Jump to content

Beta Ceti

Coordinates: Sky map 00h 43m 35.37090s, −17° 59′ 11.7827″
From Wikipedia, the free encyclopedia
β Ceti / Diphda
Location of β Ceti (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Cetus
Right ascension 00h 43m 35.37090s[1]
Declination −17° 59′ 11.7827″[1]
Apparent magnitude (V) 2.02[2]
Characteristics
Evolutionary stage Red clump (helium-burning)[3]
Spectral type K0 III[4]
U−B color index +0.88[2]
B−V color index +1.01[2]
Variable type Suspected[5]
Astrometry
Radial velocity (Rv)+12.9[6] km/s
Proper motion (μ) RA: +232.55 mas/yr[1]
Dec.: +31.99 mas/yr[1]
Parallax (π)33.86 ± 0.16 mas[1]
Distance96.3 ± 0.5 ly
(29.5 ± 0.1 pc)
Absolute magnitude (MV)−0.13[7]
Details
Mass3.5[8] M☉
Radius17.52±0.47[9] R☉
Luminosity149.7±3.4[9] L☉
Surface gravity (log g)2.43±0.07[9] cgs
Temperature4,792±35[10] K
Metallicity [Fe/H]−0.09[11] dex
Rotational velocity (v sin i)18[12] km/s
Age460±130[9] Myr
Other designations
Diphda, Deneb Kaitos, Difda al Thani, Rana Secunda, 16 Cet, BD–18°115, GCTP 134.00, Gj 31, HD 4128, HIP 3419, HR 188, SAO 147420[13]
Database references
SIMBADdata
ARICNSdata

Beta Ceti (β Ceti, abbreviated Beta Cet, β Cet), officially named Diphda /ˈdɪfdə/,[14] is the brightest star in the constellation of Cetus. Although designated 'beta', it is actually brighter than the 'alpha' star in the constellation, Menkar, by half a magnitude. This orange giant is easy to identify due to its location in an otherwise dark section of the celestial sphere. Based on parallax measurements, it lies at an estimated distance of 96.3 light-years (29.5 parsecs) from the Sun.[1]

Properties

[edit]
Image of orange giant Beta Ceti from NASA's Chandra X-ray Observatory.
An extreme ultraviolet light curve for Beta Ceti, adapted from Ayres et al. (2001)[3]


Diphda has an apparent visual magnitude of 2.02,[2] making it the brightest star in Cetus. It has a stellar classification of K0 III,[4] although some sources list a classification of G9.5 III[15] indicating that it lies along the dividing line separating G-type from K-type stars. The luminosity class 'III' means that it is a giant, a star that has consumed the hydrogen at its core and evolved away from the main sequence. With a mass of 3.5 solar masses, Beta Ceti was a B-type star when it formed on the main sequence.[8] After passing through the red giant stage, it underwent a helium flash event and is now a red clump star generating energy through the thermonuclear fusion of helium at its core.[3] Beta Ceti will remain in this mode for over 100 million years.[16]

The effective temperature of the star's outer envelope is about 4,797 K,[11] giving it the characteristic orange hue of a K-type star.[17] In spite of its cooler temperature, Diphda is much more luminous than the Sun with a luminosity of about 150 times that of the Sun, while its photosphere has swollen to around 18[9] times the size of the Sun, in contrast with the initial radius of 2.02 R☉ when still in the main sequence.[8]

This star displays flaring activity that results in random outbursts that increase the luminosity of the star over intervals lasting several days. This is a much longer duration than for comparable solar flare activity on the Sun, which typically last for periods measured in hours.[3] In 2005, a relatively high rate of X-ray emission was detected with the XMM-Newton space observatory.[15] It is emitting about 2,000 times the X-ray luminosity of the Sun, allowing the star to be imaged with the Chandra X-ray Observatory.[16]

Nomenclature

[edit]

β Ceti (Latinised to Beta Ceti) is the star's Bayer designation.

It bore the traditional names Diphda and Deneb Kaitos /ˌdɛnɛb ˈkeɪtɒs/.[18] Diphda is Arabic for 'frog', from the phrase ضفدع الثاني aḍ-ḍifdaʿ aṯ-ṯānī 'the second frog' (the first frog' is Fomalhaut); Deneb Kaitos is from الذنب القيتوس الجنوب Al Dhanab al Ḳaiṭos al Janūbīyy 'southern tail of Cetus'.[19]

In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[20] to catalogue and standardize proper names for stars. The WGSN approved the name Diphda for this star on 21 August 2016 and it is now so entered in the IAU Catalog of Star Names.[21]

In Chinese astronomy, Deneb Kaitos is called 土司空, Pinyin: Tǔsīkōng, meaning Master of Constructions, because this star is marking itself and stands alone in the Master of Constructions asterism, Legs mansion (see : Chinese constellation).[22] 土司空 (Tǔsīkōng), westernized into Too Sze Kung by R.H. Allen and the meaning is "Superintendent of Earthworks."[23]

Namesake

[edit]

USS Diphda (AKA-59) was a U.S. Navy ship.

