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Zeta Geminorum

Coordinates: Sky map 07h 04m 06.53079s, 20° 34′ 13.0739″
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ζ Geminorum
Location of ζ Geminorum (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Gemini
Right ascension 07h 04m 06.53079s[1]
Declination +20° 34′ 13.0739″[1]
Apparent magnitude (V) 3.93 (3.68 to 4.16)[2]
Characteristics
Spectral type F7Ib to G3Ib[3]
U−B color index +0.55[4]
B−V color index 0.88[4]
Variable type Classical Cepheid[5]
Astrometry
Radial velocity (Rv)+6.7[6] km/s
Proper motion (μ) RA: −7.29[1] mas/yr
Dec.: −0.41[1] mas/yr
Parallax (π)2.78 ± 0.18 mas[7]
Distance1,120 ly
(368[8] pc)
Absolute magnitude (MV)-3.99[9]
Details
Mass7.7 ± 0.3[10] M☉
Radius72±3[11] R☉
Luminosity4,413±332[11] L☉
Surface gravity (log g)1.9[12] cgs
Temperature5,260–5,780[3] K
Metallicity [Fe/H]0.16[12] dex
Rotational velocity (v sin i)19[13] km/s
Age70 ± 25[8] Myr
Other designations
Mekbuda, ζ Gem, 43 Gem, BD+20° 1687, FK5 269, HD 52973, HIP 34088, HR 2650, SAO 79031, WDS J07041+2034A[14]
Database references
SIMBADdata

Zeta Geminorum (ζ Geminorum, abbreviated Zeta Gem, ζ Gem) is a bright star with cluster components, distant optical components and a likely spectroscopic partner in the zodiac constellation of Gemini — in its south, on the left 'leg' of the twin Pollux. It is a classical Cepheid variable star, of which over 800 have been found in our galaxy. As such its regular pulsation and luminosity (proven in its class to correspond) and its relative proximity means the star is a useful calibrator in computing the cosmic distance ladder. Based on parallax measurements, it is approximately 1,200 light-years from the Sun.[7]

Zeta Geminorum is the primary or 'A' component of a multiple star system designated WDS J07041+2034. It bears traditional name Mekbuda, usually anglicised to /mɛkˈbjuːdə/.[15][16]

Nomenclature

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ζ Geminorum (Latinised to Zeta Geminorum) is the star's Bayer designation. WDS J07041+2034 A is its designation in the Washington Double Star Catalog. The designations of the two components as WDS J03158-0849 Aa and Ab derive from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).[17]

Zeta Geminorum bore the traditional name Mekbuda, from an Arabic phrase meaning "the lion's folded paw" (Zeta and Epsilon Geminorum (Mebsuta) were the paws of a lion).[18] In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[19] to catalogue and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems.[20] It approved the name Mekbuda for the component WDS J07041+2034 Aa on 12 September 2016 and it is now so included in the List of IAU-approved Star Names.[16]

In Chinese, 井宿 (Jǐng Su), meaning Well (asterism) consists of eight stars in Gemini: Zeta, Mu, Gamma, Nu, Xi, Epsilon, 36 and Lambda.[21] Zeta is 井宿七 (Jǐng Su qī, English: the Seventh Star of Well).[22]

Observation history

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A visual band light curve for Zeta Geminorum, adapted from Kiss (1998)[23]

In 1844, German astronomer Julius Schmidt discovered that Zeta Geminorum varies in brightness with a period of about 10 days,[18] although it had been suspected of variability as early as 1790.[24] It was recognised as being related to the Cepheid class of variable stars, although was often treated as the prototype of its own class, the Geminids, because of its symmetrical light curve.[25]

In 1899, American astronomer W. W. Campbell announced the star to have a variable radial velocity.[26] (This variation was independently discovered by Russian astronomer Aristarkh Belopolsky, published in 1901.[24]) Based on his observations, Campbell later published orbital elements for the binary. However, he found that the curve departed from a keplerian orbit and even suggested that it was a triple star system to explain the irregularities.[27] The periodic variation in radial velocity of the Cepheid variables was later explained as being due to pulsations in the atmosphere of the star.[24]

The periodicity of the star is itself variable, a trend first noted by German astronomer Paul Guthnick in 1920, who suspected that the period change was the result of an orbiting companion. In 1930, Danish astronomer Axel Nielsen suggested that the change was instead the result in a steady decrease of about 3.6 seconds per year in the period.[28]

Companions

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ζ Geminorum in optical light, with the companions B, C, and D visible close by

Zeta Geminorum has three visible companions known since the 19th century and listed in the Washington Double Star Catalog as B, C, and D. More recently, a possible spectroscopic companion has been listed, further faint stars close by have been catalogued, and a diffuse cluster has been identified as including Zeta Geminorum.

