A binary pair designated Zeta1 Cancri or, alternatively, Zeta Cancri AB, the two components of which are themselves designated Zeta1 Cancri A or, simply, Zeta Cancri A (formally also named Tegmine/ˈtɛɡmɪniː/, the traditional name of the Zeta Cancri system)[2] and Zeta1/Zeta Cancri B.
A triple star system designated Zeta2 Cancri or alternatively Zeta Cancri C, consisting of a single star primary, designated Zeta2/Zeta Cancri Ca, together with a secondary binary pair, designated Zeta2/Zeta Cancri Cb. The binary pair's two components are themselves designated Zeta2/Zeta Cancri Cb1 and Cb2.
ζ Cancri (Latinised to Zeta Cancri) is the system's Bayer designation; ζ1 Cancri and ζ2 Cancri those of its two constituents. The designations of the two constituents as ζ Cancri AB and C, and those of their components—ζ Cancri A, B, Ca, Cb, Cb1 and Cb2—derive from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).[3]
Considerable confusion had developed concerning the catalogue identities of the three bright stars; correct correspondences were worked out by Griffin:[4]
Zeta Cancri bore the traditional name Tegmine (Tegmen) "the shell (of the crab)".[citation needed] In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[5] to catalogue and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems.[6] It approved the name Tegmine for the component Zeta1 Cancri A on 12 September 2016 and it is now so included in the List of IAU-approved Star Names.[2]
Zeta Cancri can be resolved as a binary star in small telescopes. Its binary nature was discovered in 1756 by Tobias Mayer. William Herschel resolved the two components that make up Zeta1 Cancri in 1781. As early as 1831, John Herschel noticed perturbations in Zeta2 Cancri's orbit around Zeta1; this led Otto Wilhelm von Struve, in 1871, to postulate a fourth, unseen, component which orbited closely the visible member of Zeta2.[4] Later observations have resolved this fourth component and have indicated that there may be one or two more unobserved components.[9][10]
Zeta1 and Zeta2 Cancri are 5.06 arcseconds apart. These two star systems orbit around their common centre of mass once every 1,100 years.
Zeta1 Cancriedit
The two components are both yellow-white main-sequence dwarfs of spectral class F. The apparent magnitudes of A and B are +5.58 and +5.99, respectively. They are separated, as of 2008, by 1 arcsecond, requiring a large telescope to resolve them, but this separation will increase until the year 2020. They complete one orbit every 59.6 years.[11] The estimated masses for the pair are 1.28 and 1.18 solar masses, respectively.
Zeta2 Cancriedit
Zeta Cancri Ca is the brightest of the three components, having an apparent magnitude of +6.12. It appears to be a yellow G-type star, often reported as G5V, but now thought to be earlier, probably G0V. This star has around 1.15 solar masses.[12] The tenth magnitude Zeta Cancri Cb is a close pair of red dwarfs. The separation between Ca and Cb is approximately 0.3 arcsecond, and their orbital period is 17 years.
Referencesedit
^. Multiple Star Catalog. Archived from the original on 2018-02-18. Retrieved 2018-02-18.
^ ab"Naming Stars". IAU.org. Retrieved 16 December 2017.
^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].
^ abGriffin, R. F. (2000). "Spectroscopic Binary Orbits from Photoelectrical Radial Velocities: Paper 150: ζ Cancri C". The Observatory. 120: 1–47. Bibcode:2000Obs...120....1G.
^"WG Triennial Report (2015-2018) - Star Names" (PDF). p. 5. Retrieved 2018-07-14.
^(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, ISBN978-986-7332-25-7.
^(in Chinese) 香港太空館 - 研究資源 - 亮星中英對照表 August 19, 2010, at the Wayback Machine, Hong Kong Space Museum. Accessed on line November 23, 2010.
^Hutchings, J. B.; Griffin, R. F.; Menard, F. (2000). "Direct observation of the fourth star in the Zeta Cancri system". Publications of the Astronomical Society of the Pacific (abstract). 112 (772): 833–836. arXiv:astro-ph/0004284. Bibcode:2000PASP..112..833H. doi:10.1086/316587. S2CID 119361568.
^Richichi, A. (2000). "An Investigation of the multiple star Zet Cnc by a lunar occultation". Astronomy & Astrophysics. 364: 225–231. Bibcode:2000A&A...364..225R.
^Mason; Hartkopf, William I.; Wycoff, Gary L.; Holdenried, Ellis R. (2006). "Speckle Interferometry at the US Naval Observatory. XII". The Astronomical Journal. 132 (5): 2219–2230. Bibcode:2006AJ....132.2219M. doi:10.1086/508231.
