HD 54893

Last updated
HD 54893
Puppis constellation map.svg
Red circle.svg
Location of HD 54893 (circled)
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Puppis
Right ascension 07h 08m 51.06814s [1]
Declination −39° 39′ 20.3590″ [1]
Apparent magnitude  (V)4.83 [2]
Characteristics
Spectral type B2IV-V [3]
U−B color index −0.69 [2]
B−V color index −0.18 [2]
Variable type suspected β Cep [4]
Astrometry
Radial velocity (Rv)+19.50 [5]  km/s
Proper motion (μ)RA: −10.577 [1]   mas/yr
Dec.: +7.785 [1]   mas/yr
Parallax (π)3.7743 ± 0.0894  mas [1]
Distance 860 ± 20  ly
(265 ± 6  pc)
Absolute magnitude  (MV)−2.05 [6]
Details
Mass 6.3 [1]   M☉
Radius 7.0 [1]   R☉
Luminosity 2,389 [1]   L☉
Surface gravity (log g)3.56 [1]   cgs
Temperature 15,974 [1]   K
Metallicity [Fe/H]+0.20 [1]   dex
Rotational velocity (v sin i)42.8 [7]  km/s
Age 21.6 [8]   Myr
Other designations
A Puppis, 67 G. Puppis [9] , NSV  3431, CD−39°3105, FK5  2551, GC  9463, HD  54893, HIP  34495, HR  2702, SAO  197632
Database references
SIMBAD data
A light curve for HD 54893, plotted from TESS data HD54893LightCurve.png
A light curve for HD 54893, plotted from TESS data

HD 54893, often called A Puppis is a suspected variable star in the constellation Puppis. Its apparent magnitude is 4.83 and is approximately 860 light years away based on parallax.

With a mass over six times that of the Sun, HD 54893 is a hot luminous star with an effective temperature of about 16,000  K and a bolometric luminosity of 2,400  L☉. The spectral class of B2IV/V suggest it is on the border between the main sequence and the subgiant branch. Evolutionary models show it is towards the end of the main sequence at an age of about 22 million years.

In a 1971 paper, HD 54893 is mentioned as being a confirmed β Cephei variable, but with no explanation of when it was discovered. [11] A 1971 thesis dedicated to β Cephei variables only mentions HD 54893 as a non-variable early B star. [12] In a 1977 search for β Cephei stars, it is listed as possibly being variable. [13] It is catalogued as a suspected variable star, but not confirmed. [4]

Related Research Articles

<span class="mw-page-title-main">Omicron Velorum</span> Variable star in the constellation Vela

Omicron Velorum is a star in the constellation Vela. It is the brightest member of the loose naked eye open cluster IC 2391, also known as the ο Velorum Cluster.

<span class="mw-page-title-main">Nu Caeli</span> Star in the constellation Caelum

Nu Caeli is a yellow-white hued star in the constellation Caelum. It has an apparent visual magnitude of 6.07, which indicates it is near the lower limit on brightness that is visible to the naked eye. According to the Bortle scale, the star can be viewed from dark suburban skies. Based upon an annual parallax shift of 20.3 mas as seen from Earth, this star is located 161 light years from the Sun.

<span class="mw-page-title-main">15 Vulpeculae</span> Star in the constellation Vulpecula

15 Vulpeculae is a variable star in the northern constellation of Vulpecula, located approximately 243 light years away based on parallax. It has the variable star designation NT Vulpeculae; 15 Vulpeculae is the Flamsteed designation. It is visible to the naked eye as a faint, white-hued star with a typical apparent visual magnitude of 4.66. This object is moving closer to the Earth with a heliocentric radial velocity of −26 km/s.

<span class="mw-page-title-main">Xi Leonis</span> Star in the constellation Leo

Xi Leonis is a solitary star in the zodiac constellation of Leo. It has an apparent visual magnitude of 5.0 and is faintly visible to the naked eye. The distance to this star, as determined by parallax measurements, is roughly 229 light years.

