F Eridani

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

f Eridani is a binary, [10] or possibly a triple, star system in the equatorial constellation of Eridanus, consisting of stars HD 24071 and HD 24072. They share a single Hipparcos catalogue entry, HIP 17797, but have separate Bright Star Catalogue listings, HR 1189 and 1190. f Eridani is the Bayer designation of the pair.

f Eridani 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 may itself be a spectroscopic binary. The visible component 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

<span class="mw-page-title-main">40 Eridani</span> Triple star system in the constellation Eridanus

40 Eridani is a triple star system in the constellation of Eridanus, abbreviated 40 Eri. It has the Bayer designation Omicron2 Eridani, which is Latinized from ο2 Eridani and abbreviated Omicron2 Eri or ο2 Eri. Based on parallax measurements taken by the Gaia mission, it is about 16.3 light-years from the Sun.

<span class="mw-page-title-main">Theta Eridani</span> Star in the constellation Eridanus

Theta Eridani, Latinized from θ Eridani, is a binary system in the constellation of Eridanus with a combined apparent magnitude of 2.88. Its two components are designated θ1 Eridani, formally named Acamar, and θ2 Eridani. The system's distance from the Sun based on parallax measurements is approximately 165 light-years.

p Eridani is a binary star system in the constellation of Eridanus whose distance from the Sun is 26.7 light-years based upon parallax. It was found to be a double star in December 1825 by James Dunlop in Australia at his home at Paramatta, now spelt Parramatta. It is visible to the naked eye as a dim, orange-hued star. The system is moving further from the Earth with a heliocentric radial velocity of about +20 km/s.

HD 113703, also known by the Bayer designation f Centauri, is a multiple star system in the southern constellation of Centaurus. The combined apparent visual magnitude of this system is +4.71, which is sufficient to make it faintly visible to the naked eye. The distance to this system is approximately 400 light years based on parallax measurements. It is a member of the Lower Centaurus Crux subgroup of the Scorpius–Centaurus association.

<span class="mw-page-title-main">58 Eridani</span> Star in the constellation Eridanus

58 Eridani is a main-sequence star in the constellation Eridanus. It is a solar analogue, having similar physical properties to the Sun. The star has a relatively high proper motion across the sky, and it is located 43 light years distant. It is a probable member of the IC 2391 moving group of stars that share a common motion through space.

HD 142022 is a binary star system located in the southernmost constellation of Octans. It is too faint to be visible to the naked eye, having an apparent visual magnitude of 7.70. The distance to this system is 112 light-years based on parallax, but it is drifting closer to the Sun with a radial velocity of −10 km/s.

HD 196050 is a triple star system located in the southern constellation of Pavo. This system has an apparent magnitude of 7.50 and the absolute magnitude is 4.01. It is located at a distance of 165 light-years from the Sun based on parallax, and is drifting further away with a radial velocity of +61 km/s. It is also called by the Hipparcos designation HIP 101806.

HD 88836, also known as HR 4019, is a solitary, yellow-hued star located in the southern constellation Antlia. It has an apparent magnitude of 6.32, placing it near the limit for naked eye visibility. Based on an annual parallax shift of 7.019 mas, the object is estimated to be 465 light years away from the Solar System. Its distance from the Sun does not appear to be changing, having a radial velocity of 0 km/s.

HD 156768 is a double star in the southern constellation of Ara, with a combined apparent magnitude of 5.86. The brighter component is a sixth magnitude bright giant or supergiant star with a stellar classification of G8Ib/II. The magnitude 9.6 companion lies at an angular separation of 1.81″ along a position angle of 184°.

HD 3 is a single, white-hued star in the northern constellation Andromeda. With an apparent visual magnitude of 6.71, it is below the nominal brightness limit for visibility with the typical naked eye but may still be visible by some observers under ideal viewing conditions. It is also the first star indexed in the Bright Star Catalogue. Based upon an annual parallax shift of 6.3137±0.0826 mas, it is located roughly 517 light years away. The star is moving closer with a heliocentric radial velocity of −18 km/s, and will make perihelion in around 2.9 million years at a separation of around 351 ly (107.71 pc).

BD−17 63 is a low-mass K type star in the southern constellation Cetus. It is a 9th magnitude star at a distance of 113 light years from Earth.

HD 190984, also known as HIP 99496, is a star located in the southern circumpolar constellation Pavo, the peacock. It has an apparent magnitude of 8.76, making it readily visible in small telescopes, but not to the naked eye. Based on parallax measurements from the Gaia spacecraft, the object is estimated to be 486 light years away from the Solar System. It appears to be receding with a heliocentric radial velocity of 20.3 km/s.

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

29 Cygni is a single star in the northern constellation of Cygnus. It is dimly visible to the naked eye as a white-hued star with an apparent visual magnitude of 4.93. The distance to 29 Cyg, as estimated from an annual parallax shift of 24.5 mas, is 133 light years. The star is moving closer to the Earth with a heliocentric radial velocity of −17 km/s. It is a member of the 30–50 million year old Argus Association of co-moving stars.

Upsilon³ Eridani, officially named Beemim, is a star in the constellation of Eridanus. It is visible to the naked eye with an apparent visual magnitude of 3.96 The distance to this star, based upon an annual parallax shift of 11.01 mas, is around 296 light-years.

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

64 Eridani is a single, yellow-white hued star in the constellation Eridanus having variable star designation S Eridani. It is faintly visible to the naked eye with an apparent visual magnitude of 4.77. The annual parallax shift is measured at 12.01 mas, which equates to a distance of about 272 light years. In addition to its proper motion, it is moving closer to the Sun with a radial velocity of around −9 km/s.

<span class="mw-page-title-main">31 Cygni</span> Triple star system in the constellation Cygnus

31 Cygni, also known as ο1 Cygni, Omicron1 Cygni, or V695 Cygni, is a triple star system about 750 light years away in the constellation Cygnus.

HD 63399 is an orange hued star located in the southern constellation Puppis, the poop deck. It has an apparent magnitude of 6.45, placing it near the limit for naked eye visibility. Based on parallax measurements from Gaia DR3, the object is estimated to be 445 light years distant. It appears to be receding with a spectroscopic radial velocity of 28.5 km/s. At its current distance, HD 63399 is diminished by 0.29 magnitudes due to interstellar dust.

<span class="mw-page-title-main">TU Corvi</span> Star in the constellation Corvus

TU Corvi is a yellow-white hued star in the southern constellation of Corvus. It is a dimly visible to the naked eye with an apparent visual magnitude of 6.20. The distance to this star can be estimated from its annual parallax shift of 13.3 mas, yielding a range of about 246 light years. Based upon measured changes in its proper motion, it may be a close binary system.

<span class="mw-page-title-main">HD 53367</span> Binary star system in the constellation Monoceros

HD 53367 is a triple star system in the constellation of Monoceros. The primary star was identified as a variable Herbig Ae/Be star in 1989. Its companion, spectroscopically discovered in 2006, is a pre-main-sequence star star with an average separation of 1.7 AU. The star system is embedded in the extended nebula IC 2177.

References

  1. 1 2 3 4 5 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID   244398875. Gaia DR3 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. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID   244398875. Gaia DR3 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 (2): 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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