Xi1 Ceti

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Xi1 Ceti
Cetus IAU.svg
Red circle.svg
Location of ξ1 Ceti (circled)
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Cetus
Right ascension 02h 12m 59.99769s [1]
Declination +08° 50′ 48.2023″ [1]
Apparent magnitude  (V)+4.36 [2] [combined]
Characteristics
Spectral type G7III Ba0.4 Fe-1 [3] + DA4 [4]
B−V color index 0.878±0.024 [2]
Astrometry
Radial velocity (Rv)−3.93±0.09 [2]  km/s
Proper motion (μ)RA: −24.498 [1]   mas/yr
Dec.: −5.952 [1]   mas/yr
Parallax (π)9.5451 ± 0.3275  mas [1]
Distance 340 ± 10  ly
(105 ± 4  pc)
Absolute magnitude  (MV)–0.99 [5]
Orbit [6]
Period (P)1,642.1±1.3
Semi-major axis (a)≥ 0.896 ± 0.020  AU (134 ± 3  Gm)
Eccentricity (e)0 (fixed)
Periastron epoch (T)34,985±5  MJD
Semi-amplitude (K1)
(primary)		5.91±0.14 km/s
Details
A
Mass 3.80 [5]   M☉
Radius 18.2+1.0
−2.4 [1]   R☉
Luminosity 209.9±8.2 [1]   L☉
Surface gravity (log g)2.60 [1]   cgs
Temperature 5,184±50 [5]   K
Metallicity [Fe/H]−0.01 [5]   dex
Age 100 [7]   Myr
B
Mass 0.8 [5]   M☉
Surface gravity (log g)8.4 [8]   cgs
Other designations
ξ1 Cet, ksi01 Cet, 65 Ceti, NSV  749, BD+08° 345, HD  13611, HIP  10324, HR  649, SAO  110408, WDS 02130+0851, WD  02130+0851 [9]
Database references
SIMBAD data
Exoplanet Archive data

Xi1 Ceti , Latinized from ξ1 Ceti, is a binary star [10] system located in the equatorial constellation of Cetus. It is visible to the naked eye with a combined apparent visual magnitude of +4.36. [2] The distance to this system is approximately 340  light years based on parallax measurements, and it is drifting closer to the Sun with a radial velocity of −4 km/s. [2] The proximity of the star to the ecliptic means it is subject to lunar occultations. [11]

The spectroscopic binary nature of Xi1 Ceti was discovered in 1901 by William Wallace Campbell using the Mills spectrograph at the Lick Observatory. [12] [6] The pair have a circular orbit with a period of 4.5 years and a separation of 3.8  AU . [5] It is a suspected eclipsing binary with an amplitude of 0.03 in magnitude, which would suggest the orbital plane has a high inclination. [13]

The primary, designated component A, is a mild barium [14] giant star with a stellar classification of G7III Ba0.4 Fe-1. [3] Morgan and Keenan in 1973 had classified it as a bright giant star with an anomalous underabundance of the CN molecule. [15] Evidence has been found for an overabundance of s-process elements, [5] although this is disputed. [7] The star has 3.8 [5] times the mass and 18 [1] times the radius of the Sun. The companion, component B, is a small white dwarf companion with 80% of the mass of the Sun and a class of DA4. [4] It was detected in 1985 by its ultraviolet emission. [8]

In Chinese, 天囷 (Tiān Qūn), meaning Circular Celestial Granary , refers to an asterism consisting of α Ceti, κ1 Ceti, λ Ceti, μ Ceti, ξ1 Ceti, ξ2 Ceti, ν Ceti, γ Ceti, δ Ceti, 75 Ceti, 70 Ceti, 63 Ceti and 66 Ceti. Consequently, the Chinese name for Xi1 Ceti itself is "the Fifth Star of Circular Celestial Granary", Tiān Qūn Wu. [16]

Related Research Articles

Gliese 65, also known as Luyten 726-8, is a binary star system that is one of Earth's nearest neighbors, at 8.8 light-years from Earth in the constellation Cetus. The two component stars are both flare stars with the variable star designations BL Ceti and UV Ceti.

79 Ceti, also known as HD 16141, is a binary star system located 123 light-years from the Sun in the southern constellation of Cetus. It has an apparent visual magnitude of +6.83, which puts it below the normal limit for visibility with the average naked eye. The star is drifting closer to the Earth with a heliocentric radial velocity of −51 km/s.

<span class="mw-page-title-main">60 Sagittarii</span> Possible binary star system in the constellation Sagittarius

60 Sagittarii is a suspected binary star system in the southern constellation of Sagittarius. It has the Bayer designation A Sagittarii, while 60 Sagittarii is the Flamsteed designation. This naked-eye object forms the northwest corner of the asterism called the Terebellum and, with an apparent magnitude of approximately 4.84, it is the dimmest of the four stars in the Terebellum. It is located 379 light-years from the Sun, based on parallax, but is moving closer with a radial velocity of −51 km/s.