The brightest nearby star, WDS J07041+2034 C, is the magnitude 7.6 HD 268518, 91.9" away when discovered in 1779 and 101.3" distant in 2008.[29] It is a foreground object, only a tenth the distance of Zeta Geminorum and a high proper motion star moving rapidly compared to the more distant stars. It is a G1 main sequence star very similar to the sun.[30]

The closest visible companion is WDS J07041+2034 D, a 12th magnitude star measured to be 67.8" away in 2008. It was 80" distant when first measured in 1905. It appears on the sky between Zeta Geminorum and component C, but is a more distant object than either.[29]

WDS J07041+2034 B is an 11th magnitude star, 76.0" distant in 1831 and 87.4" in 2008.[29] It is itself a spectroscopic binary, although little is known about the two components. The combined spectrum is of an F4 main sequence star. It is thought to be physically associated with the supergiant primary and a member of a loose cluster of stars around Zeta Geminorum.[8]

A combination of photometry, spectroscopy, and astrometry has identified 26 stars approximately 355 parsecs away, which are likely to be members of the birth cluster of Zeta Geminorum. The brightest are late B and early A giant stars such as the 7th magnitude stars HD 49381 and HD 50634, while the faintest detected cluster members are 12th magnitude class F main sequence stars including WDS J07041+2034 B.[8]

Properties

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Zeta Geminorum has been reported to be a spectroscopic binary on the basis of lunar occultation observations, but this has not been confirmed by other methods.[29]

Zeta Geminorum's primary (WDS J07041+2034 Aa) is a Classical Cepheid variable that undergoes regular, periodic variation in brightness because of radial pulsations. In the V band, the apparent magnitude varies between a high of 3.68 and a low of 4.16 (with a mean of 3.93) over a period of 10.148 days.[2] This period of variation is decreasing at the rate of 3.1 seconds per year, or 0.085 seconds per cycle.[28] The spectral classification varies between F7Ib and G3Ib over the course of a pulsation cycle. Likewise the effective temperature of the outer envelope varies between 5,780 K and 5,260 K,[3] while the radius varies from 61 to 69 times the Sun's radius.[31] On average, it is radiating about 2,900 times the luminosity of the Sun.[32]

Membership of a cluster provides independent validation of distances determined using recent Hubble Space Telescope and Hipparcos parallaxes.[7][1] This strongly constrains the star's distance: 363 ± 9(σx̄) ± 26(σ) parsecs. Zeta Geminorum is thus an important calibrator for the Cepheid period-luminosity relation used for establishing the cosmic distance ladder.[8][33][34] The Gaia Data Release 2 parallax of 2.2497±0.3006 mas suggests the distance is towards the top end of this range, and has a comparable margin of error.[35]

