HD 24071

Last updated
HD 24071 and HD 24072
Eridanus constellation map.svg
Location shown, annotated: f
Observation data
Epoch J2000       Equinox J2000
Constellation Eridanus
HD 24072
Right ascension 03h 48m 35.87402s [1]
Declination −37° 37′ 12.5158″ [1]
Apparent magnitude (V)4.721±0.009 [2]
HD 24071
Right ascension 03h 48m 35.47769s [3]
Declination −37° 37′ 19.2124″ [3]
Apparent magnitude (V)5.246±0.009 [2]
Characteristics
HD 24072
Spectral type B9.5 Van [4]
HD 24071
Spectral type A1 Va [4]
Variable type suspected [5]
Astrometry
HD 24072
Proper motion (μ)RA: +81.136 [1]   mas/yr
Dec.: −6.795 [1]   mas/yr
Parallax (π)18.8093 ± 0.2220  mas [1]
Distance 173 ± 2  ly
(53.2 ± 0.6  pc)
Absolute magnitude  (MV)1.194±0.190 [2]
HD 24071
Proper motion (μ)RA: +63.372 [3]   mas/yr
Dec.: −8.121 [3]   mas/yr
Parallax (π)18.7976 ± 0.0582  mas [3]
Distance 173.5 ± 0.5  ly
(53.2 ± 0.2  pc)
Absolute magnitude  (MV)1.719±0.190 [2]
Details
HD 24072
Mass 2.6 [6]   M☉
Radius 2.0 [6]   R☉
Luminosity 35 [6]   L☉
Surface gravity (log g)4.26 [6]   cgs
Temperature 10.046 [6]   K
Rotational velocity (v sin i)225 [7]  km/s
Age 45±4 [2]   Myr
HD 24071
Mass 2.1 [3]   M☉
Radius 1.7 [3]   R☉
Luminosity20 [3]   L☉
Surface gravity (log g)4.16 [3]   cgs
Temperature 9,503 [3]   K
Metallicity [Fe/H]−1.47 [3]   dex
Rotational velocity (v sin i)39 [7]  km/s
Age 45±4 [2]   Myr
Other designations
f Eridani, CD−38 1297, HIP  17797, WDS J03486-3737
HD 24072: HR  1190, SAO  194551 [8]
HD 24071: HR  1189, SAO  194550 [9]
Database references
SIMBAD data
HD 24072
HD 24071

HD 24071 and HD 24072 form a binary [10] or possibly a triple star system in the equatorial constellation of Eridanus. The pair have the Bayer designation f Eridani. It is visible to the naked eye as a single star with a magnitude of 4.25. [11] HD 24071 has an apparent visual magnitude of 5.25 and HD 24072 a magnitude of 4.72. [2] As of 2009, the pair had an angular separation of 8.40″ along a position angle of 216°. [12] Both stars have an annual parallax shift 18.8  mas , which provides a distance estimate to the system of 173  light years. The pair are members of the Tucana-Horologium moving group, a 45 million year old set of stars that share a common motion through space. [2]

The brighter component, HD 24072, is a B-type main-sequence star with a classification of B9.5 Van. [4] The n suffix indicates "nebulous" absorption lines which are caused by its rapid rotation. It has a projected rotational velocity of 225 km/s. [7]

HD 24071 is an A-type main-sequence star with a stellar classification of A1 Va. [4] It is a suspected variable star of unknown type showing an amplitude of 0.05 magnitude, [5] and is a source of X-ray emission, which may originate from a companion of class G2-5V. [13]

Related Research Articles

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10 Canis Majoris Variable star in the constellation Canis Major

10 Canis Majoris is a single variable star in the southern constellation of Canis Major, located roughly 1,980 light years away from the Sun. It has the variable star designation FT Canis Majoris; 10 Canis Majoris is the Flamsteed designation. This body is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of 5.23. It is moving away from the Earth with a heliocentric radial velocity of +34 km/s.

V337 Carinae A K-type bright giant star in the constellation of Carina

V337 Carinae is a K-type bright giant star in the constellation of Carina. It is an irregular variable and has an apparent visual magnitude which varies between 3.36 and 3.44.

HD 69863 is a binary star system in the southern constellation of Carina. It is visible to the naked eye as a dim point of light with a combined apparent visual magnitude of 5.16. The system is located at a distance of about255 light years from the Sun based on parallax. The dual nature of this system was announced in 1832 by German astronomer Carl Rümker. As of 2015, the pair had an angular separation of 4.10″ along a position angle of 70°.

