HD 90132

Last updated
HD 90132
Antlia constellation map.svg
Red circle.svg
Location of HD 90132 in red
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Antlia
Right ascension 10h 23m 29.29608s [1]
Declination −38° 00′ 35.4255″ [1]
Apparent magnitude  (V)5.33±0.01 [2]
Characteristics
Spectral type A8 V [3]
B−V color index +0.25 [4]
Astrometry
Radial velocity (Rv)17±4.2 [5]  km/s
Proper motion (μ)RA: −158.833  mas/yr [1]
Dec.: −53.705  mas/yr [1]
Parallax (π)24.2034 ± 0.0725  mas [1]
Distance 134.8 ± 0.4  ly
(41.3 ± 0.1  pc)
Absolute magnitude  (MV)+2.25 [6]
Details
Mass 1.69±0.27 [7]   M☉
Radius 1.87±0.87 [7]   R☉
Luminosity 9.79±0.06 [8]   L☉
Surface gravity (log g)4.15 [9]   cgs
Temperature 7,737±263 [9]   K
Metallicity [Fe/H]−0.13 [10]   dex
Rotational velocity (v sin i)270 [11]  km/s
Age 70 [12]   Myr
Other designations
64 G. Antliae [13] , CD−37°6509, CPD−37°4123, FK5  1269, GC  14281, HD  90132, HIP  50888, HR  4086, SAO  201346 [14]
Database references
SIMBAD data

HD 90132 (HR 4086) is a solitary [15] white hued star located in the southern constellation Antlia. It has an apparent magnitude of 5.33, [2] making it one of the brighter members of this generally faint constellation. The star is relatively close at a distance of 135 light years [1] but is receding with a heliocentric radial velocity of 17  km/s . [5]

HD 90132 has a stellar classification of A8 V, [3] indicating that it is an ordinary A-type main-sequence star. At present it has 1.69 times the mass of the Sun and 1.87 times the radius of the Sun. [7] Despite a young age of 70 million years, [12] the star has a lower surface gravity than expected. [9] This is due to the equator being 18% larger than the poles, [16] which is due to a high projected rotational velocity of 270  km/s . [11] Nevertheless, it shines with a luminosity of 9.8  L☉ [8] from its photosphere at an effective temperature of 7,737  K . [9] HD 90132 is slightly metal deficient with a metallicity 74% that of Sun. [10]

This star was observed for infrared excess suggesting the presence of a circumstellar disk, but as of 2017 no excess have been found. [17]

Related Research Articles

HD 27274, also known as Gliese 167, is a solitary, orange hued star located in the southern constellation Dorado. It has an apparent magnitude of 7.63, making it readily visible in binoculars, but not to the naked eye. Based on parallax measurements from the Gaia spacecraft, the star is known to be located 42.5 light-years away from the Solar System However, it is drifting closer with a heliocentric radial velocity of −23 km/s. At its current distance, HD 27274 is dimmed down by 0.05 magnitudes due to interstellar dust.

<span class="mw-page-title-main">HD 24479</span> Star in the constellation Camelopardalis

HD 24479, also designated as HR 1204, is a solitary, bluish-white hued star located in the northern circumpolar constellation Camelopardalis. The star is visible to the naked eye with an apparent visual magnitude of 5.04. Based on Gaia DR3 parallax measurements, it is located 385 light years from the Sun. However, it is receding with a somewhat constrained heliocentric radial velocity of 4.6 km/s. At its current distance, HD 24479's brightness is diminished by 0.29 magnitudes due to interstellar dust.

<span class="mw-page-title-main">HD 203842</span> Star in the constellation Equuleus

HD 203842, also known as HR 8191 or rarely 30 G. Equueli, is a solitary, yellowish-white hued star located in the constellation Equuleus. It has an apparent magnitude of 6.32, placing it near the limit for naked eye visibility, even under ideal conditions. Gaia DR3 parallax measurements imply a distance of 374 light years, and it is currently drifting closer with a somewhat constrained heliocentric radial velocity of −21.8 km/s. At its current distance HD 203842's brightness is diminished by 0.15 magnitudes due to interstellar dust and it has an absolute magnitude of +1.06.

HD 201507, also designated HR 8095, is a white-hued star located in the equatorial constellation Equuleus. It has an apparent magnitude of 6.43, placing it near the limit for naked eye visibility. Parallax measurements place the object at a distance of 214 light years and it is currently drifting closer with a heliocentric radial velocity of −43 km/s.

HD 97413 is a binary star located in the southern constellation Centaurus. The system has a combined magnitude of 6.27, placing it near the limit for naked eye visibility. Based on parallax measurements from the Gaia spacecraft, the system is located 320 light years away from the Solar System.

HD 72337, also known as HR 3370, is a solitary, bluish-white hued star located in the southern constellation Volans. With an apparent magnitude of 5.51, it is faintly visible to the unaided eye but only under ideal conditions.

