Beta Arietis

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Beta Arietis
Diagram showing star positions and boundaries of the Aries constellation and its surroundings
Cercle rouge 100%.svg

Location of β Arietis (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Aries
Right ascension 01h 54m 38.41099s[1]
Declination +20° 48′ 28.9133″[1]
Apparent magnitude (V) 2.655[2]
Characteristics
Spectral type A5 V[3]
U−B color index +0.170[2]
B−V color index +0.142[2]
Astrometry
Radial velocity (Rv) -1.9[4] km/s
Proper motion (μ) RA: +98.74[1] mas/yr
Dec.: -110.41[1] mas/yr
Parallax (π) 54.74 ± 0.75[1] mas
Distance 59.6 ± 0.8 ly
(18.3 ± 0.3 pc)
Absolute magnitude (MV) 1.55 ± 0.09[5]
Orbit[6]
Companion Beta Arietis B
Period (P) 106.9954 ± 0.0005 days
Semi-major axis (a) 36.1 ± 0.3 mas
Eccentricity (e) 0.903 ± 0.012
Inclination (i) 44.7 ± 1.3°
Longitude of the node (Ω) 79.1 ± 0.8°
Argument of periastron (ω)
(secondary)
209.1 ± 1.2°
Details
A
Mass 2.34 ± 0.10[6] M
Luminosity 23[6] L
Surface gravity (log g) 4.0[7] cgs
Temperature 9,000[7] K
Metallicity [Fe/H] 0.16[7] dex
Rotational velocity (v sin i) 73[8] km/s
Age 0.3[9] Gyr
B
Mass 1.34 ± 0.07[6] M
Luminosity 1.3[6] L
Other designations
Sheratan, Sharatan, Al Sharatain,[10] 6 Arietis, Gl 80, HR 553, BD +20°306, HD 11636, SAO 75012, FK5 66, HIP 8903.[11]
Database references
SIMBAD data
ARICNS data

Beta Arietis (β Ari, β Arietis) is a binary star system in the constellation Aries, marking the Ram's second horn.

Etymology

Beta Arietis has the traditional name Sheratan (or Sharatan, Sheratim),[10] and the Flamsteed designation 6 Arietis. The traditional name, in full Al Sharatan, is from the Arabic الشراطان aš-šarāţān "the two signs", a reference to the star having marked the northern vernal equinox together with Gamma Arietis several thousand years ago.[citation needed]

In Chinese, 婁宿 (Lóu Su), meaning Bond (asterism), refers to an asterism consisting of β Arietis, γ Arietis and α Arietis.[12] Consequently, β Arietis itself is known as 婁宿一 (Lóu Su yī, English: the First Star of Bond).[13]

Properties

Beta Arietis has an apparent visual magnitude of 2.66. Based on parallax measurements, it is located at a distance of 59.6 light-years (18.3 parsecs) from Earth. This is a spectroscopic binary star system consisting of a pair of stars orbiting around each other with a separation that can not currently be resolved with a conventional telescope. However, the pair have been resolved using the Mark III Stellar Interferometer at the Mount Wilson Observatory. This allows the orbital elements to be computed, as well as the individual masses of the two stars. The stars complete their highly elliptical orbit every 107 days.[6]

The primary star has a stellar classification of A5 V, which means it is an A-type main sequence star that is generating energy through the thermonuclear fusion of hydrogen in its core region.[3] The NStars project gives the star a spectral type of kA4 hA5 mA5 Va under the revised MK spectral classification system.[9] The spectrum of the secondary star has not been determined, but, based on the mass, it may have a stellar classification of F5 III–V or G0 V. It is about four magnitudes fainter than the primary; hence the energy output from the system is dominated by the primary star.[6] In a few million years, as the primary evolves toward a red giant, significant amounts of mass transfer to the secondary component is expected.[14]

The primary has been classified as a rapid rotator, with a projected rotational velocity of 73 km/s providing a lower bound on the azimuthal rotational velocity along the equator.[8] It may also be a mildly Am star, which is a class of stars that show a peculiar spectrum with strong absorption lines from various elements and deficiencies in others. In β Arietis, these absorption lines are broadened because of the Doppler effect from the rotation, making analysis of the abundance patterns difficult.[7]

This system has been examined with the Spitzer Space Telescope for the presence of an excess emission of infrared, which would indicate a disk of dust. However, no significant excess was detected.[9]

References

  1. 1.0 1.1 1.2 1.3 1.4 Lua error in Module:Citation/CS1/Identifiers at line 47: attempt to index field 'wikibase' (a nil value).
  2. 2.0 2.1 2.2 Lua error in Module:Citation/CS1/Identifiers at line 47: attempt to index field 'wikibase' (a nil value).
  3. 3.0 3.1 Lua error in Module:Citation/CS1/Identifiers at line 47: attempt to index field 'wikibase' (a nil value).
  4. Lua error in Module:Citation/CS1/Identifiers at line 47: attempt to index field 'wikibase' (a nil value).
  5. Lua error in Module:Citation/CS1/Identifiers at line 47: attempt to index field 'wikibase' (a nil value).
  6. 6.0 6.1 6.2 6.3 6.4 6.5 6.6 Lua error in Module:Citation/CS1/Identifiers at line 47: attempt to index field 'wikibase' (a nil value).
  7. 7.0 7.1 7.2 7.3 Lua error in Module:Citation/CS1/Identifiers at line 47: attempt to index field 'wikibase' (a nil value).
  8. 8.0 8.1 Lua error in Module:Citation/CS1/Identifiers at line 47: attempt to index field 'wikibase' (a nil value).
  9. 9.0 9.1 9.2 Lua error in Module:Citation/CS1/Identifiers at line 47: attempt to index field 'wikibase' (a nil value).
  10. 10.0 10.1 Allen, Richard Hinckley (1899), Star-Names and Their Meanings, New York: G. E. Stechert, pp. 81–82, retrieved 2011-12-24<templatestyles src="Module:Citation/CS1/styles.css"></templatestyles>
  11. "bet Ari -- Spectroscopic binary", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2011-12-29<templatestyles src="Module:Citation/CS1/styles.css"></templatestyles>
  12. (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.
  13. (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.
  14. Lua error in Module:Citation/CS1/Identifiers at line 47: attempt to index field 'wikibase' (a nil value).

External links