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HD 3443

Coordinates:Sky map00h 37m 20.7196s, −24° 46′ 02.1843″
From Wikipedia, the free encyclopedia
Binary star system in constellation Cetus
HD 3443
Observation data
Epoch J2000      Equinox J2000
ConstellationCetus
Right ascension00h 37m 20.7196s[1]
Declination−24° 46′ 02.1843″[1]
Apparent magnitude (V)5.57[2]
Characteristics
HD 3443A
Evolutionary stagemain-sequence star
Spectral typeG9V[3]
Apparent magnitude (g)5.95[4]
HD 3443B
Evolutionary stagemain-sequence star
Spectral typeK0.5V[3]
Astrometry
Radial velocity (Rv)18.63[5] km/s
Proper motion (μ)RA: 1450.34mas/yr[1]
Dec.: −19.38mas/yr[1]
Parallax (π)64.93±1.85 mas[3]
Distance50 ± 1 ly
(15.4 ± 0.4 pc)
Absolute magnitude (MV)5.31±0.08[2]
Orbit[6]
PrimaryHD 3443A
CompanionHD 3443B
Period (P)25.09y
Semi-major axis (a)0.4627[7]"
(8.9AU[8])
Eccentricity (e)0.235
Inclination (i)65.9[9]°
Semi-amplitude (K1)
(primary)
18.4 km/s
Details[9]
HD 3443A
Mass0.915±0.005[3] M
Radius0.92±0.05 R
Luminosity1.2[8] L
Temperature5449[8] K
Metallicity [Fe/H]−0.12[2] dex
Rotation32.6±4.89d
Rotational velocity (v sin i)2.7±1.3 km/s
Age9.36[2] Gyr
HD 3443B
Mass0.864±0.005[3] M
Other designations
CD-25 225, CPD CPD-25 64, Gliese 25, HIP 2941, HR 159,2MASS J00372057-2446023, WDS 00373–2446
HD 3443A: Gaia EDR3 2347260998051944448,TYC 6421-1924-1
HD 3443B:TYC 6421-1924-2
Database references
SIMBADdata

HD 3443 is a binary system composed of medium-massmain sequence stars in the constellation ofCetus about50 light years away.

System

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This binary star system, with an orbital semimajor axis 8.9AU, has not had any circumstellar dust detected as of 2020.[8] While the habitable zones of the stars stretch from 0.55 to 0.95AU from the stars, planetary orbits with a semimajor axis beyond 1.87AU would become unstable due to the influence of the binary companion.[10]

Properties

[edit]

The star system is enriched in oxygen compared to theSolar System, having 140% of solar oxygen abundance,[11] but is depleted in heavier elements, having 75% of solar abundance of iron.[2]

References

[edit]
  1. ^abcvan 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.
  2. ^abcdeDavidson, James W.; Baptista, Brian J.; Horch, Elliott P.; Franz, Otto; Van Altena, William F. (2009)."A Photometric Analysis of Seventeen Binary Stars Using Speckle Imaging".The Astronomical Journal.138 (5):1354–1364.Bibcode:2009AJ....138.1354D.doi:10.1088/0004-6256/138/5/1354.
  3. ^abcdeAndrade, Manuel (2019)."Colour-dependent accurate modelling of dynamical parallaxes and masses of visual binaries".Astronomy & Astrophysics.630: A96.Bibcode:2019A&A...630A..96A.doi:10.1051/0004-6361/201936199.
  4. ^Brown, A. G. A.; et al. (Gaia collaboration) (2021)."Gaia Early Data Release 3: Summary of the contents and survey properties".Astronomy & Astrophysics.649: A1.arXiv:2012.01533.Bibcode:2021A&A...649A...1G.doi:10.1051/0004-6361/202039657.S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source atVizieR.
  5. ^Pourbaix, D.; et al. (September 2004). "SB9: The ninth catalogue of spectroscopic binary orbits".Astronomy and Astrophysics.424:727–732.arXiv:astro-ph/0406573.Bibcode:2004A&A...424..727P.doi:10.1051/0004-6361:20041213.S2CID 119387088.
  6. ^Pourbaix, D. (2000)."Resolved double-lined spectroscopic binaries: A neglected source of hypothesis-free parallaxes and stellar masses".Astronomy and Astrophysics Supplement Series.145 (2):215–222.Bibcode:2000A&AS..145..215P.doi:10.1051/aas:2000237.
  7. ^Tokovinin, A.; Cantarutti, R.; Tighe, R.; Schurter, P.; Van Der Bliek, N.; Martinez, M.; Mondaca, E. (2010). "High-Resolution Imaging at the SOAR Telescope".Publications of the Astronomical Society of the Pacific.122 (898):1483–1494.arXiv:1010.4176.Bibcode:2010PASP..122.1483T.doi:10.1086/657903.S2CID 26826524.
  8. ^abcdSu, Kate Y L.; Kennedy, Grant M.; Yelverton, Ben (2020)."No significant correlation between radial velocity planet presence and debris disc properties".Monthly Notices of the Royal Astronomical Society.495 (2):1943–1957.arXiv:2005.03573.doi:10.1093/mnras/staa1316.
  9. ^abJustesen, A. B.; Albrecht, S. (2020). "The spin-orbit alignment of visual binaries".Astronomy & Astrophysics.642: A212.arXiv:2008.12068.Bibcode:2020A&A...642A.212J.doi:10.1051/0004-6361/202039138.S2CID 221340982.
  10. ^Jaime, Luisa G.; Aguilar, Luis; Pichardo, Barbara (2014)."Habitable zones with stable orbits for planets around binary systems".Monthly Notices of the Royal Astronomical Society.443 (1):260–274.arXiv:1401.1006.Bibcode:2014MNRAS.443..260J.doi:10.1093/mnras/stu1052.
  11. ^Maldonado, J.; Villaver, E. (2016). "Evolved stars and the origin of abundance trends in planet hosts".Astronomy & Astrophysics.588: A98.arXiv:1602.00835.Bibcode:2016A&A...588A..98M.doi:10.1051/0004-6361/201527883.S2CID 119212009.
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