N Centauri is a binary star in the southern constellation of Centaurus. The brighter star is dimly visible to the naked eye with an apparent visual magnitude of 5.26, and it is approximately 304 light years away based on parallax. It has an absolute magnitude of +0.76 and is drifting further away from the Sun with a radial velocity of +27 km/s. It is a candidate member of the Sco OB2 moving group.

Omega Fornacis, which is Latinized from ω Fornacis, is a wide binary star system in the southern constellation of Fornax. It has a blue-white hue and is faintly visible to the naked eye as a fifth-magnitude star. The system lies at a distance of approximately 470 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +10 km/s.

FK Comae Berenices Star in the constellation of Coma Berenices

FK Comae Berenices is a variable star that varies in apparent magnitude between 8.14 and 8.33 over a period of 2.4 days. It is the prototype for the FK Comae Berenices class of variable stars. The variability of FK Com stars may be caused by large, cool spots on the rotating surfaces of the stars. This star is thought to be the result of a recent binary merger, resulting in a high rate of both spin and magnetic activity.

HD 223229 is a suspected variable star in the northern constellation of Andromeda. It is a double star consisting of a magnitude 6.11 primary and a magnitude 8.73 companion. The pair have an angular separation of 0.80″ along a position angle of 250°, as of 2009. The primary is a B-type subgiant star with a stellar classification of B3IV. It has an estimated 6.3 times the mass of the Sun, with an effective temperature of 17,900 K.

HD 225218 is a quadruple star system in the northern constellation of Andromeda. The primary component, HD 225218 A, is a giant star with a stellar classification of B9III, an apparent magnitude of 6.16, and is a candidate Lambda Boötis star. It has a fainter, magnitude 9.65 companion, HD 225218 B, at an angular separation of 5.2″ along a position angle of 171°. The primary itself has been identified as a binary star system through interferometry, with the two components separated by 0.165″. The pair, HD 225218 Aa and Ab, orbit each other with a period of about 70 years and an eccentricity of 0.515. Component B is likewise a spectroscopic binary.

LN Andromedae, also known as HD 217811, HR 8768, is a formerly suspected variable star in the constellation Andromeda. Located approximately 458 parsecs (1,490 ly) away from Earth, it shines with an apparent visual magnitude 6.41, thus it can be seen by the naked eye under very favourable conditions. Its spectral classification is B2V, meaning that it's a hot main sequence star, emitting light approximately with a blackbody spectrum at an effective temperature of 18,090 K.

HD 6114 is a visual binary star system in the northern constellation of Andromeda. With a combined apparent magnitude of 6.46, the star can only be seen with the naked eye by keen-eyed observers even on the best of nights. Based upon an annual parallax shift of 10.4 mas as seen from Earth's orbit, the system is located approximately 108 parsecs (350 ly) distant.

HD 90089 is a star located in the northern circumpolar constellation Camelopardalis. With an apparent magnitude of 5.25, it is faintly visible to the naked eye under ideal conditions. This star is located relatively close at a distance of 75 light years, but is drifting away at a rate of almost 8 km/s.

2 Vulpeculae is a binary star system in the northern constellation of Vulpecula, located around 1,800 light years away from the Sun. It is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of 5.43.

1 Serpentis is a red giant in the constellation Virgo with an apparent magnitude of 5.5. It is a red clump giant, a cool horizontal branch star that is fusing helium in its core. It has expanded to over 13 times the radius of the Sun and although it is cooler at 4,581 K it is 77 times more luminous. It is 322 light years away.

Epsilon Sagittae G-type star in the constellation Sagitta

Epsilon Sagittae (ε Sagittae) is a solitary, yellow-hued star in the northern constellation of Sagitta. With an apparent visual magnitude of +5.64 to +5.67, it is faintly visible to the naked eye on a dark night. It is a variable star with a small amplitude of 0.03 magnitudes. Based upon an annual parallax shift of 5.60 mas as seen from Earth, it is located roughly 580 light years from the Sun. At that distance, the visual magnitude of the star is diminished by an extinction factor of 0.1 due to interstellar dust.

HD 102350 is a single star in the constellation Centaurus. It has a yellow hue and is visible to the naked eye with an apparent visual magnitude of 4.11. The distance to this star is approximately 390 light years based on parallax, but it is drifting closer with a radial velocity of −3 km/s. It has an absolute magnitude of −1.51.