<span class="mw-page-title-main">Epsilon Aquilae</span> Binary star in the constellation of Aquila

Epsilon Aquilae, Latinized from ε Aquilae, is the Bayer designation for a binary star system in the equatorial constellation of Aquila, near the western constellation boundary with Hercules. It has an apparent visual magnitude of 4.02 and is visible to the naked eye. Based upon an annual parallax of 23.993 mas, Epsilon Aquilae lies at a distance of approximately 136 light-years from Earth, but is drifting closer with a radial velocity of –46 km/s.

14 Boötis is a possible binary star system located 110 light years away from the Sun in the northern constellation of Boötes. It is visible to the naked eye as a dim, yellow-white hued star with a combined apparent visual magnitude of 5.53. This system is moving closer to the Earth with a heliocentric radial velocity of −40 km/s. It has a relatively high proper motion, traversing the celestial sphere at the rate of 0.260 arc seconds per annum.

<span class="mw-page-title-main">Gamma Ceti</span> Star system in the constellation Cetus

Gamma Ceti is a triple star system in the equatorial constellation of Cetus. It has a combined apparent visual magnitude of 3.47. Based upon parallax measurements, this star is located at a distance of about 80 light-years from the Sun.

<span class="mw-page-title-main">Zeta Capricorni</span> Star in the constellation Capricornus

Zeta Capricorni, Latinised from ζ Capricorni, is a binary star system in the southern constellation of Capricornus. It is visible to the naked eye with an apparent visual magnitude of 3.77. The system is located at a distance of approximately 386 light-years from the Sun based on parallax. It is drifting further away with a radial velocity of +2 km/s. The absolute magnitude of this system is −1.59.

Xi<sup>1</sup> Centauri Star in the constellation Centaurus

Xi1 Centauri, Latinized from ξ1 Centauri, is a solitary star in the southern constellation of Centaurus. It is visible to the naked eye with an apparent visual magnitude of +4.83. With an annual parallax shift of 14.79 mas, it is located around 221 light years from the Sun. At that distance, the apparent visual magnitude of the star is diminished by an interstellar extinction factor of 0.10 due to intervening dust. Just 17 arc minutes to the east of Xi1 Centauri lies the galaxy NGC 4945.

<span class="mw-page-title-main">Zeta Cygni</span> Star in the constellation Cygnus

Zeta Cygni is a binary star system in the northern constellation of Cygnus, the swan. It has an apparent visual magnitude of 3.26 and, based upon parallax measurements, is about 143 light-years away.

Pi Cephei is a trinary star located in the constellation Cepheus. With a combined apparent magnitude of about 4.4, the system is faintly visible to the naked eye. The inner pair of stars orbits in 1.5 years while the outer companion completes one orbit in about 160 years.

<span class="mw-page-title-main">EQ Virginis</span> Star in the constellation Virgo

EQ Virginis is a single variable star in the equatorial constellation of Virgo. It has a baseline visual apparent magnitude of 9.36, but is a flare star that undergoes sporadic bursts of brightening. The star is located at a distance of 67 light-years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −23 km/s. It is a member of the IC 2391 moving group of stars, which is between 30 and 50 million years old.

<span class="mw-page-title-main">Xi Piscium</span> Binary star system in the constellation Pisces

Xi Piscium (ξ Piscium) is an orange-hued binary star system in the zodiac constellation of Pisces. In 1690, the astronomer Johannes Hevelius in his Firmamentum Sobiescianum regarded the constellation Pisces as being composed of four subdivisions. Xi Piscium was considered to be part of the Linum Austrinum, the South Cord. The star is visible to the naked eye, having an apparent visual magnitude of 4.60. Based upon an annual parallax shift of 11.67 mas as seen from Earth, it is located about 280 light years from the Sun. It is moving away from the Sun, having a radial velocity of +26 km/s.

<span class="mw-page-title-main">Mu Ceti</span> Variable star in the constellation Cetus

Mu Ceti is a star in the constellation Cetus. The combined apparent magnitude of the system is +4.27, and it is located 84 light-years from the Sun.

<span class="mw-page-title-main">Nu Ceti</span> Binary star system in the constellation Cetus

ν Ceti, Latinized as Nu Ceti, is a binary star system in the equatorial constellation of Cetus. It is visible to the naked eye as a faint point of light with a combined apparent visual magnitude of 4.86. The system is located approximately 340 light years distant from the Sun, based on parallax, and is drifting further away with a radial velocity of 4.8 km/s. Nu Ceti is believed to be part of the Ursa Major stream of co-moving stars.

Xi2 Ceti, Latinized from ξ2 Ceti, is a star located in the equatorial constellation of Cetus. It is visible to the naked eye with an apparent visual magnitude of +4.3. This star is located at a distance of approximately 197 light years from the Sun based on parallax, and is drifting further away with a radial velocity of 12 km/s. It made its closest approach some 2.7 million years ago at a distance of around 128 light-years.

75 Ceti is a single star in the equatorial constellation of Cetus with at least two planets. It is visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude of +5.36. The star is located 268 light-years distant from the Sun, based on parallax, but is drifting closer with a radial velocity of −6 km/s.

