HD 28375

Last updated
HD 28375
Taurus constellation map.svg
Red circle.svg
Location of HD 28375 (circled)
Observation data
Epoch J2000        Equinox J2000
Constellation Taurus
Right ascension 04h 28m 32.12178s [1]
Declination +01° 22′ 50.9687″ [1]
Apparent magnitude  (V)5.53 [2]
Characteristics
Spectral type B3V [3]
U−B color index -0.55 [4]
B−V color index −0.099±0.008 [2]
Astrometry
Radial velocity (Rv)18.0±4.3 [5]  km/s
Proper motion (μ)RA: +19.530 [1]   mas/yr
Dec.: −20.272 [1]   mas/yr
Parallax (π)6.8102 ± 0.1690  mas [1]
Distance 480 ± 10  ly
(147 ± 4  pc)
Absolute magnitude  (MV)0.19 [2]
Details
Mass 5.0±0.1 [6]   M☉
Luminosity 126.75 [2]   L☉
Surface gravity (log g)4 [3]   cgs
Temperature 13,000 [3]   K
Metallicity [Fe/H]0.05±0.06 [7]   dex
Rotational velocity (v sin i)13±3 [8]  km/s
Age 3.1±2.1 [6]   Myr
Other designations
BD+01°757, FK5  1123, GC  5441, HD  28375, HIP  20884, HR  1415, SAO  111845 [9]
Database references
SIMBAD data

HD 28375 is a single [10] star in the equatorial constellation of Taurus, near the southern constellation border with Eridanus. It was previously known by the Flamsteed designation 44 Eridani, although the name has fallen out of use because constellations were redrawn, placing the star out of Eridanus and into Taurus. The star is blue-white in hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.53. [2] The distance to this star is approximately 480  light-years based on parallax. [1] It is drifting further away with a radial velocity of 18 km/s, [5] after having come to within an estimated 249 light-years some 3.7 million years ago. [2]

Cowley (1972) and later Bragança et al. (2012) found a stellar classification of B3V [11] [12] for this object, matching a B-type main-sequence star. Houk and Swift assigned it a class of B5 III/IV, [13] suggesting it is a more evolved star that is entering the giant stage. It has five times the mass of the Sun and is around three million years old, [6] with a projected rotational velocity of just 13 km/s. [8] The star is radiating 127 [2] times the luminosity of the Sun from its photosphere at an effective temperature of about 13,000 K. [3]

An infrared excess has been detected, indicating the presence of a circumstellar disk. The dust has a temperature of about 119 K and is orbiting 67  AU from the star. [3]

Related Research Articles

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6 Andromedae is an astrometric binary star system in the northern constellation of Andromeda. The designation comes from the star catalogue of John Flamsteed, first published in 1712. Its apparent visual magnitude is 5.91, which is just bright enough to be visible to the naked eye under good seeing conditions. Based upon an annual parallax shift of 34.1 mas as seen from Earth, it is around 96 light years from the Sun. It is moving closer to the Sun with a radial velocity of −32.4 km/s. The system has a relatively high proper motion, advancing across the celestial sphere at the rate of 0.272 arc seconds per annum.

<span class="mw-page-title-main">20 Aquilae</span> Star in the constellation Aquila

20 Aquilae, abbreviated 20 Aql, is an irregular variable star in the equatorial constellation of Aquila. 20 Aquilae is its Flamsteed designation. It ranges in magnitude from a peak of 5.33 down to 5.36, which is bright enough for the star to be visible to the naked eye. The estimated distance to this star is around 920 light years, based upon an annual parallax shift of 3.5 mas. The star is moving closer to the Earth with a heliocentric radial velocity of −23 km/s.

18 Boötis is a single star in the northern constellation of Boötes, located about 85 light years away from the Sun. It is visible to the naked eye as a faint, yellow-white hued star with an apparent visual magnitude of 5.41. This object is a suspected member of the Ursa Major Moving Group, based on velocity criteria. It has a magnitude 10.84 optical companion at an angular separation of 163.7″ along a position angle of 219°, as of 2010.

32 Boötis is a single star in the northern constellation of Boötes, located 360 light years away from the Sun. It is visible to the naked eye as a faint, yellow-hued star with an apparent visual magnitude of 5.55. This object is moving closer to the Earth with a heliocentric radial velocity of −23 km/s. It has a relatively high proper motion, traversing the celestial sphere at the rate of 0.195 arc seconds per annum.