Delta2 Gruis, Latinized from δ2 Gruis, is a solitary, red-hued star in the southern constellation of Grus. It is visible to the naked eye with an apparent visual magnitude of 4.11. Based upon an annual parallax shift of 9.88 mas as seen from the Earth, the star is located around 330 light years from the Sun. It is moving further away from the Sun with a radial velocity of +3 km/s.

9 Ceti G-type star in the constellation Cetus

9 Ceti is the Flamsteed designation for a star in the equatorial constellation of Cetus. It has an apparent visual magnitude of 6.39, which is below the limit that can be seen with the naked eye by a typical observer. Based upon parallax measurements, this star is 69.6 light years away from the Sun. There is a magnitude 12.57 optical companion at an angular separation of 214 arc seconds along a position angle of 294°, although the pair are not physically associated as they have different proper motions.

17 Comae Berenices Star in the constellation Coma Berenices

17 Comae Berenices is a multiple star system in the northern constellation of Coma Berenices. The brighter component, 17 Com A, is a naked eye star with an apparent visual magnitude of 5.2. It has a faint companion of magnitude 6.6, 17 Com B, positioned at an angular separation of 146.4″ along a position angle of 251°, as of 2018. They are located at a distance of approximately 240 light years from the Sun based on parallax measurements.

HD 200044 is a solitary star in the equatorial constellation Delphinus. It has an apparent magnitude of 5.7, allowing it to be faintly seen with the naked eye. The object is located 598 light years away, but is approaching the Solar System with a heliocentric radial velocity of −15.07 km/s.

References

  1. 1 2 3 4 5 Vallenari, A.; et al. (2022). "Gaia DR3: data release content and main properties" . Retrieved 2022-06-13. Gaia EDR3 record for this source at VizieR.
  2. 1 2 3 4 5 6 7 8 Bell, Cameron P. M.; et al. (November 2015), "A self-consistent, absolute isochronal age scale for young moving groups in the solar neighbourhood", Monthly Notices of the Royal Astronomical Society, 454 (1): 593–614, arXiv: 1508.05955 , Bibcode:2015MNRAS.454..593B, doi:10.1093/mnras/stv1981, S2CID   55297862.
  3. 1 2 3 4 5 6 7 8 9 10 11 Vallenari, A.; et al. (2022). "Gaia DR3: data release content and main properties" . Retrieved 2022-06-13. Gaia EDR3 record for this source at VizieR.
  4. 1 2 3 4 Gray, R. O.; Garrison, R. F. (December 1987), "The Early A-Type Stars: Refined MK Classification, Confrontation with Stroemgren Photometry, and the Effects of Rotation", Astrophysical Journal Supplement, 65: 581, Bibcode:1987ApJS...65..581G, doi:10.1086/191237.
  5. 1 2 Adelman, S. J.; et al. (November 2000), "On the Variability of A0-A2 Luminosity Class III-V Stars", Information Bulletin on Variable Stars, 4984: 1, Bibcode:2000IBVS.4984....1A.
  6. 1 2 3 4 5 Stassun, Keivan G.; et al. (9 September 2019). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv: 1905.10694 . Bibcode:2019AJ....158..138S. doi: 10.3847/1538-3881/ab3467 . ISSN   0004-6256.
  7. 1 2 3 Royer, F.; et al. (October 2002), "Rotational velocities of A-type stars in the northern hemisphere. II. Measurement of v sin i", Astronomy and Astrophysics, 393: 897–911, arXiv: astro-ph/0205255 , Bibcode:2002A&A...393..897R, doi:10.1051/0004-6361:20020943, S2CID   14070763.
  8. ↑ "HD 24072". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2018-07-22.
  9. ↑ "HD 24071". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2018-07-22.
  10. ↑ Eggleton, P. P.; Tokovinin, A. A. (2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869, arXiv: 0806.2878 , Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID   14878976.
  11. ↑ Mallama, A. (2014). "Sloan Magnitudes for the Brightest Stars". The Journal of the American Association of Variable Star Observers. 42: 443. Bibcode:2014JAVSO..42..443M.
  12. ↑ 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
  13. ↑ Schröder, C.; Schmitt, J. H. M. M. (November 2007), "X-ray emission from A-type stars", Astronomy and Astrophysics, 475 (2): 677–684, Bibcode:2007A&A...475..677S, doi: 10.1051/0004-6361:20077429 .
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