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13 Ceti

April 12, 2024

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]

13 Ceti

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]
Distance69.3 ± 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
Mass1.18±0.09[5] M☉
Luminosity2.63[8] L☉
Temperature6,457[8] K
Age3.8+1.8
−0.3[2] Gyr
B
Mass0.90±0.09[5] M☉
Luminosity0.83[8] L☉
Temperature5,754[8] K
Age2.5[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
SIMBADdata

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]

References edit

  1. ^ a b c d e 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.
  2. ^ a b c d e f 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. ^ a b c d Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466, Bibcode:2001AJ....122.3466M, doi:10.1086/323920, retrieved 2015-07-22.
  4. ^ a b c 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.
  5. ^ a b c d e f g h Andrade, Manuel (October 2019), "Colour-dependent accurate modelling of dynamical parallaxes and masses of visual binaries. Application to the VB+SB2 systems with definitive orbits", Astronomy & Astrophysics, 630: 11, Bibcode:2019A&A...630A..96A, doi:10.1051/0004-6361/201936199, A96.
  6. ^ a b 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. ^ a b 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. ^ a b c d e f g 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.

April 12, 2024
ceti, triple, star, system, equatorial, constellation, cetus, dimly, visible, naked, with, combined, apparent, visual, magnitude, system, located, distance, approximately, light, years, from, based, stellar, parallax, drifting, further, away, with, radial, vel. 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 13 CetiA light curve for BU Ceti plotted from TESS dataObservation dataEpoch J2000 0 Equinox J2000 0Constellation CetusRight ascension 00h 35m 14 87968s 1 Declination 03 35 34 2367 1 Apparent magnitude V 5 20 2 5 61 6 90 3 CharacteristicsEvolutionary stage Main sequenceSpectral type F6 V G4 V K3 5 V 4 5 B V color index 0 567 0 008 2 Variable type RS CVn 6 AstrometryRadial velocity Rv 10 37 0 40 7 km sProper motion m RA 408 34 1 mas yr Dec 35 22 1 mas yrParallax p 47 05 0 67 mas 1 Distance69 3 1 0 ly 21 3 0 3 pc Absolute magnitude MV 3 56 2 Orbit 8 PrimaryACompanionBPeriod P 2 516 6163 2 7808 dEccentricity e 0 77300Periastron epoch T 56 935 2034 MJDArgument of periastron w secondary 283 8 Orbit 9 PrimaryAaCompanionAbPeriod P 2 081891 0 000005 dSemi major axis a 1 260 0 010 MmEccentricity e 0 0 fixed Periastron epoch T 2 443 400 4573 0 0032 HJDArgument of periastron w secondary 0 0 Semi amplitude K1 primary 43 98 0 39 km sDetailsAaMass1 18 0 09 5 M Luminosity2 63 8 L Temperature6 457 8 KAge3 8 1 8 0 3 2 GyrBMass0 90 0 09 5 M Luminosity0 83 8 L Temperature5 754 8 KAge2 5 8 GyrOther designationsHO 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 referencesSIMBADdataThis 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 References edit a b c d e van Leeuwen F 2007 Validation of the new Hipparcos reduction Astronomy and Astrophysics 474 2 653 664 arXiv 0708 1752 Bibcode 2007A amp A 474 653V doi 10 1051 0004 6361 20078357 S2CID 18759600 a b c d e f 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 a b c d Mason B D et al 2014 The Washington Visual Double Star Catalog The Astronomical Journal 122 6 3466 Bibcode 2001AJ 122 3466M doi 10 1086 323920 retrieved 2015 07 22 a b c 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 amp AS 100 173S a b c d e f g h Andrade Manuel October 2019 Colour dependent accurate modelling of dynamical parallaxes and masses of visual binaries Application to the VB SB2 systems with definitive orbits Astronomy amp Astrophysics 630 11 Bibcode 2019A amp A 630A 96A doi 10 1051 0004 6361 201936199 A96 a b 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 a b Karataș Yuksel 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 a b c d e f g 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 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 amp A 248 485D 13 Cet SIMBAD Centre de donnees astronomiques de Strasbourg Retrieved 2020 11 05 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 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 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 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 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 Retrieved from https en wikipedia org w index php title 13 Ceti amp oldid 1170150802, wikipedia, wiki, book, books, library,

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