Star in the constellation Cancer
27 Cancri |
Observation data
Epoch J2000.0 Equinox J2000.0 |
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| Constellation | Cancer |
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| Right ascension | 08h 26m 43.94035s[2] |
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| Declination | +12° 39′ 16.6066″[2] |
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| Apparent magnitude (V) | +5.56[3] |
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| Characteristics |
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| Evolutionary stage | Asymptotic giant branch[4] |
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| Spectral type | M3 IIIa[5] |
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| B−Vcolor index | 1.608±0.002[3] |
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| Variable type | SRb[4] |
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| Astrometry |
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|
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| Radial velocity (Rv) | −8.30±0.31[6] km/s |
| Proper motion (μ) | RA: −19.760[2]mas/yr
Dec.: −104.664[2]mas/yr |
| Parallax (π) | 3.3094±0.3176 mas[2] |
| Distance | 990 ± 90 ly
(300 ± 30 pc) |
| Absolute magnitude (MV) | −1.62[3] |
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| Details |
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|
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| Radius | 119[2] R☉ |
| Luminosity | 2,455+707
−550[7] L☉ |
| Surface gravity (log g) | 1.00[7] cgs |
| Temperature | 3,574[7] K |
| Metallicity[Fe/H] | 0.00[7] dex |
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| Other designations |
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| 27 Cnc,BP Cancri,AAVSO 0821+13,BD+13°1912,FK5 2658,GC 11525,HD 71250,HIP 41400,HR 3319,SAO 97819[8] |
| Database references |
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| SIMBAD | data |
27 Cancri is a single[9]star in thezodiacconstellation ofCancer, located around 990 light-years away from theSun.[2] It is visible to thenaked eye as a faint, red-hued star with a typicalapparent visual magnitude of around +5.56.[3] The star is moving closer to the Earth with a heliocentricradial velocity of −8.3 km/s.[6] It is a member of theArcturus stream, a group of stars with high proper motion and metal-poor properties thought to be the remnants of a small galaxy consumed by theMilky Way.[10]
Thevariability of the brightness of 27 Cancri was announced byJoel Stebbins andCharles Morse Huffer in 1928, based on observations made atWashburn Observatory.[11] It was given itsvariable star designation, BP Cancri, in 1977.[12]
This is an agingred giant with astellar classification of M3 IIIa,[5] currently on theasymptotic giant branch.[4] It is classified as asemiregular variable star of type SRb and its brightness varies from magnitude +5.41 to +5.75 with a period of 40 days.[13] The star is radiating around 2,455[7] times theSun's luminosity from its enlargedphotosphere at aneffective temperature of 3,574 K.[7]
- ^EAS (1997)."The HIPPARCOS and TYCHO catalogues".Astrometric and Photometric Star Catalogues Derived from the ESA Hipparcos Space Astrometry Mission. ESA SP Series.1200. Noordwijk, Netherlands: ESA Publications Division.Bibcode:1997HIP...C......0E.ISBN 9290923997. Retrieved7 December 2024.
- ^abcdefgBrown, 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 atVizieR.
- ^abcdAnderson, 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.
- ^abcLebzelter, T.; Hron, J. (December 2003), "Technetium and the third dredge up in AGB stars. I. Field stars",Astronomy and Astrophysics,411 (3):533–542,arXiv:astro-ph/0310018,Bibcode:2003A&A...411..533L,doi:10.1051/0004-6361:20031458,S2CID 18879265.
- ^abKeenan, Philip C.; McNeil, Raymond C. (1989), "The Perkins catalog of revised MK types for the cooler stars",Astrophysical Journal Supplement Series,71: 245,Bibcode:1989ApJS...71..245K,doi:10.1086/191373,S2CID 123149047.
- ^abde Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project",Astronomy & Astrophysics,546: 14,arXiv:1208.3048,Bibcode:2012A&A...546A..61D,doi:10.1051/0004-6361/201219219,S2CID 59451347, A61.
- ^abcdefMaas, Z. G.; et al. (December 2016), "Chlorine Abundances in Cool Stars",The Astronomical Journal,152 (6): 14,arXiv:1609.01626,Bibcode:2016AJ....152..196M,doi:10.3847/0004-6256/152/6/196,S2CID 118722950, 196.
- ^"27 Cnc".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved2019-02-26.
- ^Eggleton, P. P.; Tokovinin, A. A. (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.
- ^Eggen, Olin (1971), "The Arcturus Group",Publications of the Astronomical Society of the Pacific,83 (493):271–85,Bibcode:1971PASP...83..271E,doi:10.1086/129120.
- ^Stebbins, Joel; Huffer, C. M. (1928)."The Constancy of the Light of Red Stars".Publications of the Washburn Observatory.15:137–174.Bibcode:1928PWasO..15..137S. Retrieved5 December 2024.
- ^Kukarkin, B. V.; Kholopov, P. N.; Kukarkina, N. P.; Perova, N. B. (October 1973)."59th Name-List of Variable Stars"(PDF).Information Bulletin on Variable Stars.834:1–22.Bibcode:1973IBVS..834....1K. Retrieved8 December 2024.
- ^Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars",Astronomy Reports, 5.1,61 (1):80–88,Bibcode:2017ARep...61...80S,doi:10.1134/S1063772917010085,S2CID 125853869.