<span class="mw-page-title-main">HD 26764</span> Star in the constellation Camelopardalis

HD 26764, also known as HR 1314 or rarely 14 H. Camelopardalis, is a solitary white hued star located in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.19, making it faintly to the naked eye if viewed under good conditions. Gaia DR3 parallax measurements place the object at a distance of 266 light years and is drifting closer with a poorly constrained heliocentric radial velocity of 3 km/s. At its current distance, HD 26764's brightness is diminished by 0.26 magnitudes due to interstellar dust.

HD 28454, also known as HR 1418, is a solitary, yellowish-white hued star located in the southern constellation Caelum, the chisel. It has an apparent magnitude of 6.1, making it faintly visible to the naked eye under ideal conditions. This star is located relatively close at a distance of about 107 light years based on parallax measurements of Gaia DR3 but is receding with a heliocentric radial velocity of 15 km/s.

HD 208741, also known as HR 8380, is a yellowish-white hued star located in the southern circumpolar constellation Octans. It has an apparent magnitude of 5.91, making it faintly visible to the naked eye. Parallax measurements place it at a distance of 211 light years, and it is currently receding with a heliocentric radial velocity of 8 km/s.

HD 183552, also known as HR 7411, is a probable spectroscopic binary located in the southern constellation Telescopium. The system has a combined apparent magnitude of 5.74, allowing it to be faintly visible to the naked eye. Based on parallax measurements from the Gaia spacecraft, it is estimated to be 337 light years distant. The value is horribly constrained, but it appears to receding with a radial velocity of 14 km/s.

HD 58425, also known as HR 2830, is an astrometric binary located in the northern circumpolar constellation Camelopardalis. It is faintly visible to the naked eye as an orang point of light at an apparent magnitude of 5.64. Based on parallax measurements from Gaia DR3, the system is estimated to be 470 light years away from Earth. It appears to be rapidly receding from the Sun, having a heliocentric radial velocity of 58.6 km/s. HD 58425 is listed as 54 Ursae Majoris in Johann Hevelius' catalogue, but this was dropped after the official IAU's official constellation borders were drawn.

HD 10455, also known as HR 4595, is a star located in the southern circumpolar constellation Octans. It has an apparent magnitude of 6.02, allowing it to be faintly visible to the naked eye. Based on parallax measurements from Gaia Data Release 3, it is estimated to be 336 light years distant. It appears to be receding from the Solar System, having a heliocentric radial velocity of 17.1 km/s.

HD 50885, also known as HR 2581, is a star located in the northern circumpolar constellation Camelopardalis, the giraffe. It has an apparent magnitude of 5.69, making it faintly visible to the naked eye if viewed under ideal conditions. Based on parallax measurements from Gaia DR3, the object is estimated to be 513 light years distant. It appears to be approaching the Solar System with a heliocentric radial velocity of −17.8 km/s.

HR 8526, also known as HD 212168, is the primary of a triple star located in the southern circumpolar constellation Octans. The star and its companion have apparent magnitudes of 6.12 and 9.36 respectively. The system is located relatively close at a distance of 76 light years based on Gaia DR3 parallax measurements, but is receding with a heliocentric radial velocity of 15 km/s.

<span class="mw-page-title-main">40 Leonis Minoris</span> Binary star system in the constellation of Leo Minor

40 Leonis Minoris is a white hued star located in the northern constellation Leo Minor. It is rarely called 14 H. Leonis Minoris, which is the designation given by Polis astronomer Johann Hevelius.

<span class="mw-page-title-main">HD 201772</span> Star in the constellation Microscopium

HD 201772, also known as HR 8104, is a yellowish-white hued star located in the southern constellation Microscopium. It has an apparent magnitude of 5.26, making it one of the brighter members of this generally faint constellation. The object is located relatively close at a distance of 111 light-years based on Gaia DR3 parallax measurements but is approaching closer with a heliocentric radial velocity of −41 km/s. At its current distance, HD 201772's brightness is diminished by 0.11 magnitudes due to interstellar dust.

<span class="mw-page-title-main">HD 22764</span> Double star; Camelopardalis

HD 22764, also known as HR 1112, is an orange hued star located in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.78, allowing it to be faintly visible to the naked eye. The object is located relatively far at a distance of approximately 1,770 light years based on Gaia DR3 parallax measurements but is approaching the Solar System with a heliocentric radial velocity of −12.5 km/s. At its current distance, HD 22764's brightness is diminished by 0.66 magnitudes due to interstellar dust.

<span class="mw-page-title-main">HD 174474</span> High proper motion star; Telescopium

HD 174474, also designated as HR 7095 or rarely 35 G. Telescopii, is a solitary white-hued star located in the southern constellation Telescopium. It has an apparent magnitude of 6.17, placing it near the limit for naked eye visibility. The object is located relatively close at a distance of 244 light years based on Gaia DR3 parallax measurements but is drifting closer with a heliocentric radial velocity of −44 km/s. At its current distance, HD 174474's brightness is diminished by 0.26 magnitudes due to interstellar dust. It has an absolute magnitude of +1.61.