Lambda Canis Majoris is a solitary, blue-white hued star in the constellation Canis Major. Lambda CMa is visible to the naked eye with an apparent visual magnitude of +4.48. Based upon an annual parallax shift of 7.70 mas as seen from Earth, this star is located about 424 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction of 0.14 due to interstellar dust.

<span class="mw-page-title-main">HD 19275</span> Star in the constellation Cassiopeia

HD 19275 is a single star in the northern constellation of Cassiopeia. It has a white hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.85. The distance to HD 19275 is 163 light years as determined using parallax measurements. It is drifting further away from the Sun with a radial velocity of around 12 km/s.

<span class="mw-page-title-main">22 Scorpii</span> Star in the constellation Scorpius

22 Scorpii (i Scorpii) is a single star in the southern zodiac constellation of Scorpius, about one degree from Antares. It is faintly visible to the naked eye with an apparent visual magnitude of 4.78. The distance to this star is estimated to be around 410 light years, as derived from its annual parallax shift of 7.89±0.24 mas. The star is embedded in, or adjacent to, the diffuse nebulous cloud IC 4605 located in the western regions of the Rho Ophiuchi cloud complex.

<span class="mw-page-title-main">HD 110956</span> Star in the constellation Crux

HD 110956 is a single star in the southern constellation of Crux. It is faintly visible to the naked eye with an apparent visual magnitude of 4.62. The distance to this star is approximately 385 light years based on parallax and it is drifting further away with a radial velocity of 15.5 km/s. It is a probable member of the Lower Centaurus–Crux subgroup of the Scorpius–Centaurus association.

Psi Eridani, Latinized from ψ Eridani, is a star in the constellation Eridanus. With an apparent visual magnitude is 4.81, it can be seen with the naked eye on a clear, dark night. Based upon an annual parallax shift of 4.41 milliarcseconds, it is located roughly 740 light-years away from the Sun.

38 Geminorum is a binary star system in the northern zodiac constellation of Gemini. It has the Bayer designation e Geminorum, while 38 Geminorum is the Flamsteed designation. This system is visible to the naked eye as a faint, white-hued point of light with an apparent visual magnitude of 4.71. The primary component is a magnitude 4.75 star, while the secondary is magnitude 7.80. The system is located about 98 light years away from the Sun based on parallax, and is drifting further away with a radial velocity of +16 km/s. It is a potential member of the Tucana–Horologium stellar kinematic group.

Tau1 Hydrae is a triple star system in the equatorial constellation of Hydra. Based upon the annual parallax shift of the two visible components as seen from Earth, they are located about 18 parsecs (59 ly) from the Sun. The system has a combined apparent visual magnitude of +4.59, which is bright enough to be visible to the naked eye at night.

11 Librae is a single, fifth-magnitude star in the southern zodiac constellation of Libra. It is faintly visible to the naked eye with an apparent visual magnitude is 4.93. The star is moving further from the Sun with a heliocentric radial velocity of +83.6 km/s. The distance to this star, as estimated from its annual parallax shift of 14.92±0.40 mas, is about 219 light years.

Phi2 Lupi, Latinized from φ2 Lupi, is a solitary star in the southern constellation of Lupus. With an apparent magnitude of 4.535, it is bright enough to be seen with the naked eye. Based upon an annual parallax shift of 6.28 mas as seen from Earth, it is located around 520 light years from the Sun. At that distance, the visual magnitude of the star is diminished by an extinction factor of 0.052±0.013 due to interstellar dust. It is a member of the Upper Centaurus–Lupus subgroup of the Scorpius–Centaurus association.

HD 202628 is a single star in the southern constellation of Microscopium. It has an apparent visual magnitude of +6.7, which makes it too faint to be readily visible to the naked eye. The star is located at a distance of 77.7 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +12.1 km/s. The absolute magnitude of this star is 4.86.

HR 4699 is a single star in the southern constellation of Corvus. It is orange in hue and is dimly visible to the naked eye with an apparent visual magnitude of +5.14. This star is located at a distance of approximately 201 light years from the Sun based on parallax. It is drifting further away with a radial velocity of +14 km/s, after come to within 45.1 light-years some four million years ago.

