HD 3443

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Coordinates: Sky map 00h 37m 20.7196s, −24° 46′ 02.1843″

HD 3443
Observation data
Epoch J2000      Equinox J2000
Constellation Cetus
Right ascension 00h 37m 20.7196s[1]
Declination −24° 46′ 02.1843″[1]
Apparent magnitude (V) 5.57[2]
Characteristics
HD 3443A
Evolutionary stage main-sequence star
Spectral type G9V[3]
Apparent magnitude (g) 5.95[4]
HD 3443B
Evolutionary stage main-sequence star
Spectral type K0.5V[3]
Astrometry
Radial velocity (Rv)18.63[5] km/s
Proper motion (μ) RA: 1450.34[1] mas/yr
Dec.: −19.38[1] mas/yr
Parallax (π)64.93 ± 1.85[3] mas
Distance50 ± 1 ly
(15.4 ± 0.4 pc)
Absolute magnitude (MV)5.31±0.08[2]
Orbit[6]
PrimaryHD 3443A
CompanionHD 3443B
Period (P)25.09 y
Semi-major axis (a)0.4627[7]"
(8.9 AU[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±4.89 d
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-mass main sequence stars in the constellation of Cetus about 50 light years away.

System[]

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

Properties[]

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

References[]

  1. ^ a b c van 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. ^ a b c d e Davidson, 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. doi:10.1088/0004-6256/138/5/1354.
  3. ^ a b c d e Andrade, Manuel (2019). "Colour-dependent accurate modelling of dynamical parallaxes and masses of visual binaries". Astronomy & Astrophysics. 630: A96. 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. Gaia EDR3 record for this source at VizieR.
  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. 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. doi:10.1086/657903. S2CID 26826524.
  8. ^ a b c d Su, 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. ^ a b Justesen, A. B.; Albrecht, S. (2020). "The spin-orbit alignment of visual binaries". Astronomy & Astrophysics. 642: A212. arXiv:2008.12068. 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: 260–274. arXiv:1401.1006. 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. doi:10.1051/0004-6361/201527883. S2CID 119212009.
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