zeta, cancri, cancri, abbreviated, zeta, multiple, star, system, constellation, cancer, approximately, light, years, from, earth, combined, apparent, magnitude, since, near, ecliptic, occulted, moon, very, rarely, planets, cancri, clocation, cancri, circled, o. Zeta Cancri z Cancri abbreviated Zeta Cnc z Cnc is a multiple star system in the constellation of Cancer It is approximately 83 4 light years from Earth and has a combined apparent magnitude of 4 67 Since it is near the ecliptic it can be occulted by the Moon and very rarely by planets z Cancri A B CLocation of z Cancri circled Observation dataEpoch J2000 0 Equinox J2000 0 Constellation Cancer Right ascension 08h 12m 12 7s Declination 17 38 52 Apparent magnitude V 5 58 5 99 6 12 Characteristics Evolutionary stage main sequence star Spectral type F7V F9V G0V Other designationsTegmen Tegmine 16 Cancri HR 3208 3209 3210 HD 68257 68255 68256 BD 18 1867 HIP 40167 SAO 97645 97646 GC 11142 11141 ADS 6650 CCDM J08123 1738 WDS 08122 1739 The system is constituted as follows 1 A binary pair designated Zeta1 Cancri or alternatively Zeta Cancri AB the two components of which are themselves designated Zeta1 Cancri A or simply Zeta Cancri A formally also named Tegmine ˈ t ɛ ɡ m ɪ n iː the traditional name of the Zeta Cancri system 2 and Zeta1 Zeta Cancri B A triple star system designated Zeta2 Cancri or alternatively Zeta Cancri C consisting of a single star primary designated Zeta2 Zeta Cancri Ca together with a secondary binary pair designated Zeta2 Zeta Cancri Cb The binary pair s two components are themselves designated Zeta2 Zeta Cancri Cb1 and Cb2 Contents 1 Nomenclature 2 Properties 2 1 Zeta1 Cancri 2 2 Zeta2 Cancri 3 ReferencesNomenclature editz Cancri Latinised to Zeta Cancri is the system s Bayer designation z1 Cancri and z2 Cancri those of its two constituents The designations of the two constituents as z Cancri AB and C and those of their components z Cancri A B Ca Cb Cb1 and Cb2 derive from the convention used by the Washington Multiplicity Catalog WMC for multiple star systems and adopted by the International Astronomical Union IAU 3 Considerable confusion had developed concerning the catalogue identities of the three bright stars correct correspondences were worked out by Griffin 4 Component HR HD SAO HIP z Cancri A 3208 68257 97645 40167 z Cancri B 3209 68255 z Cancri C 3210 68256 97646 Zeta Cancri bore the traditional name Tegmine Tegmen the shell of the crab citation needed In 2016 the International Astronomical Union organized a Working Group on Star Names WGSN 5 to catalogue and standardize proper names for stars The WGSN decided to attribute proper names to individual stars rather than entire multiple systems 6 It approved the name Tegmine for the component Zeta1 Cancri A on 12 September 2016 and it is now so included in the List of IAU approved Star Names 2 In Chinese 水位 Shuǐ Wei meaning Water Level refers to an asterism consisting of Zeta Cancri 6 Canis Minoris 11 Canis Minoris and 8 Cancri 7 Consequently Zeta Cancri itself is known as 水位四 Shuǐ Wei si English the Fourth Star of Water Level 8 Properties editZeta Cancri can be resolved as a binary star in small telescopes Its binary nature was discovered in 1756 by Tobias Mayer William Herschel resolved the two components that make up Zeta1 Cancri in 1781 As early as 1831 John Herschel noticed perturbations in Zeta2 Cancri s orbit around Zeta1 this led Otto Wilhelm von Struve in 1871 to postulate a fourth unseen component which orbited closely the visible member of Zeta2 4 Later observations have resolved this fourth component and have indicated that there may be one or two more unobserved components 9 10 Zeta1 and Zeta2 Cancri are 5 06 arcseconds apart These two star systems orbit around their common centre of mass once every 1 100 years Zeta1 Cancri edit The two components are both yellow white main sequence dwarfs of spectral class F The apparent magnitudes of A and B are 5 58 and 5 99 respectively They are separated as of 2008 by 1 arcsecond requiring a large telescope to resolve them but this separation will increase until the year 2020 They complete one orbit every 59 6 years 11 The estimated masses for the pair are 1 28 and 1 18 solar masses respectively Zeta2 Cancri edit Zeta Cancri Ca is the brightest of the three components having an apparent magnitude of 6 12 It appears to be a yellow G type star often reported as G5V but now thought to be earlier probably G0V This star has around 1 15 solar masses 12 The tenth magnitude Zeta Cancri Cb is a close pair of red dwarfs The separation between Ca and Cb is approximately 0 3 arcsecond and their orbital period is 17 years References edit Displaying next number in catalog HIP gt 40167 Multiple Star Catalog Archived from the original on 2018 02 18 Retrieved 2018 02 18 a b Naming Stars IAU org Retrieved 16 December 2017 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 a b Griffin R F 2000 Spectroscopic Binary Orbits from Photoelectrical Radial Velocities Paper 150 z Cancri C The Observatory 120 1 47 Bibcode 2000Obs 120 1G IAU Working Group on Star Names WGSN International Astronomical Union retrieved 22 May 2016 WG Triennial Report 2015 2018 Star Names PDF p 5 Retrieved 2018 07 14 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 in Chinese 香港太空館 研究資源 亮星中英對照表 Archived August 19 2010 at the Wayback Machine Hong Kong Space Museum Accessed on line November 23 2010 Hutchings J B Griffin R F Menard F 2000 Direct observation of the fourth star in the Zeta Cancri system Publications of the Astronomical Society of the Pacific abstract 112 772 833 836 arXiv astro ph 0004284 Bibcode 2000PASP 112 833H doi 10 1086 316587 S2CID 119361568 Richichi A 2000 An Investigation of the multiple star Zet Cnc by a lunar occultation Astronomy amp Astrophysics 364 225 231 Bibcode 2000A amp A 364 225R Mason Hartkopf William I Wycoff Gary L Holdenried Ellis R 2006 Speckle Interferometry at the US Naval Observatory XII The Astronomical Journal 132 5 2219 2230 Bibcode 2006AJ 132 2219M doi 10 1086 508231 Fuhrmann Klaus February 2008 Nearby stars of the Galactic disc and halo IV Monthly Notices of the Royal Astronomical Society 384 1 173 224 Bibcode 2008MNRAS 384 173F doi 10 1111 j 1365 2966 2007 12671 x Retrieved from https en wikipedia org w index php title Zeta Cancri amp oldid 1203048912, wikipedia, wiki, book, books, library,