See also

[edit]

References

[edit]
  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 c d Johnson, H. L.; et al. (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Laboratory. 4 (99): 99. Bibcode:1966CoLPL...4...99J.
  3. ^ a b c d Ayres, Thomas R.; Osten, Rachel A.; Brown, Alexander (November 2001). "3 Ms in the Life of β Ceti: Sustained Flare Activity on a Clump Giant Detected by the Extreme Ultraviolet Explorer". The Astrophysical Journal. 562 (1): L83 – L86. Bibcode:2001ApJ...562L..83A. doi:10.1086/337971.
  4. ^ a b Montes, D.; et al. (November 2001). "Late-type members of young stellar kinematic groups - I. Single stars". Monthly Notices of the Royal Astronomical Society. 328 (1): 45–63. arXiv:astro-ph/0106537. Bibcode:2001MNRAS.328...45M. doi:10.1046/j.1365-8711.2001.04781.x. S2CID 55727428.
  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. ^ Elgarøy, Øystein; Engvold, Oddbjørn; Lund, Niels (March 1999). "The Wilson-Bappu effect of the MgII K line - dependence on stellar temperature, activity and metallicity". Astronomy and Astrophysics. 343: 222–228. Bibcode:1999A&A...343..222E.
  8. ^ a b c Tsvetkova, S.; Petit, P.; Aurière, M.; Konstantinova-Antova, R.; Wade, G. A.; Charbonnel, C.; Decressin, T.; Bogdanovski, R. (2013-08-01). "Magnetic field structure in single late-type giants: β Ceti in 2010–2012". Astronomy & Astrophysics. 556: A43. arXiv:1301.1592. doi:10.1051/0004-6361/201321051. ISSN 0004-6361.
  9. ^ a b c d e Reffert, Sabine; Bergmann, Christoph; Quirrenbach, Andreas; Trifonov, Trifon; Künstler, Andreas (2015-02-01). "Precise radial velocities of giant stars. VII. Occurrence rate of giant extrasolar planets as a function of mass and metallicity". Astronomy and Astrophysics. 574: A116. arXiv:1412.4634. Bibcode:2015A&A...574A.116R. doi:10.1051/0004-6361/201322360. ISSN 0004-6361. Beta Ceti's database entry at VizieR.
  10. ^ Luck, R. Earle (25 August 2015). "Abundances in the Local Region. I. G and K Giants". The Astronomical Journal. 150 (3): 88. arXiv:1507.01466. Bibcode:2015AJ....150...88L. doi:10.1088/0004-6256/150/3/88.
  11. ^ a b Massarotti, Alessandro; et al. (January 2008). "Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity". The Astronomical Journal. 135 (1): 209–231. Bibcode:2008AJ....135..209M. doi:10.1088/0004-6256/135/1/209.
  12. ^ "Bright Star Catalogue, 5th Revised Ed. (Hoffleit+, 1991)". VizieR. Centre de Données astronomiques de Strasbourg. Retrieved 2010-09-30.
  13. ^ "bet Cet -- Variable Star". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2010-09-30.
  14. ^ "International Astronomical Union | IAU". www.iau.org. Retrieved 2022-06-15.
  15. ^ a b Sägesser, S. N.; Jordan, C. (March 2005). "Emission measures for the single giant β Ceti". In Favata, F.; Hussain, G. A. J.; Battrick, B. (eds.). Proceedings of the 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun, held 5–9 July 2004 in Hamburg, Germany. European Space Agency. p. 931. Bibcode:2005ESASP.560..931S.
  16. ^ a b "Beta Ceti: Giant Star's Corona Brightens with Age". Chandra Photo Album. Harvard-Smithsonian Center for Astrophysics. February 20, 2009. Retrieved 2011-12-28.
  17. ^ "The Colour of Stars". Australia Telescope, Outreach and Education. Commonwealth Scientific and Industrial Research Organisation. December 21, 2004. Archived from the original on 2012-03-18. Retrieved 2012-01-16.
  18. ^ Kunitzsch, Paul; Smart, Tim (2006). A Dictionary of Modern star Names: A Short Guide to 254 Star Names and Their Derivations (2nd rev. ed.). Cambridge, Massachusetts: Sky Pub. ISBN 978-1-931559-44-7.
  19. ^ Allen, Richard H. (1963). Star Names: Their Lore and Meaning (Reprint ed.). New York: Dover Publications Inc. p. 163. ISBN 0-486-21079-0. Retrieved 2010-12-12.
  20. ^ "IAU Working Group on Star Names (WGSN)". International Astronomical Union. Retrieved 22 May 2016.
  21. ^ "IAU Catalog of Star Names". Retrieved 28 July 2016.
  22. ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 9 日 Archived 2011-05-22 at the Wayback Machine
  23. ^ Star Name - R.H. Allen p. 160
[edit]
Retrieved from "https://en.wikipedia.org/w/index.php?title=Beta_Ceti&oldid=1257474470"