HD 137366 is a solitary blue-hued star located in the southern circumpolar constellation Apus. It has an apparent magnitude of 6.38, placing it near the limit for naked eye visibility, even under ideal conditions. The object is located relatively far at a distance of approximately 1,100 light-years based on Gaia DR3 parallax measurements, but its heliocentric radial velocity is not known. At its current distance, HD 137366's brightness is diminished by three-tenths of a magnitudes due to interstellar extinction and it has an absolute magnitude of −1.54.

<span class="mw-page-title-main">32 Tauri</span> Yellow-white hued subgiant star in the constellation Taurus.

32 Tauri is the Flamsteed designation for a solitary star in the zodiac constellation of Taurus. It has a visual magnitude of 5.64, making it visible to the naked eye from suburban skies. The position of this star near the ecliptic plane means that it is subject to occultations by the Moon. Parallax measurements put it at a distance of 144 light years from the Sun. It is drifting further away with a radial velocity of +31.9 km/s, having come to within 88.9 light-years some 759,000 years ago.

<span class="mw-page-title-main">HD 111395</span> Star in the constellation Coma Berenices

HD 111395 is a single, variable star in the northern constellation of Coma Berenices. It has the variable star designation LW Com, short for LW Comae Berenices; HD 111395 is the Henry Draper Catalogue designation. The star has a yellow hue and is just bright enough to be barely visible to the naked eye with an apparent visual magnitude that fluctuates around 6.29. Based upon parallax measurements, it is located at a distance of 55.8 light years from the Sun. The star is drifting closer with a radial velocity of −8.9 km/s. It is a member of the Eta Chamaeleontis stellar kinematic group.

HD 196775 is a solitary star in the equatorial constellation Delphinus. It has an apparent magnitude of 5.98, allowing it to be faintly seen with the naked eye. The object is relatively far at a distance of 1,050 light years but is approaching the Solar System with a heliocentric radial velocity of −4.6 km/s. HD 196775 has a high peculiar velocity of 21.8+1.9
−4.1 km/s compared to neighboring stars, indicating that it may be a runaway star.

References

  1. 1 2 3 4 5 6 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 4 5 6 7 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.
  3. 1 2 3 4 5 Liu, Qiong; Wang, Tinggui; Jiang, Peng (2014). "Bright Debris Disk Candidates Detected with Theakari/far-Infrared Surveyor". The Astronomical Journal. 148 (1): 3. arXiv: 1308.5593 . Bibcode:2014AJ....148....3L. doi:10.1088/0004-6256/148/1/3. S2CID   117353888.
  4. ↑ Johnson, H. L. (1966). "UBVRIJKL Photometry of the Bright Stars". Communications of the Lunar and Planetary Laboratory. 4: 99. Bibcode:1966CoLPL...4...99J.
  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 Tetzlaff, N.; et al. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society, 410 (1): 190–200, arXiv: 1007.4883 , Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x, S2CID   118629873
  7. ↑ Gáspár, András; et al. (2016), "The Correlation between Metallicity and Debris Disk Mass", The Astrophysical Journal, 826 (2): 171, arXiv: 1604.07403 , Bibcode:2016ApJ...826..171G, doi: 10.3847/0004-637X/826/2/171 , S2CID   119241004.
  8. 1 2 Bragança, G. A.; Daflon, S.; Cunha, K.; Bensby, T.; Oey, M. S.; Walth, G. (2012). "Projected Rotational Velocities and Stellar Characterization of 350 B Stars in the Nearby Galactic Disk". The Astronomical Journal. 144 (5): 130. arXiv: 1208.1674 . Bibcode:2012AJ....144..130B. doi:10.1088/0004-6256/144/5/130. S2CID   118868235.
  9. ↑ "HD 28375". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-12-18.
  10. ↑ 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.
  11. ↑ Cowley, A. (November 1972), "Spectral classification of the bright B8 stars", Astronomical Journal, 77: 750–755, Bibcode:1972AJ.....77..750C, doi:10.1086/111348.
  12. ↑ Bragança, G. A.; et al. (November 2012), "Projected Rotational Velocities and Stellar Characterization of 350 B Stars in the Nearby Galactic Disk", The Astronomical Journal, 144 (5): 10, arXiv: 1208.1674 , Bibcode:2012AJ....144..130B, doi:10.1088/0004-6256/144/5/130, S2CID   118868235, 130.
  13. ↑ Houk, N.; Swift, C. (1999), "Michigan catalogue of two-dimensional spectral types for the HD Stars", Michigan Spectral Survey, 5, Bibcode:1999MSS...C05....0H
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