94 Ceti

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94 Ceti A / B
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Cetus
Right ascension 03h 12m 46.43719s [1]
Declination −01° 11′ 45.9613″ [1]
Apparent magnitude  (V)+5.070 [2]
Characteristics
Spectral type F8V / M3V / M
U−B color index +0.09 [3]
B−V color index +0.56 [3]
Astrometry
Radial velocity (Rv)+18.96 ± 0.08 [4] km/s
Proper motion (μ)RA: 194.56 [1] mas/yr
Dec.: −69.01 [1] mas/yr
Parallax (π)44.29±0.28  mas [1]
Distance 73.6 ± 0.5  ly
(22.6 ± 0.1  pc)
Absolute magnitude  (MV)3.32
Orbit [5]
Primary94 Ceti A
Companion94 Ceti BC
Period (P)2029±41  yr
Semi-major axis (a)220±5 AU
Eccentricity (e)0.26±0.01
Inclination (i)104±2°
Longitude of the node (Ω)97±2°
Argument of periastron (ω)
(secondary)		342±7°
Orbit [6]
Primary94 Ceti B
Companion94 Ceti C
Period (P)378.35+0.36
−0.34 d
Semi-major axis (a)0.984±0.007 AU
Eccentricity (e)0.360±0.005
Inclination (i)108.323+0.581
−0.561°
Longitude of the node (Ω)191.496+1.602
−1.562°
Periastron epoch (T)MJD 55113.904±0.220
Argument of periastron (ω)
(secondary)		334.895±0.240°
Details
Mass 1.30 [7]   M☉
Radius 1.898 ± 0.070 [8]   R☉
Luminosity 4.02 ± 0.05 [9]   L☉
Surface gravity (log g)3.98 ± 0.10 [7]   cgs
Temperature 6,055 ± 10.0 [10]   K
Metallicity [Fe/H]1.15 ± 0.07 [7]   dex
Rotation 12.2  d [11]
Rotational velocity (v sin i)8.4 ± 0.8 [7]  km/s
Age 4.8 [9]   Gyr
Other designations
BD−01°457, FK5 116, GJ 128, HD 19994, HIP  14954, HR 962, LTT 1515, SAO 130355
Database references
SIMBAD data

94 Ceti (HD 19994) is a trinary star system approximately 73 light-years away in the constellation Cetus.

Contents

94 Ceti A is a yellow-white dwarf star with about 1.3 times the mass of the Sun while 94 Ceti B and C are red dwarf stars.

An infrared excess has been detected around the primary, most likely indicating the presence of a circumstellar disk at a radius of 95  AU. The temperature of this dust is 40 K. [12]

Stellar system

This system is a hierarchical triple star system with 94 Ceti A being orbited by 94 Ceti BC, a pair of M dwarfs, in 2000 years. 94 Ceti B and C meanwhile orbit each other in a 1-year orbit. [5]

Planetary system

On 7 August 2000, a planet was announced by the Geneva Extrasolar Planet Search team as a result of radial velocity measurements taken with the Swiss 1.2-metre Leonhard Euler Telescope at La Silla Observatory in Chile. [13] It is most stable if its inclination is either 65 or 115, ± 3. [14]

The 94 Ceti planetary system [14]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 1.855 ± 0.045  MJ 1.427535.7 ± 3.10.30 ± 0.04——

See also

References

  1. 1 2 3 4 5 van Leeuwen, F. (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. Vizier catalog entry
  2. ↑ Høg, E.; et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27 –L30. Bibcode:2000A&A...355L..27H.
  3. 1 2 Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode:1986EgUBV........0M.
  4. ↑ Nidever, David L.; et al. (2013). "Radial Velocities for 889 Late-Type Stars". The Astrophysical Journal Supplement Series. 141 (2): 503–522. arXiv: astro-ph/0112477 . Bibcode:2002ApJS..141..503N. doi:10.1086/340570. S2CID   51814894.
  5. 1 2 Wiegert, J.; et al. (2016). "94 Ceti: A triple star with a planet and dust disc". Monthly Notices of the Royal Astronomical Society. 462 (2): 1735–1748. arXiv: 1607.03038 . Bibcode:2016MNRAS.462.1735W. doi: 10.1093/mnras/stw1682 . S2CID   55234970.
  6. ↑ Röll, Tristan Alexander (2011). Astrometric search for extrasolar planets in stellar multiple systems (PhD). Friedrich-Schiller-University Jena.
  7. 1 2 3 4 Fuhrmann, K. (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 .
  8. ↑ van Belle, G. T.; von Brau, K. (2009). "Directly Determined Linear Radii and Effective Temperatures of Exoplanet Host Stars". The Astrophysical Journal . 694 (2): 1085–1098. arXiv: 0901.1206 . Bibcode:2009ApJ...694.1085V. doi:10.1088/0004-637X/694/2/1085. S2CID   18370219.
  9. 1 2 Boyajian, Tabetha S.; et al. (July 2013), "Stellar Diameters and Temperatures. III. Main-sequence A, F, G, and K Stars: Additional High-precision Measurements and Empirical Relations", The Astrophysical Journal, 771 (1): 31, arXiv: 1306.2974 , Bibcode:2013ApJ...771...40B, doi:10.1088/0004-637X/771/1/40, S2CID   14911430, 40. See Table 3.
  10. ↑ Kovtyukh, V. V.; Soubiran, C.; Belik, S. I.; Gorlova, N. I. (2003). "High precision effective temperatures for 181 F-K dwarfs from line-depth ratios". Astronomy and Astrophysics . 411 (3): 559–564. arXiv: astro-ph/0308429 . Bibcode:2003A&A...411..559K. doi:10.1051/0004-6361:20031378. S2CID   18478960.
  11. ↑ Mayor, M.; et al. (2004). "The CORALIE survey for southern extra-solar planets XII. Orbital solutions for 16 extra-solar planets discovered with CORALIE". Astronomy and Astrophysics. 415 (1): 391–402. arXiv: astro-ph/0310316 . Bibcode:2004A&A...415..391M. doi:10.1051/0004-6361:20034250. S2CID   5233877.
  12. ↑ Eiroa, C.; et al. (July 2013). "DUst around NEarby Stars. The survey observational results". Astronomy & Astrophysics. 555: A11. arXiv: 1305.0155 . Bibcode:2013A&A...555A..11E. doi:10.1051/0004-6361/201321050. S2CID   377244.
  13. ↑ "European Southern Observatory: Six Extrasolar Planets Discovered". SpaceRef.com. 7 August 2000. Retrieved 2 August 2009.
  14. 1 2 Plávalová, Eva; Solovaya, Nina A. (2013). "Analysis of the motion of an extrasolar planet in a binary system". The Astronomical Journal. 146 (5): 108. arXiv: 1212.3843 . Bibcode:2013AJ....146..108P. doi:10.1088/0004-6256/146/5/108. S2CID   118629538.
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