<span class="mw-page-title-main">HD 24141</span> Am star?; Camelopardalis

HD 24141, also known as HR 1192, is a star located in the northern constellation Camelopardalis, the giraffe. It is faintly visible to the naked eye as a white-hued point of light with an apparent magnitude of 5.79. The object is located relatively close at a distance of 176 light-years based on Gaia DR3 parallax measurements and it is slowly drifting closer with a heliocentric radial velocity of −0.2 km/s. At its current distance, HD 24141's brightness is diminished by 0.17 magnitudes due to interstellar extinction and it has an absolute magnitude of +2.28.

<span class="mw-page-title-main">HD 27322</span> A-type dwarf; Camelopardalis

HD 27322, also known as HR 1342, is a binary star located in the northern circumpolar constellation Camelopardalis. The visible component is faintly visible to the naked eye as a white-hued point of light with an apparent magnitude of 5.92. The object is located relatively close at a distance of 313 light-years based on Gaia DR3 parallax measurements, and it is drifting closer with a heliocentric radial velocity of approximately −13 km/s. At its current distance, HD 27322's brightness is diminished by 0.24 magnitudes due to interstellar extinction and it has an absolute magnitude of +0.98.

References

  1. 1 2 3 4 5 6 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.
  2. 1 2 Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H. ISSN   0004-6361.
  3. 1 2 Houk, N. (1982). Michigan Catalogue of Two-dimensional Spectral Types for the HD stars. Volume_3. Declinations −40° to −26°. Bibcode:1982mcts.book.....H.
  4. ↑ Johnson, H. L.; Mitchell, R. I.; Iriarte, B.; Wisniewski, W. Z. (1966). "UBVRIJKL Photometry of the Bright Stars". Communications of the Lunar and Planetary Laboratory. 4: 99–110. Bibcode:1966CoLPL...4...99J.
  5. 1 2 Gontcharov, G. A. (November 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. eISSN   1562-6873. ISSN   1063-7737. S2CID   119231169.
  6. ↑ Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331–346. arXiv: 1108.4971 . Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. eISSN   1562-6873. ISSN   1063-7737. S2CID   255204555.
  7. 1 2 3 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.
  8. 1 2 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.
  9. 1 2 3 4 David, Trevor J.; Hillenbrand, Lynne A. (12 May 2015). "The Ages of Early-type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets". The Astrophysical Journal. 804 (2): 146. arXiv: 1501.03154 . Bibcode:2015ApJ...804..146D. doi: 10.1088/0004-637X/804/2/146 . eISSN   1538-4357.
  10. 1 2 Netopil, Martin (4 May 2017). "Metallicity calibrations for dwarf stars and giants in the Geneva photometric system". Monthly Notices of the Royal Astronomical Society. 469 (3): 3042–3055. arXiv: 1705.00883 . Bibcode:2017MNRAS.469.3042N. doi: 10.1093/mnras/stx1077 . eISSN   1365-2966. ISSN   0035-8711.
  11. 1 2 Huang, Su-Shu (September 1953). "A Statistical Study of the Rotation of the Stars". The Astrophysical Journal. 118: 285. Bibcode:1953ApJ...118..285H. doi: 10.1086/145751 . eISSN   1538-4357. ISSN   0004-637X.
  12. 1 2 Vican, Laura (2 May 2012). "Age Determination for 346 Nearby Stars in the Herschel DEBRIS Survey". The Astronomical Journal. 143 (6): 135. arXiv: 1203.1966 . Bibcode:2012AJ....143..135V. doi: 10.1088/0004-6256/143/6/135 . eISSN   1538-3881. ISSN   0004-6256.
  13. ↑ Gould, Benjamin Apthorp (January 1879). "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.
  14. ↑ "HD 90132". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 20 September 2015.
  15. ↑ Eggleton, P. P.; Tokovinin, A. A. (11 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 . eISSN   1365-2966. ISSN   0035-8711.
  16. ↑ van Belle, Gerard T. (14 March 2012). "Interferometric observations of rapidly rotating stars". The Astronomy and Astrophysics Review. 20 (1): 51. arXiv: 1204.2572 . Bibcode:2012A&ARv..20...51V. doi: 10.1007/s00159-012-0051-2 . eISSN   1432-0754. ISSN   0935-4956.
  17. ↑ Meshkat, Tiffany; Mawet, Dimitri; Bryan, Marta L.; Hinkley, Sasha; Bowler, Brendan P.; Stapelfeldt, Karl R.; Batygin, Konstantin; Padgett, Deborah; Morales, Farisa Y.; Serabyn, Eugene; Christiaens, Valentin; Brandt, Timothy D.; Wahhaj, Zahed (21 November 2017). "A Direct Imaging Survey ofSpitzer-detected Debris Disks: Occurrence of Giant Planets in Dusty Systems". The Astronomical Journal. 154 (6): 245. arXiv: 1710.04185 . Bibcode:2017AJ....154..245M. doi: 10.3847/1538-3881/aa8e9a . eISSN   1538-3881.
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.