HD 74423

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HD 74423
HD74423LightCurve.png
A light curve for HD 74423 plotted from TESS data [1]
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Volans [2]
Right ascension 08h 40m 17.985s [3]
Declination −64° 50′ 16.84″ [3]
Apparent magnitude  (V)8.58–8.66 [4]
Characteristics
Spectral type A7VkA0mA0 λ Boo [5]
Apparent magnitude  (B)8.81±0.02 [6]
Apparent magnitude  (J)8.065±0.020 [6]
Apparent magnitude  (H)8.021±0.067 [6]
Apparent magnitude  (K)7.944±0.040 [6]
Variable type α2 CVn [4] or Ellipsoidal and δ Sct [7]
Astrometry
Proper motion (μ)RA: −9.719 [3]   mas/yr
Dec.: 11.732 [3]   mas/yr
Parallax (π)2.1018 ± 0.0150  mas [3]
Distance 1,550 ± 10  ly
(476 ± 3  pc)
Details
primary
Mass 2.1 [8]   M☉
Radius 3.3 [8]   R☉
Surface gravity (log g)3.6 [5]   cgs
Temperature 7,900 [8]   K
Metallicity [Fe/H]−1.0 [5]   dex
secondary
Mass 2.0 [8]   M☉
Radius 3.2 [8]   R☉
Surface gravity (log g)3.6 [5]   cgs
Temperature 7,600 [8]   K
Metallicity [Fe/H]−1.0 [5]   dex
Age 800 [7]   Myr
Other designations
HD  74423, CD−64°342, SAO  250298, TYC  8934-1662-1, TIC  355151781
Database references
SIMBAD data

HD 74423 is a heartbeat binary star and one component pulsates on only one hemisphere. This is caused by tidal interaction with its partner. [7] The star is located in the Volans constellation.

HD 74423 is slightly variable in brightness. It fluctuates between magnitudes 8.58 and 8.66 every 19 hours. [4] The exact variability type is unclear. It was initially found in a search for α2 Canum Venaticorum variables and assumed to be one, but has since been considered to be a δ Scuti variable. [7] The spectrum shows unusually strong absorption lines of some iron peak elements, a characteristic of λ Boötis stars. Both components are thought to show the chemical peculiarity. [7]

Related Research Articles

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<span class="mw-page-title-main">V1401 Aquilae</span> Star in the constellation Aquila

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Psi<sup>2</sup> Orionis Spectroscopic binary system in the constellation of Orion

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<span class="mw-page-title-main">AZ Phoenicis</span> A type variable star in the constellation Phoenix

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<span class="mw-page-title-main">Rho Phoenicis</span> Variable star in the constellation Phoenix

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HR 3831, also known as HD 83368, is a binary star system in the southern constellation of Vela at a distance of 233 light years. This object is barely visible to the naked eye as a dim, blue star with an apparent visual magnitude of 6.232. It is approaching the Earth with a heliocentric radial velocity of 4.0±0.3 km/s.

<span class="mw-page-title-main">FG Virginis</span> Variable star in the constellation Virgo

FG Virginis is a well-studied variable star in the equatorial constellation of Virgo. It is a dim star, near the lower limit of visibility to the naked eye, with an apparent visual magnitude that ranges from 6.53 down to 6.58. The star is located at a distance of 273.5 light years from the Sun based on parallax measurements, and is drifting further away with a radial velocity of +16 km/s. Because of its position near the ecliptic, it is subject to lunar occultations.

<span class="mw-page-title-main">HR 1217</span> Star in the constellation Eridanus

HR 1217 is a variable star in the constellation Eridanus. It has the variable star designation DO Eridani, but this seldom appears in the astronomical literature; it is usually called either HR 1217 or HD 24712. At its brightest, HR 1217 has an apparent magnitude of 5.97, making it very faintly visible to the naked eye for an observer with excellent dark-sky conditions.

<span class="mw-page-title-main">32 Virginis</span> Variable star in the constellation Virgo

32 Virginis, also known as FM Virginis, is a star located about 250 light years from the Earth, in the constellation Virgo. Its apparent magnitude ranges from 5.20 to 5.28, making it faintly visible to the naked eye of an observer well away from city lights. 32 Virginis is a binary star, and the more massive component of the binary is a Delta Scuti variable star which oscillates with a dominant period of 103.51 minutes.

<span class="mw-page-title-main">QQ Telescopii</span> Delta Scuti variable; Telescopium

QQ Telescopii, also known as HD 185139 or simply QQ Tel, is a solitary variable star located in the southern constellation Telescopium. It has an apparent magnitude of 6.25, placing it near the limit for naked eye visibility, even under ideal conditions. Gaia DR3 parallax measurements imply a distance of 333 light years and it is currently receding with a heliocentric radial velocity of 7.8 km/s. At its current distance, QQ Telescopii's brightness is diminished by two tenths of a magnitude due to interstellar dust and it has an absolute magnitude of +1.01.

References

  1. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. ↑ Staff (2 August 2008). "Finding the constellation which contains given sky coordinates". DJM.cc. Retrieved 31 July 2020.
  3. 1 2 3 4 5 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. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  4. 1 2 3 Bernhard, K.; Hümmerich, S.; Otero, S.; Paunzen, E. (2015). "A search for photometric variability in magnetic chemically peculiar stars using ASAS-3 data". Astronomy and Astrophysics. 581: A138. arXiv: 1507.01112 . Bibcode:2015A&A...581A.138B. doi:10.1051/0004-6361/201526424. S2CID   54062866.
  5. 1 2 3 4 5 Gray, R. O.; Riggs, Q. S.; Koen, C.; Murphy, S. J.; Newsome, I. M.; Corbally, C. J.; Cheng, K. -P.; Neff, J. E. (2017). "The Discovery of λ Bootis Stars: The Southern Survey I". The Astronomical Journal. 154 (1): 31. Bibcode:2017AJ....154...31G. doi: 10.3847/1538-3881/aa6d5e .
  6. 1 2 3 4 "HD 74423 -- Star". SIMBAD. Centre de Données astronomiques de Strasbourg . Retrieved 31 July 2020.
  7. 1 2 3 4 5 Handler, G.; Kurtz, D. W.; Rappaport, S. A.; Saio, H.; Fuller, J.; Jones, D.; Guo, Z.; Chowdhury, S.; Sowicka, P.; Aliçavuş, F. Kahraman; Streamer, M. (9 March 2020). "Tidally trapped pulsations in a close binary star system discovered by TESS". Nature Astronomy. 4 (7): 684–689. arXiv: 2003.04071 . Bibcode:2020NatAs...4..684H. doi:10.1038/s41550-020-1035-1. ISSN   2397-3366. S2CID   212634328.
  8. 1 2 3 4 5 6 Fuller, J.; Kurtz, D. W.; Handler, G.; Rappaport, S. (2020). "Tidally trapped pulsations in binary stars". Monthly Notices of the Royal Astronomical Society. 498 (4): 5730. arXiv: 2008.02836 . Bibcode:2020MNRAS.498.5730F. doi: 10.1093/mnras/staa2376 .
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