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 Klagyivik, P.; Szabados, L. (September 2009), "Observational studies of Cepheid amplitudes. I. Period-amplitude relationships for Galactic Cepheids and interrelation of amplitudes", Astronomy and Astrophysics, 504 (3): 959–972, arXiv:0908.3561, Bibcode:2009A&A...504..959K, doi:10.1051/0004-6361/200811464, S2CID 18283579
  3. ^ a b c Kervella, P.; et al. (March 2001), "The angular diameter and distance of the Cepheid ? Geminorum", Astronomy and Astrophysics, 367 (3): 876–883, arXiv:astro-ph/0102359, Bibcode:2001A&A...367..876K, doi:10.1051/0004-6361:20000490, S2CID 16426067
  4. ^ a b Nicolet, B. (1978), "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System", Observatory, Bibcode:1978ppch.book.....N
  5. ^ Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  6. ^ Wielen, R.; et al. (1999), "Sixth Catalogue of Fundamental Stars (FK6). Part I. Basic fundamental stars with direct solutions", Veröff. Astron. Rechen-Inst. Heidelb, 35 (35), Astronomisches Rechen-Institut Heidelberg: 1, Bibcode:1999VeARI..35....1W
  7. ^ a b c Benedict, G. Fritz; et al. (April 2007), "Hubble Space Telescope Fine Guidance Sensor Parallaxes of Galactic Cepheid Variable Stars: Period-Luminosity Relations", Astronomical Journal, 133 (4): 1810–1827, arXiv:astro-ph/0612465, Bibcode:2007AJ....133.1810B, doi:10.1086/511980, S2CID 16384267.
  8. ^ a b c d e Majaess, D.; et al. (2012), "Discovery of the Host Cluster for the Fundamental Cepheid Calibrator Zeta Geminorum", Astrophysical Journal Letters, 748 (1): L9, arXiv:1202.2363, Bibcode:2012ApJ...748L...9M, doi:10.1088/2041-8205/748/1/L9, S2CID 118833920
  9. ^ Turner, D. G. (2010). "The PL calibration for Milky Way Cepheids and its implications for the distance scale". Astrophysics and Space Science. 326 (2): 219–231. arXiv:0912.4864. Bibcode:2010Ap&SS.326..219T. doi:10.1007/s10509-009-0258-5. S2CID 119264970.
  10. ^ 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
  11. ^ a b Gallenne, A.; Mérand, A.; Kervella, P.; Pietrzyński, G.; Gieren, W.; Hocdé, V.; Breuval, L.; Nardetto, N.; Lagadec, E. (May 25, 2021). "Extended envelopes around Galactic Cepheids. V. Multi-wavelength and time-dependent analysis of IR excess". Astronomy & Astrophysics. 651: A113. arXiv:2105.12197. Bibcode:2021A&A...651A.113G. doi:10.1051/0004-6361/202140350. ISSN 0004-6361.
  12. ^ a b Mallik, Sushma V. (October 1998), "Chromospheric activity in cool stars and the lithium abundance", Astronomy and Astrophysics, 338: 623–636, Bibcode:1998A&A...338..623M
  13. ^ Uesugi, Akira; Fukuda, Ichiro (1970), "Catalogue of rotational velocities of the stars", Contributions from the Institute of Astrophysics and Kwasan Observatory, University of Kyoto, Bibcode:1970crvs.book.....U
  14. ^ "V* zet Gem -- Classical Cepheid (delta Cep type)", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2012-01-01
  15. ^ Davis, George A. (1944). "The pronunciations, derivations, and meanings of a selected list of star names". Popular Astronomy. 52: 8–30. Bibcode:1944PA.....52....8D.
  16. ^ a b "Naming Stars". IAU.org. Retrieved 24 February 2018.
  17. ^ Hessman, F. V.; Dhillon, V. S.; Winget, D. E.; Schreiber, M. R.; Horne, K.; Marsh, T. R.; Guenther, E.; Schwope, A.; Heber, U. (2010). "On the naming convention used for multiple star systems and extrasolar planets". arXiv:1012.0707 [astro-ph.SR].
  18. ^ a b Allen, Richard Hinckley (1899), "Star-names and their meanings", New York, G. E. Stechert: 235, Bibcode:1899sntm.book.....A
  19. ^ IAU Working Group on Star Names (WGSN), International Astronomical Union, retrieved 22 May 2016.
  20. ^ "WG Triennial Report (2015-2018) - Star Names" (PDF). p. 5. Retrieved 2018-07-14.
  21. ^ (in Chinese) 中國星座神話, written by 陳久金. Published by 台灣書房出版有限公司, 2005, ISBN 978-986-7332-25-7.
  22. ^ (in Chinese) 香港太空館 - 研究資源 - 亮星中英對照表 Archived January 30, 2011, at the Wayback Machine, Hong Kong Space Museum. Accessed on line November 23, 2010.
  23. ^ Kiss, Laszlo L. (July 1998). "A photometric and spectroscopic study of the brightest northern Cepheids - I. Observations". Monthly Notices of the Royal Astronomical Society. 297 (3): 825. Bibcode:1998MNRAS.297..825K. doi:10.1046/j.1365-8711.1998.01559.x.
  24. ^ a b c Henroteau, F. (1925), "A study of zeta Geminorum, I.", Publications of the Dominion Observatory Ottawa, 9: 105–116, Bibcode:1925PDO.....9..105H
  25. ^ Engle, Scott G. (2015). The Secret Lives of Cepheids: A Multi-Wavelength Study of the Atmospheres and Real-Time Evolution of Classical Cepheids (Thesis). arXiv.org. arXiv:1504.02713. Bibcode:2015PhDT........45E. doi:10.5281/zenodo.45252. S2CID 118408237.
  26. ^ Campbell, W. W. (February 1899), "The variable velocity of zeta Geminorum in the line of sight.", Astrophysical Journal, 9: 86, Bibcode:1899ApJ.....9...86C, doi:10.1086/140556
  27. ^ Campbell, W. W. (January 1901), "The motion of zeta Geminorum in the line of sight", Astrophysical Journal, 13: 90–97, Bibcode:1901ApJ....13...90C, doi:10.1086/140792
  28. ^ a b Abt, Helmut A.; Levy, Saul G. (March 1974), "Period Variation of the Cepheid Zeta Geminorum", Astrophysical Journal, 188: L75, Bibcode:1974ApJ...188L..75A, doi:10.1086/181436
  29. ^ a b c d Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal. 122 (6): 3466. Bibcode:2001AJ....122.3466M. doi:10.1086/323920.
  30. ^ 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.
  31. ^ Groenewegen, M. A. T. (November 2007), "The projection factor, period-radius relation, and surface-brightness colour relation in classical cepheids", Astronomy and Astrophysics, 474 (3): 975–981, Bibcode:2007A&A...474..975G, doi:10.1051/0004-6361:20078225
  32. ^ Mallik, Sushma V. (December 1999), "Lithium abundance and mass", Astronomy and Astrophysics, 352: 495–507, Bibcode:1999A&A...352..495M
  33. ^ de Zeeuw, P. T.; et al. (1999), "A HIPPARCOS Census of the Nearby OB Associations", Astronomical Journal, 117 (1): 354–399, arXiv:astro-ph/9809227, Bibcode:1999AJ....117..354D, doi:10.1086/300682, S2CID 16098861.
  34. ^ Majaess, D.; Turner, D.; Gieren, W. (2012), "New Evidence Supporting Cluster Membership for the Keystone Calibrator Delta Cephei", Astrophysical Journal, 747 (2): 145, arXiv:1201.0993, Bibcode:2012ApJ...747..145M, doi:10.1088/0004-637X/747/2/145, S2CID 118672744.
  35. ^ 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.
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