Бета -баран

β -оперативная память
	Расположение β -arietis (Circled)
Данные наблюдения ; Epoch J2000 Equinox J2000
Созвездие	Овен
Правильное восхождение	01 час 54 м 38.41099 с
Склонение	+20° 48′ 28.9133″
Apparent magnitude (V)	2.655 (2.712 + 5.789 )
Характеристики
Спектральный тип	A3V + G2V
U -B Цветовой индекс	+0.170
B - V Индекс цвета	+0.142
Астрометрия
Radial velocity (Rv)	-1.9 km/s
Proper motion (μ)	RA: +98.74 mas/yr ; Dec.: -110.41 mas/yr
Parallax (π)	55.827 ± 0.308 mas
Distance	58.4 ± 0.3 ly ; (17.91 ± 0.10 pc)
Absolute magnitude (MV)	1.382 (1.444 + 4.521)
Orbit
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	2.067±0.057 M☉
Radius	1.985 ± 0.229 R☉
Luminosity	20.9+5.4; −4.3 L☉
Surface gravity (log g)	4.0 cgs
Temperature	8,759 K
Metallicity [Fe/H]	0.16 dex
Rotational velocity (v sin i)	73 km/s
Age	447+261; −165 Myr
B
Mass	1.058±0.026 M☉
Radius	1.12 ± 0.064 R☉
Luminosity	1.29+0.16; −0.14 L☉
Temperature	5,811 K
Other designations
	Sheratan, Sharatan, Al Sharatain, 6 Arietis, Gl 80, HR 553, BD +20°306, HD 11636, SAO 75012, FK5 66, HIP 8903.
Database references
SIMBAD	data
ARICNS	data

Бета -оперативная память ( β -оперативная память , сокращенная -ari , β -ari ), официально Sheratan / ʃ ɛr ə t ar n / бета названная ^{[ 10 ]}^{[ 11 ]} второй самым ярким звездой в созвездии Овна является звездной системой и , отмечая второй рог оперативной памяти.

Номенклатура

Бета -Ариетис - звезда Bayer . Это также несет обозначение Flamsteed 6 Arietis .

Традиционное название, Шератан (или Шаратан, Шератим), ^{[ 8 ]} В полном Аль-Шаратане -от арабского الشرطان ashharaţān «Два знака», ссылка на звезду, отмечающую северное ядотворное равноденствие вместе с гамма-Ариетисом несколько тысяч лет назад. ^{[ Цитация необходима ]} В 2016 году Международный астрономический союз организовал рабочую группу по звездным именам (WGSN) ^{[ 12 ]} Каталог и стандартизировать собственные названия для звезд. WGSN одобрил имя Sheratan для этой звезды 21 августа 2016 года, и теперь оно так введено в каталоге IAU звездных имен. ^{[ 11 ]}

В Китае , 婁宿 ( lóu xiù ), что означает связь (астеризм) , относится к астеризму, состоящему из шахт, γ Arietis α -Arires и ^{[ 13 ]} Следовательно, китайское название для самого β -arietis составляет 婁宿一 ( Lóu Su Yī , английский: первая звезда Бонда ). ^[14]

Properties

Beta Arietis has an apparent visual magnitude of 2.65. Based on dynamical parallax measurements, it is located at a distance of 58.4 light-years (17.9 parsecs) from Earth.^[3] 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.^[5]

The primary star has a stellar classification of A3 V,^[3] which means it is an A-type main-sequence star that is generating energy through the thermonuclear fusion of hydrogen in its core region. The NStars project gives the star a spectral type of kA4 hA5 mA5 Va under the revised MK spectral classification system.^[15] The secondary star is a G-type main-sequence star, with a stellar classification of G2V.^[3] It is about four magnitudes fainter than the primary; hence the energy output from the system is dominated by the primary star.^[5] In a few million years, as the primary evolves toward a red giant, significant amounts of mass transfer to the secondary component is expected.^[16]

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.^[7] 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.^[6]

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.^[15]

Notes

^ Jump up to: ^a ^b Calculated, using the Stefan-Boltzmann law and the star's effective temperature and luminosity, with respect to the solar nominal effective temperature of 5,772 K: ${\sqrt {{\biggl (}{\frac {5,772}{8,759}}{\biggr )}^{4}\cdot 10^{1.32}}}=1.985\ R_{\odot }.$ ${\sqrt {{\biggl (}{\frac {5,772}{5,811}}{\biggr )}^{4}\cdot 10^{0.11}}}=1.12\ R_{\odot }.$