<span class="mw-page-title-main">V381 Cephei</span> Triple star system in the constellation Cepheus

V381 Cephei is a triple star system in the northern constellation of Cepheus. Its apparent magnitude is slightly variable between 5.5 and 5.7.

<span class="mw-page-title-main">19 Monocerotis</span> Star in the constellation Monoceros

19 Monocerotis is a single, variable star in the equatorial constellation of Monoceros, located approximately 1,220 light years away from the Sun based on parallax. It has the variable star designation V637 Monocerotis, while 19 Monocerotis is the Flamsteed designation. This object is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of 5.00. It is receding from the Earth with a heliocentric radial velocity of +25 km/s.

<span class="mw-page-title-main">22 Orionis</span> Binary star system in the constellation Orion

22 Orionis is a binary star in the equatorial constellation of Orion. It has the Bayer designation o Orionis, while 22 Orionis is the Flamsteed designation. This system is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of 4.74. It is located approximately 1,100 light years away from the Sun based on parallax. The system is moving further from the Earth with a heliocentric radial velocity of +28.80

<span class="mw-page-title-main">Lambda Pavonis</span> Star in the constellation Pavo

λ Pavonis, Latinized as Lambda Pavonis, is a single, variable star in the southern constellation of Pavo. It is a blue-white hued star that is faintly visible to the naked eye with an apparent visual magnitude that fluctuates around 4.22. This object is located approximately 1,400 light years from the Sun, based upon parallax. It is a member of the Scorpius–Centaurus association.

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

Rho Pavonis, Latinized from ρ Pavonis, is a single, variable star in the southern constellation of Pavo. It is yellow-white in hue and faintly visible to the naked eye with an apparent visual magnitude that fluctuates around 4.86. The star is located at a distance of approximately 190 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +8 km/s. It is a candidate outlying member of the Tucana Association of co-moving stars.

<span class="mw-page-title-main">Kappa Phoenicis</span> Star in the constellation Phoenix

κ Phoenicis, Latinized as Kappa Phoenicis, is a single star in the southern constellation of Phoenix. It is visible to the naked eye as a white-hued point of light with an apparent visual magnitude of 3.94. The distance to this star is approximately 77.7 light years based on parallax, and it is drifting further away with a radial velocity of +11 km/s. It is a member of the Castor Moving Group of co-moving stars.

<span class="mw-page-title-main">V Puppis</span> Variable star in the constellation Puppis

V Puppis is a star system in the constellation Puppis. Its apparent magnitude is 4.41. There is a binary star system at the center with a B1 dwarf orbiting a B3 subgiant star. They have an orbital period of 1.45 days and a distance of only 15 solar radii apart. However, the system moves back and forth, indicating that there is a massive object orbiting them with a period around 5.47 years. Based on the mass of the object, its lack of a visible spectrum, and circumstellar matter in the system with many heavy elements, it is probably a black hole. However, a follow-up study could not confirm this object, but found signs that there may be a third object which is fainter than the other components.

<span class="mw-page-title-main">QZ Puppis</span> Star in the constellation Puppis

QZ Puppis is a class B2.5V star in the constellation Puppis. Its apparent magnitude is 4.5 and it is approximately 650 light years away based on parallax.

<span class="mw-page-title-main">1 Puppis</span> Star in the constellation Puppis

1 Puppis is a single star in the southern constellation of Puppis. It lies in the northern part of the constellation at a distance of about 790 ly, east of Aludra in Canis Major and just north of the white supergiant, 3 Puppis. This object is visible to the naked eye as a faint, red-hued star with an apparent visual magnitude of 4.59. It is moving further from the Earth with a heliocentric radial velocity of +32.4 km/s.

<span class="mw-page-title-main">NV Puppis</span> Star in the constellation Puppis

NV Puppis, also known as υ1 Puppis, is a class B2V star in the constellation Puppis. Its apparent magnitude is 4.67 and it is approximately 800 light years away based on parallax.

<span class="mw-page-title-main">HD 59890</span> Star in the constellation Puppis

HD 59890 is a class G3Ib yellow supergiant star in the constellation Puppis. Its apparent magnitude is 4.65 and it is approximately 1,360 light years away based on parallax.