<span class="mw-page-title-main">56 Pegasi</span> Star in the constellation Pegasus

56 Pegasi is a binary star system in the northern constellation of Pegasus. It is visible to the naked eye with a combined apparent visual magnitude of 4.74. The system is approximately 590 light years away from the Sun based on parallax, but is drifting closer with a radial velocity of −28 km/s. It is listed as a member of the Wolf 630 moving group.

Xi<sup>1</sup> Lupi Probable binary star system in the constellation Lupus

Xi1 Lupi (ξ1 Lup, ξ1 Lupi) is a probable binary star in the southern constellation of Lupus. It is faintly visible to the naked eye with an apparent visual magnitude of 5.1, and forms a visual double star with Xi2 Lupi. Based upon an annual parallax shift of 23.60 mas as seen from Earth, it is located around 140 light-years from the Sun. It is a member of the Upper Scorpius sub-group of the nearby Sco OB2 association.

16 Serpentis is a binary star system in the Serpens Caput portion of the equatorial constellation of Serpens, located 228 light years from the Sun. It is visible to the naked eye as a fain, orange-hued star with an apparent visual magnitude of 5.261. The system is moving further from the Earth with a heliocentric radial velocity of +3 km/s.

HD 136138, or HR 5692, is a binary star system in the Serpens Caput segment of the Serpens constellation. It has a golden hue like the Sun and is dimly visible to the naked eye with an apparent visual magnitude of 5.68; the light contribution from the companion is effectively negligible. This system is located at a distance of approximately 420 light years from the Sun based on parallax. It is drifting closer with a radial velocity of −7.7 km/s and has a proper motion of 23.5 mas·yr−1.

References

  1. 1 2 3 4 5 6 7 8 9 Brown, 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 at VizieR.
  2. 1 2 3 4 5 Anderson, 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.
  3. 1 2 Keenan, 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.
  4. 1 2 McCook, G. P.; Sion, E. M. (1999), "A Catalogue of Spectroscopically Identified White Dwarfs", The Astrophysical Journal Supplement Series, 121 (1): 1–130, Bibcode:1999ApJS..121....1M, CiteSeerX   10.1.1.565.5507 , doi: 10.1086/313186 .
  5. 1 2 3 4 5 6 7 8 Kong, X. M.; et al. (May 2018), "Chemical abundances of primary stars in the Sirius-like binary systems", Monthly Notices of the Royal Astronomical Society, 476 (1): 724–740, arXiv: 1801.10284 , Bibcode:2018MNRAS.476..724K, doi:10.1093/mnras/sty280.
  6. 1 2 Griffin, R. F.; Herbig, G. H. (1981). "Spectroscopic Orbits of Xi Piscium 60 Andromedae and ξ1 Ceti". Monthly Notices of the Royal Astronomical Society . 196: 33–43. Bibcode:1981MNRAS.196...33G. doi: 10.1093/mnras/196.1.33 .
  7. 1 2 Smiljanic, R.; et al. (June 2007), "Abundance analysis of barium and mild barium stars", Astronomy and Astrophysics, 468 (2): 679–693, arXiv: astro-ph/0702421 , Bibcode:2007A&A...468..679S, doi:10.1051/0004-6361:20065867, S2CID   5863942.
  8. 1 2 Böhm-Vitense, E.; Johnson, H. R. (June 1985), "Detection of a compact companion of the mild barium star ksi1 Ceti", Astrophysical Journal, 293: 288–293, Bibcode:1985ApJ...293..288B, doi:10.1086/163236.
  9. ↑ "ksi01 Cet". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2021-07-02.{{cite web}}: CS1 maint: postscript (link)
  10. ↑ Eggleton, P. P.; Tokovinin, A. A. (September 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.
  11. ↑ Schmidtke, P. C.; Africano, J. L. (September 1984), "KPNO lunar occultation summary. I", Astronomical Journal, 89: 1371–1378, Bibcode:1984AJ.....89.1371S, doi: 10.1086/113637 .
  12. ↑ Campbell, William Wallace (1901). "Some recent results secured with the Mills spectrograph". Lick Observatory Bulletin. 1 (4): 22–25. Bibcode:1901LicOB...1...22C. doi:10.5479/ADS/bib/1901LicOB.1.22C.
  13. ↑ Hoffleit, Dorrit (1996), "A Catalogue of Correlations Between Eclipsing Binaries and Other Categories of Double Stars", The Journal of the American Association of Variable Star Observers, 24 (2): 105–116, Bibcode:1996JAVSO..24..105H.
  14. ↑ Pinsonneault, M. H.; et al. (March 1984), "Lithium in the barium stars", Publications of the Astronomical Society of the Pacific, 96: 239–246, Bibcode:1984PASP...96..239P, doi:10.1086/131327, S2CID   120248035.
  15. ↑ Morgan, W. W.; Keenan, P. C. (1973), "Spectral Classification", Annual Review of Astronomy and Astrophysics, 11: 29, Bibcode:1973ARA&A..11...29M, doi:10.1146/annurev.aa.11.090173.000333.
  16. ↑ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 11 日 Archived 2012-02-04 at the Wayback Machine
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