13 Ceti

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13 Ceti
BUCetLightCurve.png
A light curve for BU Ceti, plotted from TESS data
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Cetus
Right ascension 00h 35m 14.87968s [1]
Declination −03° 35′ 34.2367″ [1]
Apparent magnitude  (V)5.20 [2] (5.61 + 6.90) [3]
Characteristics
Evolutionary stage Main sequence
Spectral type F6 V + G4 V + K3.5 V [4] [5]
B−V color index 0.567±0.008 [2]
Variable type RS CVn [6]
Astrometry
Radial velocity (Rv)+10.37±0.40 [7]  km/s
Proper motion (μ)RA: +408.34 [1]   mas/yr
Dec.: −35.22 [1]   mas/yr
Parallax (π)47.05 ± 0.67  mas [1]
Distance 69.3 ± 1.0  ly
(21.3 ± 0.3  pc)
Absolute magnitude  (MV)3.56 [2]
Orbit [8]
PrimaryA
CompanionB
Period (P)2,516.6163±2.7808 d
Eccentricity (e)0.77300
Periastron epoch (T)56,935.2034 MJD
Argument of periastron (ω)
(secondary)		283.8°°
Orbit [9]
PrimaryAa
CompanionAb
Period (P)2.081891±0.000005 d
Semi-major axis (a)≥1.260±0.010 Mm
Eccentricity (e)0.0 (fixed)
Periastron epoch (T)2,443,400.4573±0.0032 HJD
Argument of periastron (ω)
(secondary)		0.0°
Semi-amplitude (K1)
(primary)		43.98±0.39 km/s
Details
Aa
Mass 1.18±0.09 [5]   M☉
Luminosity 2.63 [8]   L☉
Temperature 6,457 [8]   K
Age 3.8+1.8
−0.3 [2]   Gyr
B
Mass 0.90±0.09 [5]   M☉
Luminosity0.83 [8]   L☉
Temperature 5,754 [8]   K
Age 2.5 [8]   Gyr
Other designations
HO 212, 13 Cet, BU Cet, NSV  212, BD−04°62, GC  696, GJ  23, HD  3196, HIP  2762, HR  142, SAO  128839, WDS 00352-0336 [10]
Database references
SIMBAD data

13 Ceti is a triple star system [5] in the equatorial constellation of Cetus. It is dimly visible to the naked eye with a combined apparent visual magnitude of 5.20. [2] The system is located at a distance of approximately 69  light years from the Sun based on stellar parallax, and is drifting further away with a radial velocity of +10.4 km/s. [7] It shares a common motion with the Hyades moving group, [5] although it is too old to be a member. [11]

This star was identified as a visual binary system by G. W. Hough in 1844 and given the identifier HO 212. [12] The pair have an orbital period of 6.9 years and an eccentricity of 0.77. [8] The brighter member, designated component A, is an F-type main-sequence star with a stellar classification of F6 V [4] and a visual magnitude of 5.61. [3] It appears to have an active chromosphere and is classified as an RS Canum Venaticorum variable with a variable star designation of BU Cet. [6] The star was detected as a source of soft X-ray emission by EXOSAT. [13] It has 18% [5] more mass than the Sun and is estimated to be about four [2]  billion years old.

In 1907, E. B. Frost discovered the primary is a spectroscopic binary, making this a triple star system. This is a double-lined spectroscopic binary with a period of 2.1 days and a circularized orbit. The companion signature was confirmed using the separated fringe packet technique with the CHARA array. [14] It is most likely a K-type main-sequence star with a class of K3.5 V and 70% of the mass of the Sun. [5]

The secondary member of the visual binary, designated component B, is a G-type main-sequence star with a class of G4 V. [4] It has 90% [5] of the Sun's mass and a visual magnitude of 6.90. [3] A distant visual companion to this system was detected by S. W. Burnham in 1877. Designated component C, this star is a background object [15] of magnitude 12.50. As of 1999, it was located at an angular separation of 24.0″ from the primary along a position angle of 322°. [3]

Related Research Articles

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<span class="mw-page-title-main">Epsilon Ursae Minoris</span> Binary star system in the constellation Ursa Minor

Epsilon Ursae Minoris is a binary star system in the northern circumpolar constellation of Ursa Minor. It is visible to the naked eye with a combined apparent visual magnitude of 4.19. Based upon an annual parallax shift of 10.73 mas as seen from the Earth, it is located around 300 light years from the Sun. The pair are drawing nearer to the Sun with a radial velocity of −10.57 km/s.

<span class="mw-page-title-main">12 Camelopardalis</span> Star in the constellation of Camelopardalis

12 Camelopardalis is a binary star in the northern circumpolar constellation of Camelopardalis, located 700 light years away from the Sun as determined from parallax measurements. It forms a double star with 11 Camelopardalis, which is only 3 arcminutes away. The system has the variable star designation BM Camelopardalis; 12 Camelopardalis is the Flamsteed designation. It is just visible to the naked eye, appearing as a dim, orange-hued star with an apparent visual magnitude of 6.08. The system is moving closer to the Earth with a heliocentric radial velocity of −2 km/s.

