HD 56405

Last updated
HD 56405
Canis Major constellation map.svg
Red circle.svg
Location of HD 56405 (circled)
Observation data
Epoch J2000       Equinox J2000
Constellation Canis Major
Right ascension 07h 16m 14.55342s [1]
Declination −15° 35′ 08.4724″
Apparent magnitude  (V)5.45 [2]
Characteristics
Spectral type A1V [3]
B−V color index 0.079±0.005 [4]
Astrometry
Radial velocity (Rv)+6.30±0.9 [5]  km/s
Proper motion (μ)RA: -46.118 [1]   mas/yr
Dec.: -15.488 [1]   mas/yr
Parallax (π)13.1152 ± 0.1293  mas [1]
Distance 249 ± 2  ly
(76.2 ± 0.8  pc)
Absolute magnitude  (MV)0.88 [4]
Details
Mass 2.13 [6]   M☉
Luminosity 38.86 [4]   L☉
Surface gravity (log g)4.14±0.14 [6]   cgs
Temperature 9,562±325 [6]   K
Rotational velocity (v sin i)149 [6]  km/s
Age 212 [6]   Myr
Other designations
BD−15°1734, FK5  2561, GC  9657, GJ  9228, HD  56405, HIP  35180, HR  2758, SAO  152641, TYC  5965-363-1 [7]
Database references
SIMBAD data

HD 56405 is a star in the southern constellation of Canis Major. It is white in hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.45. [2] To the east of HD 56405 is the open cluster NGC 2360, also known as Caroline's Cluster. [8] The distance to HD 56405, as determined from parallax measurements, is approximately 249  light years. It is drifting further away with a radial velocity (RV) of about +6 km/s. [5] Although classed as a single star, [9] it is to suspected to vary in RV. [10]

This is an A-type main-sequence star with a stellar classification of A1V. [3] It was classed as a candidate Lambda Boötis star, [11] but as of 2015 this classification has been rejected by astronomers due to the star having an inconsistent UV flux, possible RV variability, and a fairly high rotation rate. [2] The star is about 212 million years old with 2.13 times the mass of the Sun and is spinning with a projected rotational velocity of 149 km/s. [6] It is radiating 39 [4] times the luminosity of the Sun from its photosphere at an effective temperature of around 9,562 K. [6]

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<span class="mw-page-title-main">HD 211575</span> Star in the constellation Aquarius

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<span class="mw-page-title-main">29 Cygni</span> A-type main sequence star in the constellation Cygnus

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HD 16754 is a binary or triple-star system in the constellation Eridanus. It has the Bayer designation s Eridani; HD 16754 is the designation from the Henry Draper catalogue. The system is visible to the naked eye as a faint point of light with an apparent visual magnitude of +4.74. It is located at a distance of approximately 132 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +18 km/s. The system is a member of the Columba association of co-moving stars.

<span class="mw-page-title-main">64 Eridani</span> Single, yellow-white hued star in the constellation Eridanus

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HD 125442 is a single star in the southern constellation of Lupus. Its apparent visual magnitude is 4.78, which can be seen with the naked eye. The distance to HD 125442, as determined from its annual parallax shift of 22.1 mas, is 147 light years.

36 Serpentis is a binary star system in the equatorial constellation of Serpens. It has the Bayer designation b Serpentis, while 36 Serpentis is the Flamsteed designation. The system is visible to the naked eye as a dim, white-hued point of light with a combined apparent visual magnitude of 5.09. It is located 162 light years away from the Sun based on parallax, and is moving closer with a radial velocity of −8 km/s.

HD 26764 is a solitary star located in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.19, making it faintly to the naked eye if seen under ideal conditions. The star is currently situated at a distance of 266 light years but is drifting closer with a heliocentric radial velocity of 3.0 km/s, which is poorly constrained.

HD 218108, also known as HR 8786, is a solitary, white hued star located in the southern circumpolar constellation Octans. It has an apparent magnitude of 6.11, making it faintly visible to the naked eye under ideal conditions. Based on parallax measurements from Gaia DR3, the object is estimated to be 247 light years away. It appears to be approaching the Solar System with a fairly constrained radial velocity of −7 km/s. Paunzen et al. (2001) lists it as a λ Boötis star with a weak magnesium line.

References

  1. 1 2 3 4 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
  2. 1 2 3 Murphy, Simon J.; et al. (October 2015). "An Evaluation of the Membership Probability of 212 λ Boo Stars. I. A Catalogue". Publications of the Astronomical Society of Australia. 32: 43. arXiv: 1508.03633 . Bibcode:2015PASA...32...36M. doi:10.1017/pasa.2015.34. S2CID   59405545. e036.
  3. 1 2 Houk, Nancy; Smith-Moore, M. (1978). Michigan catalogue of two-dimensional spectral types for the HD stars. Vol. 4. Ann Arbor: Dept. of Astronomy, University of Michigan. Bibcode:1988mcts.book.....H.
  4. 1 2 3 4 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.
  5. 1 2 Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv: 1606.08053 . Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. S2CID   119231169.
  6. 1 2 3 4 5 6 7 David, Trevor J.; Hillenbrand, Lynne A. (2015). "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets". The Astrophysical Journal. 804 (2): 146. arXiv: 1501.03154 . Bibcode:2015ApJ...804..146D. doi:10.1088/0004-637X/804/2/146. S2CID   33401607.
  7. ↑ "HD 56405". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-01-06.
  8. ↑ Streicher, M. (December 2005). "Deepsky Delights: Caroline Herschel's deepsky discoveries". Monthly Notes of the Astronomical Society of Southern Africa. 64 (11 and 12): 234–236. Bibcode:2005MNSSA..64..234S.
  9. ↑ Eggleton, P. P.; Tokovinin, A. A. (September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society . 389 (2): 869–879. arXiv: 0806.2878 . Bibcode:2008MNRAS.389..869E. doi:10.1111/j.1365-2966.2008.13596.x. S2CID   14878976.
  10. ↑ Gerbaldi, M.; et al. (December 2003). "The heterogeneous class of lambda Bootis stars". Astronomy and Astrophysics. 412 (2): 447–464. Bibcode:2003A&A...412..447G. doi: 10.1051/0004-6361:20031472 .
  11. ↑ Renson, P.; et al. (December 1990). "Catalogue of Lambda Bootis Candidates". Bulletin d'Information du Centre de Données Stellaires. 38: 137. Bibcode:1990BICDS..38..137R.
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