<span class="mw-page-title-main">MX Puppis</span> Star in the constellation Puppis

MX Puppis is a class B1.5IV star in the constellation Puppis. Its apparent magnitude varies irregularly between magnitude 4.6 and 4.9 and it is classified as a Gamma Cassiopeiae variable. It is approximately 930 light years away based on parallax.

<span class="mw-page-title-main">KQ Puppis</span> Binary star in the constellation Puppis

KQ Puppis is a spectroscopic binary variable star in the constellation Puppis. A red supergiant star and a hot main sequence star orbit each other every 9,742 days. Its apparent magnitude varies between 4.82 and 5.17.

NW Puppis, also known as υ2 Puppis, is a star in the constellation Puppis. Located around 910 light-years distant, it shines with a luminosity approximately 1,108 times that of the Sun and has a surface temperature of 15,000 K. Anamarija Stankov ruled this star out as a Beta Cephei variable.

<span class="mw-page-title-main">R Puppis</span> Variable star in the constellation Puppis

R Puppis is a variable star in the constellation Puppis. It is a rare yellow hypergiant and a candidate member of the open cluster NGC 2439. It is also an MK spectral standard for the class G2 0-Ia.

<span class="mw-page-title-main">UX Orionis</span> Variable star in the constellation Orion

UX Orionis is a variable star in the constellation of Orion. It is a Herbig Ae star, located about 1000 light years from the Earth. At its brightest it is a magnitude 9.5 object, so it is too faint to be seen with the naked eye. UX Orionis is the prototype of the UX Orionis class of variable stars, which are young stellar objects that exhibit large, irregular changes in visual band brightness. UX Orionis was discovered by Henrietta Swan Leavitt.

References

  1. 1 2 3 4 5 6 7 8 9 10 11 Gaia Collaboration; et al. (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674. 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 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
  3. ↑ Hiltner, W. A.; Garrison, R. F.; Schild, R. E. (July 1969). "MK Spectral Types for Bright Southern OB Stars". The Astrophysical Journal. 157: 313. Bibcode:1969ApJ...157..313H. doi: 10.1086/150069 . eISSN   1538-4357. ISSN   0004-637X.
  4. 1 2 Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  5. ↑ Wilson, R. E. (1953). "General Catalogue of Stellar Radial Velocities". Carnegie Institute Washington D.C. Publication. Carnegie Institution for Science. Bibcode:1953GCRV..C......0W. LCCN   54001336.
  6. ↑ 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. Vizier catalog entry
  7. ↑ Glebocki, R.; Gnacinski, P. (2005). "VizieR Online Data Catalog: Catalog of Stellar Rotational Velocities (Glebocki+ 2005)". VizieR On-line Data Catalog: III/244. Originally Published in: 2005csss...13..571G; 2005yCat.3244....0G. 3244. Bibcode:2005yCat.3244....0G.
  8. ↑ Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (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. Vizier catalog entry
  9. ↑ Gould, Benjamin Apthorp (1878). "Uranometria Argentina : brillantez y posicion de las estrellas fijas, hasta la septima magnitud, comprendidas dentro de cien grados del polo austral : con atlas". Resultados del Observatorio Nacional Argentino. 1. Bibcode:1879RNAO....1.....G.
  10. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  11. ↑ Percy, John R.; Madore, Katherine (1971). "On Stothers' and Simon's Binary-Star Hypothesis for Beta Canis Majoris Star Pulsation". International Astronomical Union Colloquium. 15: 197–203. doi: 10.1017/S0252921100032954 . S2CID   124791098.
  12. ↑ Watson, Robert Dudley (1971). A study of the beta Cephei stars (Thesis).
  13. ↑ Jerzykiewicz, M.; Sterken, C. (1977). "Search for beta Cephei stars south of declination -20 . I. Incidence of light variability among early B giants and subgiants - summer objects". Acta Astronomica. 27: 365. Bibcode:1977AcA....27..365J.
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.