<span class="mw-page-title-main">42 Capricorni</span> Binary star system in the constellation Capricornus

42 Capricorni is a binary star system in the zodiac constellation of Capricornus. It has a combined apparent visual magnitude of 5.18, so it is faintly visible to the naked eye. Its annual parallax shift of 30.09 mas yields a distance estimate of about 108 light years; the system is moving closer to the Sun with a radial velocity of −1.2 km/s. 42 Capricorni is 0.2 degree south of the ecliptic and so is subject to lunar occultations.

<span class="mw-page-title-main">HR 5553</span> Binary star system in the constellation Boötes

HR 5553 is a binary star system located thirty-eight light-years away from the Sun, in the northern constellation Boötes. It has the variable star designation DE Boötis, and is classified as an RS Canum Venaticorum variable that ranges in apparent visual magnitude from 5.97 down to 6.04, which is bright enough to be dimly visible to the naked eye. The system is drifting closer to the Sun with a radial velocity of −30 km/s, and is expected to come as close as 26.9 light-years in 210,000 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">Omicron Draconis</span> Variable star in the constellation Draco

Omicron Draconis is a giant star in the constellation Draco located 322.93 light years from the Earth. Its path in the night sky is circumpolar for latitudes greater than 31o north, meaning the star never rises or sets when viewed in the night sky.

AM Canum Venaticorum is a hydrogen-deficient cataclysmic variable binary star in the constellation of Canes Venatici. It is the type star of its class of variables, the AM Canum Venaticorum stars. The system consists of a white dwarf gaining matter via an accretion disk from a semi-degenerate or white dwarf companion.

<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.

Xi<sup>1</sup> Ceti Star in the constellation Cetus

Xi1 Ceti , Latinized from ξ1 Ceti, is a binary star system located in the equatorial constellation of Cetus. It is visible to the naked eye with a combined apparent visual magnitude of +4.36. 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. The proximity of the star to the ecliptic means it is subject to lunar occultations.

Tau1 Eridani, Latinized from τ1 Eridani, is a binary star system in the constellation Eridanus. It has an apparent magnitude of 4.46, making it visible to the naked eye in suitably dark conditions. This is a spectroscopic binary with an orbital period of 958 days. It is located about 46 light years from the Earth. At present, the system is moving away from the Sun with a radial velocity of +26 km/s. About 305,000 years ago, perihelion passage was made at an estimated distance of 30.5 ly (9.35 pc).

<span class="mw-page-title-main">50 Persei</span> Star in the constellation Perseus

50 Persei is a star in the constellation Perseus. Its apparent magnitude is 5.52, which is bright enough to be seen with the naked eye. Located around 21.00 parsecs (68.5 ly) distant, it is a White main-sequence star of spectral type F7V, a star that is currently fusing its core hydrogen. In 1998 the star was named a candidate Gamma Doradus variable with a period of 3.05 days, which would means it displays variations in luminosity due to non-radial pulsations in the photosphere. Subsequently, it was classified as a RS Canum Venaticorum and BY Draconis variable by an automated program.

<span class="mw-page-title-main">Sigma Coronae Borealis</span> Star in the constellation Corona Borealis

Sigma Coronae Borealis is a star system in the constellation of Corona Borealis. It is a quintuple star system containing three sunlike main-sequence stars and two other low-mass stars. The combined visual magnitude is 5.3 and the system lies 74 light years from Earth. σ CrB A is the variable star TZ Coronae Borealis.

c Ursae Majoris is the Bayer designation for a double-lined spectroscopic binary star system in the northern constellation of Ursa Major. It has an apparent visual magnitude of 5.18, which indicates that is visible to the naked eye. Parallax measurements yield an estimated distance of 66 light years from the Sun. The star is moving closer to the Earth with a heliocentric radial velocity of −14 km/s.

<span class="mw-page-title-main">RS Canum Venaticorum</span> Binary star in the constellation Canes Venatici

RS Canum Venaticorum is a binary star system in the northern constellation of Canes Venatici. It serves as the prototype to the class of RS Canum Venaticorum variables. The peak apparent visual magnitude of this system is below the level needed to observe it with the naked eye. It is located at a distance of approximately 443 light years from the Sun based on parallax, but is drifting closer with a net radial velocity of −14 km/s. Olin J. Eggen (1991) included this system as a member of the IC 2391 supercluster, but it was later excluded.

<span class="mw-page-title-main">SZ Piscium</span> Star system in the constellation Pisces

SZ Piscium is a triple star system in the equatorial constellation of Pisces. The inner pair form a double-lined spectroscopic binary with an orbital period of 3.966 days. It is a detached Algol-type eclipsing binary of the RS Canum Venaticorum class with a subgiant component. The system is too faint to be readily visible to the naked eye with a combined apparent visual magnitude of 7.18. It is located at a distance of approximately 306 light years based on parallax measurements.