References

^ Jump up to: ^a ^b ^c ^d 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
^ Jump up to: ^a ^b ^c Gutierrez-Moreno, Adelina; et al. (1966). "A System of photometric standards". Publications of the Department of Astronomy University of Chile. 1. Publicaciones Universidad de Chile, Department de Astronomy: 1–17. Bibcode:1966PDAUC...1....1G.
^ Jump up to: ^a ^b ^c ^d ^e ^f ^g ^h Piccotti, Luca; Docobo, José Ángel; Carini, Roberta; Tamazian, Vakhtang S.; Brocato, Enzo; Andrade, Manuel; Campo, Pedro P. (2020-02-01). "A study of the physical properties of SB2s with both the visual and spectroscopic orbits". Monthly Notices of the Royal Astronomical Society. 492 (2): 2709–2721. Bibcode:2020MNRAS.492.2709P. doi:10.1093/mnras/stz3616. ISSN 0035-8711.
^ Wilson, Ralph Elmer (1953). "General Catalogue of Stellar Radial Velocities". Carnegie Institute Washington D.C. Publication. Washington: Carnegie Institution of Washington. Bibcode:1953GCRV..C......0W.
^ Jump up to: ^a ^b ^c Pan, X. P.; et al. (1990), "Apparent orbit of the spectroscopic binary Beta Arietis with the time Mark III Stellar Interferometer", Astrophysical Journal, 356: 641–645, Bibcode:1990ApJ...356..641P, doi:10.1086/168870
^ Jump up to: ^a ^b ^c Mitton, J. (January 1977), "Spectroscopic observations and curve-of-growth analyses of the four A stars omicron Peg, beta Ari, kappa Ari and 32 Vir.", Astronomy and Astrophysics Supplement Series, 27: 35–46, Bibcode:1977A&AS...27...35M
^ Jump up to: ^a ^b Royer, F.; Zorec, J.; Gómez, A. E. (February 2007), "Rotational velocities of A-type stars. III. Velocity distributions", Astronomy and Astrophysics, 463 (2): 671–682, arXiv:astro-ph/0610785, Bibcode:2007A&A...463..671R, doi:10.1051/0004-6361:20065224, S2CID 18475298
^ Jump up to: ^a ^b Allen, Richard Hinckley (1899), Star-Names and Their Meanings, New York: G. E. Stechert, pp. 81–82, retrieved 2011-12-24
^ "bet Ari -- Spectroscopic binary", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2011-12-29
^ 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.
^ Jump up to: ^a ^b "IAU Catalog of Star Names". Retrieved 28 July 2016.
^ IAU Working Group on Star Names (WGSN), International Astronomical Union, retrieved 22 May 2016.
^ (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 2010-08-18 at the Wayback Machine, Hong Kong Space Museum. Accessed on line November 23, 2010.
^ Jump up to: ^a ^b Gray, R. O.; et al. (October 2003), "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 Parsecs: The Northern Sample. I.", The Astronomical Journal, 126 (4): 2048–2059, arXiv:astro-ph/0308182, Bibcode:2003AJ....126.2048G, doi:10.1086/378365, S2CID 119417105
^ 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

External links

[rad-6] Jump up to: ^a ^b Calculated, using the Stefan-Boltzmann law and the star's effective temperature and luminosity, with respect to the solar nominal effective temperature of 5,772 K: ${\sqrt {{\biggl (}{\frac {5,772}{8,759}}{\biggr )}^{4}\cdot 10^{1.32}}}=1.985\ R_{\odot }.$ ${\sqrt {{\biggl (}{\frac {5,772}{5,811}}{\biggr )}^{4}\cdot 10^{0.11}}}=1.12\ R_{\odot }.$

[aaa474_2_653-1] Jump up to: ^a ^b ^c ^d 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

[sps1966-2] Jump up to: ^a ^b ^c Gutierrez-Moreno, Adelina; et al. (1966). "A System of photometric standards". Publications of the Department of Astronomy University of Chile. 1. Publicaciones Universidad de Chile, Department de Astronomy: 1–17. Bibcode:1966PDAUC...1....1G.

[sb2-3] Jump up to: ^a ^b ^c ^d ^e ^f ^g ^h Piccotti, Luca; Docobo, José Ángel; Carini, Roberta; Tamazian, Vakhtang S.; Brocato, Enzo; Andrade, Manuel; Campo, Pedro P. (2020-02-01). "A study of the physical properties of SB2s with both the visual and spectroscopic orbits". Monthly Notices of the Royal Astronomical Society. 492 (2): 2709–2721. Bibcode:2020MNRAS.492.2709P. doi:10.1093/mnras/stz3616. ISSN 0035-8711.

