309.4284. Bibcode:2013AJ....146..134K. doi:10.1088/0004-6256/146/5/134. S2CID 119221010.
^ Pietrzyński, G.; Graczyk, D.; Gallenne, A.; Gieren, W.; Thompson, I. B.; Pilecki, B.; Karczmarek, P.; Górski, M.; Suchomska, K.; Taormina, M.; Zgirski, B.; Wielgórski, P.; Kołaczkowski, Z.; Konorski, P.; Villanova, S.; Nardetto, N.; Kervella, P.; Bresolin, F.; Kudritzki, R. P.; Storm, J.; Smolec, R.; Narloch, W. (2019). "A distance to the Large Magellanic Cloud that is precise to one per cent". Nature. 567 (7747): 200–203. arXiv:1903.08096. Bibcode:2019Natur.567..200P. doi:10.1038/s41586-019-0999-4. PMID 30867610. S2CID 76660316.
^ Bresolin, Fabio (2003). "Blue Supergiants as a Tool for Extragalactic Distances — Empirical Diagnostics". Stellar Candles for the Extragalactic Distance Scale. Lecture Notes in Physics. Vol. 635. pp. 149–174. arXiv:astro-ph/0301179. Bibcode:2003LNP...635..149B. doi:10.1007/978-3-540-39882-0_8. ISBN 978-3-540-20128-1. S2CID 9978035.
^ Yungelson, L. R.; Van Den Heuvel, E. P. J.; Vink, Jorick S.; Portegies Zwart, S. F.; De Koter, A. (2008). "On the evolution and fate of super-massive stars". Astronomy and Astrophysics. 477 (1): 223–237. arXiv:0710.1181. Bibcode:2008A&A...477..223Y. doi:10.1051/0004-6361:20078345. S2CID 18269577.
^ ^a ^b ^c ^d Georgy, Cyril; Saio, Hideyuki; Meynet, Georges (2021-06-01). "Blue supergiants as tests for stellar physics". Astronomy & Astrophysics. 650: A128. arXiv:2104.06278. Bibcode:2021A&A...650A.128G. doi:10.1051/0004-6361/202040105. ISSN 0004-6361.
^ Dorn-Wallenstein, Trevor; Levesque, Emily; Davenport, James; Neugent, Kathryn; Morris, Brett; Bostroem, K. Azalee (2023-01-01), "The Properties of Fast Yellow Pulsating Supergiants: FYPS Point the Way to Missing Red Supergiants", American Astronomical Society Meeting Abstracts, 241: 452.01, arXiv:2206.11917, Bibcode:2023AAS...24145201D, doi:10.3847/1538-4357/ac79b2
^ Van Genderen, A. M. (1974). "A Probable Periodicity in the Light Variation of the LMC Supergiant HD 33579". Information Bulletin on Variable Stars. 877: 1. Bibcode:1974IBVS..877....1V.
^ Van Genderen, A. M. (1979). "Long time baseline VBLUW photometry of four of the most luminous LMC supergiants HD 33579, HD 35343=S Dor, HDE 268757 and HDE 269006. I". Astronomy and Astrophysics Supplement Series. 38: 151. Bibcode:1979A&AS...38..151V.
^ Grieve, G. R.; Madore, B. F.; Welch, D. L. (1985). "Leavitt variables—Bright variable supergiants and their implications for the distance scale". Astrophysical Journal. 294: 513. Bibcode:1985ApJ...294..513G. doi:10.1086/163318.
^ Koen, Chris; Eyer, Laurent (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. S2CID 10505995.