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

UV Piscium is a binary star system in the constellation of Pisces. With a peak apparent visual magnitude of 8.98, it is too faint to be visible to the naked eye. This is an eclipsing binary system that decreases to magnitude 10.05 during the primary eclipse, then to magnitude 9.54 with the secondary eclipse. It is located at a distance of 232 light years from the Sun based on parallax measurements, and is receding with a radial velocity of 6.5 km/s. The position of this star near the ecliptic means it is subject to lunar occultation.

<span class="mw-page-title-main">ER Vulpeculae</span> Variable star in the constellation Vulpecula

ER Vulpeculae is a binary star system in the northern constellation of Vulpecula, abbreviated ER Vul. It is a variable star system with a brightness that ranges from an apparent visual magnitude of 7.27 down to 7.49, which is too faint to be visible to the naked eye. This system is located at a distance of 165 light years from the Sun based on parallax measurements. It is drifting closer with a radial velocity of −25 km/s.

<span class="mw-page-title-main">DM Ursae Majoris</span> Variable star in the constellation Ursa Major

DM Ursae Majoris is a binary star system in the northern circumpolar constellation of Ursa Major, abbreviated DM UMa. It is sometimes identified by the Bonner Durchmusterung catalogue designation BD +61 1211; DM UMa is the variable star designation. The system has a combined apparent visual magnitude of 9.29, which is too faint to be visible to the naked eye. Based on parallax measurements, the system is located at a distance of approximately 606 light years from the Sun, but it is drifting closer with a heliocentric radial velocity of −7 km/s.

<span class="mw-page-title-main">HD 8357</span> Binary star in the constellation Pisces

AR Piscium is a binary star system in the northern constellation of Canes Venatici, abbreviated AR Psc. It has the Henry Draper Catalogue identifier HD 8357; AR Piscium is its variable star designation. The pair have a combined apparent visual magnitude that fluctuates around 7.24, which is too faint to be readily visible to the naked eye. Parallax measurements place it at a distance of 148 light years from the Sun. The motion of this star through the Milky Way suggests it is a member of the intermediate disc population.

References

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  4. 1 2 3 Strassmeier, K. G.; et al. (July 1993), "A catalog of chromospherically active binary stars", Astronomy and Astrophysics, Supplemental Series, 100 (2nd ed.): 173–225, Bibcode:1993A&AS..100..173S.
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  6. 1 2 Fernandez-Figueroa, M. J.; et al. (January 1994), "CA II H and K and H alpha Emissions in Chromospherically Active Binary Systems (RS Canum Venaticorum and BY Draconis)" (PDF), Astrophysical Journal Supplement, 90: 433, Bibcode:1994ApJS...90..433F, doi:10.1086/191866.
  7. 1 2 Karataș, Yüksel; et al. (2004), "Kinematics of chromospherically active binaries and evidence of an orbital period decrease in binary evolution", Monthly Notices of the Royal Astronomical Society, 349 (3): 1069–1092, arXiv: astro-ph/0404219 , Bibcode:2004MNRAS.349.1069K, doi: 10.1111/j.1365-2966.2004.07588.x , S2CID   15290475.
  8. 1 2 3 4 5 6 7 Piccotti, Luca; et al. (February 2020), "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 .
  9. ↑ Duquennoy, A.; Mayor, M. (1991), "Multiplicity among solar-type stars in the solar neighbourhood. II - Distribution of the orbital elements in an unbiased sample", Astronomy and Astrophysics , 248 (2): 485–524, Bibcode:1991A&A...248..485D.
  10. ↑ "13 Cet". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2020-11-05.
  11. ↑ Montes, D.; et al. (2001), Garcia Lopez, Ramon J.; et al. (eds.), "Chromospherically Active Binaries Members of Young Stellar Kinematic Groups (CD-ROM Directory: contribs/montes2)", 11th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun, ASP Conference Proceedings, vol. 223, San Francisco: Astronomical Society of the Pacific, p. 1477, arXiv: astro-ph/9912161 , Bibcode:2001ASPC..223.1477M.
  12. ↑ Bauer, Carl August (November 1944), "A Report on New Spectrographic Material of 13 Ceti", Astrophysical Journal, 100: 302, Bibcode:1944ApJ...100..302B, doi:10.1086/144671.
  13. ↑ Bedford, D. K.; et al. (February 1985), "X-Ray Observations of Active Chromosphere Stars", Space Science Reviews, 40 (1–2): 51–54, Bibcode:1985SSRv...40...51B, doi:10.1007/BF00212865, S2CID   121806441.
  14. ↑ Raghavan, Deepak; et al. (January 2012), "A Search for Separated Fringe Packet Binaries Using the CHARA Array", The Astrophysical Journal, 745 (1): 10, Bibcode:2012ApJ...745...24R, doi: 10.1088/0004-637X/745/1/24 , S2CID   15622813, 24.
  15. ↑ Pogo, A. (September 1928), "Spectrographic study of the multiple system HO 212 = 13 Ceti AB.", Astrophysical Journal, 68: 116−144, Bibcode:1928ApJ....68..116P, doi:10.1086/143133.
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