[gcsrv-4] Wilson, Ralph Elmer (1953). "General Catalogue of Stellar Radial Velocities". Carnegie Institute Washington D.C. Publication. Washington: Carnegie Institution of Washington. Bibcode:1953GCRV..C......0W.

[apj356_641-5] Jump up to: ^a ^b ^c Pan, X. P.; et al. (1990), "Apparent orbit of the spectroscopic binary Beta Arietis with the time Mark III Stellar Interferometer", Astrophysical Journal, 356: 641–645, Bibcode:1990ApJ...356..641P, doi:10.1086/168870

[aaass27_35-7] Jump up to: ^a ^b ^c Mitton, J. (January 1977), "Spectroscopic observations and curve-of-growth analyses of the four A stars omicron Peg, beta Ari, kappa Ari and 32 Vir.", Astronomy and Astrophysics Supplement Series, 27: 35–46, Bibcode:1977A&AS...27...35M

[aaa463_2_671-8] Jump up to: ^a ^b Royer, F.; Zorec, J.; Gómez, A. E. (February 2007), "Rotational velocities of A-type stars. III. Velocity distributions", Astronomy and Astrophysics, 463 (2): 671–682, arXiv:astro-ph/0610785, Bibcode:2007A&A...463..671R, doi:10.1051/0004-6361:20065224, S2CID 18475298

[allen1899-9] Jump up to: ^a ^b Allen, Richard Hinckley (1899), Star-Names and Their Meanings, New York: G. E. Stechert, pp. 81–82, retrieved 2011-12-24

[SIMBAD-10] "bet Ari -- Spectroscopic binary", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2011-12-29

[Kunitzsch-11] 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.

[IAU-CSN-12] Jump up to: ^a ^b "IAU Catalog of Star Names". Retrieved 28 July 2016.

[WGSN-13] IAU Working Group on Star Names (WGSN), International Astronomical Union, retrieved 22 May 2016.

[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.

[15] (in Chinese) 香港太空館 - 研究資源 - 亮星中英對照表 Archived 2010-08-18 at the Wayback Machine, Hong Kong Space Museum. Accessed on line November 23, 2010.

[aj126_4_2048-16] Jump up to: ^a ^b Gray, R. O.; et al. (October 2003), "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 Parsecs: The Northern Sample. I.", The Astronomical Journal, 126 (4): 2048–2059, arXiv:astro-ph/0308182, Bibcode:2003AJ....126.2048G, doi:10.1086/378365, S2CID 119417105

[mnras384_1_173-17] 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

[ 1 ]

[ 2 ]

[ 3 ]

[4]

[5]

[a]

[6]

[7]

[8]

[9]

[ 10 ]

[ 11 ]

[ 12 ]

[ 13 ]

[14]

[15]

[16]

Данные наблюдения Epoch J2000 Equinox J2000
Расположение β -arietis (Circled)
Созвездие	Овен
Правильное восхождение	01 ^час 54 ^м 38.41099 ^с^{[ 1 ]}
Склонение	+20° 48′ 28.9133″ ^{[ 1 ]}
Apparent magnitude (V)	2.655 ^{[ 2 ]} (2.712 + 5.789 ^{[ 3 ]})
Характеристики
Спектральный тип	A3V + G2V ^{[ 3 ]}
U -B Цветовой индекс	+0.170 ^{[ 2 ]}
B - V Индекс цвета	+0.142 ^{[ 2 ]}
Астрометрия

Radial velocity (R_v)	-1.9^[4] km/s
Proper motion (μ)	RA: +98.74^[1] mas/yr Dec.: -110.41^[1] mas/yr
Parallax (π)	55.827 ± 0.308 mas^[3]
Distance	58.4 ± 0.3 ly (17.91 ± 0.10 pc)
Absolute magnitude (M_V)	1.382 (1.444 + 4.521)^[3]

Orbit^[5]
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^[3]
A
Mass	2.067±0.057 `M`_☉
Radius	1.985 ± 0.229^[a] `R`_☉
Luminosity	20.9+5.4 −4.3 `L`_☉
Surface gravity (log g)	4.0^[6] cgs
Temperature	8,759 K
Metallicity [Fe/H]	0.16^[6] dex
Rotational velocity (v sin i)	73^[7] km/s
Age	447+261 −165 Myr
B
Mass	1.058±0.026 `M`_☉
Radius	1.12 ± 0.064^[a] `R`_☉
Luminosity	1.29+0.16 −0.14 `L`_☉
Temperature	5,811 K
Other designations
Sheratan, Sharatan, Al Sharatain,^[8] 6 Arietis, Gl 80, HR 553, BD +20°306, HD 11636, SAO 75012, FK5 66, HIP 8903.^[9]
Database references
SIMBAD	data
ARICNS	data