Eta Boötis

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Eta Boötis
Diagram showing star positions and boundaries of the Boötes constellation and its surroundings
Cercle rouge 100%.svg

Location of η Boötis
Observation data
Epoch J2000      Equinox J2000
Constellation Boötes
Right ascension 13h 54m 41.07892s[1]
Declination +18° 23′ 51.7946″[1]
Apparent magnitude (V) 2.680[2]
Characteristics
Spectral type G0 IV[3]
U−B color index +0.207[4]
B−V color index +0.585[4]
R−I color index 0.2
Astrometry
Radial velocity (Rv) -1.6[2] km/s
Proper motion (μ) RA: -60.95[1] mas/yr
Dec.: -356.29[1] mas/yr
Parallax (π) 87.75 ± 1.24[1] mas
Distance 37.2 ± 0.5 ly
(11.4 ± 0.2 pc)
Absolute magnitude (MV) 2.41[2]
Details
Mass 1.71 ± 0.05[5] M
Radius 2.672 ± 0.028[5] R
Luminosity 8.89 ± 0.16[5] L
Surface gravity (log g) 3.817 ± 0.015[5] cgs
Temperature 6,100 ± 28[5] K
Metallicity [Fe/H] 0.27[2] dex
Rotational velocity (v sin i) 11.8[6] km/s
Age 2.7[3] Gyr
Other designations
Muphrid, Mufride, Muphride, Mufrid, Saak, 8 Boötis, Gl 534, HR 5235, BD +19°2725, HD 121370, LTT 14060, GCTP 3175.00, SAO 100766, FK5 513, HIP 67927.
Data sources:
Hipparcos Catalogue,
CCDM (2002),
Bright Star Catalogue (5th rev. ed.)

Eta Boötis (η Boo, η Boötis) is a star in the constellation Boötes. It has the traditional names Muphrid and Saak,[7] and the Flamsteed designation 8 Boötis. Since 1943, the spectrum of this star has served as one of the stable anchor points by which other stars are classified.[8]

The name Muphrid is from the Arabic مفرد الرامح mufrid ar-rāmiħ "the (single) one of the lancer".[9] In Chinese, 右攝提 (Yòu Niè Dī), meaning "the Right Conductor", refers to an asterism consisting of Eta Boötis, Tau Boötis and Upsilon Boötis.[10] Consequently, Eta Boötis itself is known as 右攝提一 (Yòu Niè Dī yī, English: the First Star of the Right Conductor.)[11] In the catalogue of stars in the Calendarium of Al Achsasi al Mouakket, this star was designated Ramih al Ramih (رمح الرامح - rumḥ al rāmiḥ), which was translated into Latin as Lancea Lanceator, possibly meaning the lance of the lancer.[12]

This star is a subgiant that has begun the process of evolving from a main sequence star into a red giant. It has about 1.7 times the mass of the Sun and 2.7 times the Sun's radius. The estimated age of this star is about 2.7 billion years.[3] Based on its spectra, Eta Boötis has a significant excess of elements heavier than helium.[2] In fact the ratio of iron to hydrogen is considered close to the upper limit for dwarf stars in the galactic disk.[citation needed] The star is a suspected spectroscopic binary with a reported period of 494 days, but the companion was not confirmed through speckle interferometry. This measurement does not rule out a low mass stellar companion of spectral class M7.[5]

Eta Boötis appears close to the prominent star Arcturus (Alpha Bootis) in Earth's sky, and Arcturus is in fact its closest stellar neighbor, as both stars are nearly identical in distance from the Sun. The two stars are about 3.24 light years apart [1], and each would appear bright in the other's sky. Arcturus would appear as roughly magnitude -5.2 (about 120 times brighter than it appears from Earth, or close to twice the brightness of Venus) in the night sky of a hypothetical planet orbiting Eta Boötis, while Eta Boötis would appear at about magnitude -2.5 in the sky of a hypothetical planet orbiting Arcturus, or over twice the brightness of Sirius in our night sky.[citation needed]

See also[edit]

References[edit]

  1. ^ a b c d e van Leeuwen, Floor (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, arXiv:0708.1752v1, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357  Note: see VizieR catalogue I/311.
  2. ^ a b c d e Holmberg, J.; Nordström, B.; Andersen, J. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics 501 (3): 941–947, arXiv:0811.3982, Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191 
  3. ^ a b c Thévenin, F. et al. (June 2005), "VLTI/VINCI diameter constraints on the evolutionary status of δ Eri, ξ Hya, η Boo", Astronomy and Astrophysics 436 (1): 253–262, arXiv:astro-ph/0501420, Bibcode:2005A&A...436..253T, doi:10.1051/0004-6361:20042075 
  4. ^ a b Oja, T., "UBV photometry of stars whose positions are accurately known. III", Astronomy and Astrophysics Supplement Series 65 (2): 405–4 
  5. ^ a b c d e f van Belle, Gerard T.; Ciardi, David R.; Boden, Andrew F. (March 2007), "Measurement of the Surface Gravity of η Bootis", The Astrophysical Journal 657 (2): 1058–1063, arXiv:astro-ph/0701120, Bibcode:2007ApJ...657.1058V, doi:10.1086/510830 
  6. ^ Schröder, C.; Reiners, J. H. M. M.; Schmitt (January 2009), "Ca II HK emission in rapidly rotating stars. Evidence for an onset of the solar-type dynamo", Astronomy and Astrophysics 493 (3): 1099–1107, Bibcode:2009A&A...493.1099S, doi:10.1051/0004-6361:200810377 
  7. ^ Rumrill, H. B. (June 1936), "Star Name Pronunciation", Publications of the Astronomical Society of the Pacific 48 (283): 139–154, Bibcode:1936PASP...48..139R, doi:10.1086/124681  See p. 150.
  8. ^ Garrison, R. F. (December 1993), "Anchor Points for the MK System of Spectral Classification", Bulletin of the American Astronomical Society 25: 1319, Bibcode:1993AAS...183.1710G, retrieved 2012-02-04 
  9. ^ Cannon, Garland Hampton (1994), The Arabic contributions to the English language: an historical dictionary, Otto Harrassowitz Verlag, p. 264, ISBN 3-447-03491-2 
  10. ^ (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.
  11. ^ (Chinese) 香港太空館 - 研究資源 - 亮星中英對照表, Hong Kong Space Museum. Accessed on line November 23, 2010.
  12. ^ Knobel, E. B. (June 1895), "Al Achsasi Al Mouakket, on a catalogue of stars in the Calendarium of Mohammad Al Achsasi Al Mouakket", Monthly Notices of the Royal Astronomical Society 55: 429, Bibcode:1895MNRAS..55..429K 

External links[edit]