HD 74423

Last updated

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

<span class="mw-page-title-main">RT Aurigae</span> Star in the constellation Auriga

RT Aurigae is a yellow supergiant variable star in the constellation Auriga, about 1,500 light years from Earth.

<span class="mw-page-title-main">Gamma Boötis</span> Binary star system in the constellation Boötes

Gamma Boötis, Latinised from γ Boötis, is a binary star system in the northern constellation of Boötes the herdsman, forming the left shoulder of this asterism. The primary component has the proper name Seginus, the traditional name of the Gamma Bootis system. It has a white hue and is visible to the naked eye with a typical apparent visual magnitude of +3.03. Based on parallax measurements obtained during the Hipparcos mission, it is located at a distance of approximately 85 light-years from the Sun, but is drifting closer with a radial velocity of −32 km/s.

<span class="mw-page-title-main">Iota Boötis</span> Binary star system in the northern constellation of Boötes

Iota Boötis is a member of a binary star system in the constellation Boötes, approximately 96 light-years from Earth. It has the traditional name Asellus Secundus and the Flamsteed designation 21 Boötis. The companion is HD 234121, a K0 main sequence star.

<span class="mw-page-title-main">Kappa Boötis</span> Double star in the constellation of Boötes

Kappa Boötis is a double star in the constellation Boötes. It has the traditional name Asellus Tertius and the Flamsteed designation 17 Boötis. The components are separated by an angular distance of 13.5 arcsec, viewable in a small telescope. Kappa Boötis is approximately 155 light years from Earth.

Lambda Geminorum, Latinized from λ Geminorum, is a candidate multiple star system in the constellation Gemini. It is visible to the naked eye at night with a combined apparent visual magnitude of 3.57. The distance to this system is 101 light years based on parallax, and it is drifting closer with a radial velocity of –7.4 km/s. It is a member of what is suspected to be a trailing tidal tail of the Hyades Stream.

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.

<span class="mw-page-title-main">4U 1700-37</span>

4U 1700-37 is one of the stronger binary X-ray sources in the sky, and is classified as a high-mass X-ray binary. It was discovered by the Uhuru satellite. The "4U" designation refers to the fourth Uhuru catalog.

<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.

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

S Cassiopeiae is a Mira variable and S-type star in the constellation Cassiopeia. It is an unusually cool star, rapidly losing mass and surrounded by dense gas and dust producing masers.

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

BD Phoenicis is a variable star in the constellation of Phoenix. From parallax measurements by the Gaia spacecraft, it is located at a distance of 256 light-years from Earth. Its absolute magnitude is calculated at 1.5.

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

AZ Phoenicis is a variable star in the constellation of Phoenix. It has an average visual apparent magnitude of 6.47, so it is at the limit of naked eye visibility. From parallax measurements by the Gaia spacecraft, it is located at a distance of 322 light-years from Earth. Its absolute magnitude is calculated at 1.65.

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

Rho Phoenicis is a variable star in the constellation of Phoenix. From parallax measurements by the Gaia spacecraft, it is located at a distance of 245 light-years from Earth.

<span class="mw-page-title-main">DH Cephei</span> Binary star system in the constellation Cepheus

DH Cephei is a variable binary star system in the northern circumpolar constellation of Cepheus, positioned about two degrees to the east of the star system Delta Cephei. With an apparent visual magnitude of 8.61, it is too faint to be visible without a telescope. Based on parallax measurements, this system is located at a distance of approximately 9.6 kilolight-years from the Sun. At present it is moving closer to the Earth with a radial velocity of −33 km/s.

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">HD 139319</span> Triple star system in constellation Draco

HD 139319 is a ternary system composed of the binary Algol variable star known as TW Draconis, and a main-sequence companion star at a separation of 3 arcseconds. The system lies in the constellation of Draco about 540 light years away.

<span class="mw-page-title-main">17 Comae Berenices</span> Multiple star system 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.

<span class="mw-page-title-main">HD 104237</span> Multiple star system in the constellation of Chamaeleon

HD 104237 is a candidate multiple star system in the southern constellation of Chamaeleon. It has the variable star designation DX Chamaeleontis, abbreviated DX Cha; HD 104237 is the stellar designation from the Henry Draper Catalogue. The system is dimly visible to the naked eye with an apparent visual magnitude that ranges from 6.59 down to 6.70. It is located at a distance of approximately 348 light-years from the Sun based on parallax measurements. The system is positioned just 2′ to the north-east of the 5th magnitude star Epsilon Chamaeleontis, and is a member of the ε Cha association of co-moving stars.

<span class="mw-page-title-main">RR Lyncis</span> Variable star in the constellation Lynx

RR Lyncis is a star system in the northern constellation of Lynx, abbreviated RR Lyn. It is an eclipsing binary of the Algol type; one of the closest in the northern sky at an estimated distance of approximately 263 light years based on parallax measurements. The system is faintly visible to the naked eye with a combined apparent visual magnitude of 5.53. During the primary eclipse the brightness drops to 6.03, while it decreases to magnitude 5.90 with the secondary eclipse. The system is drifting closer to the Sun with a radial velocity of −12 km/s.

<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">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.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.