HD 116852

Last updated
HD 116852
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Chamaeleon
Right ascension 13h 30m 23.51858s [1]
Declination −78° 51′ 20.5477″ [1]
Apparent magnitude  (V)8.47 [2]
Characteristics
Spectral type O8.5 II-III ((f)) [3]
U−B color index −0.99 [4]
B−V color index −0.09 [2]
Astrometry
Radial velocity (Rv)−47±7.4 [5]  km/s
Proper motion (μ)RA: +7.197  mas/yr [1]
Dec.: −7.736  mas/yr [1]
Parallax (π)0.2823 ± 0.0293  mas [1]
Distance 6,309 [6]   pc
Absolute bolometric
magnitude  (Mbol)		−9.0 [7]
Details
Mass 15±0.7 [8]   M☉
Radius 18.9±1.0 [9]   R☉
Luminosity (bolometric)16,187 [8]   L☉
Surface gravity (log g)3.52±0.04 [10]   cgs
Temperature 34,000±500 [10]   K
Metallicity [Fe/H]−0.2 [11]   dex
Rotational velocity (v sin i)136 [12]  km/s
Age ~5 [7]   Myr
Other designations
CD−78°545, CPD−78°813, HD  116852, HIP  65890, TYC  9434-1988-1, GSC  09434-01988 [13]
Database references
SIMBAD data

HD 116852, also known as HIP 65890, is a solitary, [14] whitish-blue-hued star located in the southern circumpolar constellation Chamaeleon. It has an apparent magnitude of 8.47, making it readily visible in binoculars but not to the naked eye. The star is located relatively far at a distance of 6,310 parsecs [6] but is drifting closer with a heliocentric radial velocity of −47  km/s . [5] At its current distance, HD 116852's brightness is diminished by 0.67 magnitudes due to extinction from interstellar dust. [6] It has an absolute bolometric magnitude of −9.0. [7]

HD 116852 has a stellar classification of O8.5 II-III ((f)), [3] indicating that it is an evolved O-type star with a luminosity class intermediate between a bright giant and a regular giant star. The spectrum also includes a strong He II absorption accompanied by weak N III emissions. It has 15 times the mass of the Sun [8] and 19 times the solar radius. [9] It radiates a bolometric luminosity 16,187 times greater than the Sun [8] from its photosphere at an effective temperature of 34,000  K . [10] HD 116852 is metal deficient ([Fe/H] = −0.20) [11] and is estimated to be 5 million years old. [7] Like many hot stars the object spins rapidly, having a projected rotational velocity of 136  km/s . [12]

There is a cloud of highly ionized gas in the line-of-sight towards HD 116852. It was first noticed by astronomers Kenneth R. Sembach and Blair D. Savage in 1994. [15] The cloud in question contains an overabundance of carbon including other chemical elements such as silicon, phosphorus, nickel, and germanium. [15] HD 116852 has a high galactic latitude, indicating that it is currently in the galactic halo between the Scutum-Centaurus Arm and the Sagittarius-Carina Arm. [16] It is most likely a runaway star that was ejected from its birthplace into its current location. [17] [18]

Related Research Articles

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HD 165259, also known as HR 6751 is a triple star system located in the southern circumpolar constellation of Apus. It has an apparent magnitude of 5.86, making it faintly visible to the naked eye Parallax measurements place the system at a distance of 138 light years, and it is currently receding with a heliocentric radial velocity of 13.1 km/s.

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<span class="mw-page-title-main">HD 70514</span> Star in the constellation Volans

HD 70514, also known as HR 3280, is a solitary, orange hued star located in the southern circumpolar constellation Volans, the flying fish. It has an apparent magnitude of 5.06, making it one of the brighter members of this generally faint constellation. Based on parallax measurements from the Gaia spacecraft, the star is estimated to be 298 light years distant. It appears that its distance to the Solar System isn't changing, having a heliocentric radial velocity of 0 km/s. Eggen (1994) lists it as a member of the thin disk population.

HD 30080, also known as HR 1509, is a solitary, orange hued star located in the southern constellation Caelum, the chisel. It has an apparent magnitude of 5.66, allowing it to be faintly visible to the naked eye. Parallax measurements from Gaia DR3 place the object at a distance of 612 light years. It appears to be approaching the Solar System with a heliocentric radial velocity of −3.8 km/s. Eggen (1989) lists it as a member of the thick disk population.

<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.

<span class="mw-page-title-main">Theta Mensae</span> Star in the constellation Mensa

θ Mensae, Latinized to Theta Mensae, is a star located in the southern circumpolar constellation Mensa. It has an apparent magnitude of 5.45, making it faintly visible to the naked eye if viewed under ideal conditions. Based on parallax measurements from Gaia Data Release 3, the object is estimated to be 385 light years distant. The value is horribly constrained, but it appears to be receding with a heliocentric radial velocity of 6 km/s.

<span class="mw-page-title-main">HD 27022</span> Star in the constellation Camelopardalis

HD 27022, also known as HR 1327, is a star located in the northern circumpolar constellation Camelopardalis. The object has also been designated as 20 H. Camelopardalis, but is not commonly used in modern times. It has an apparent magnitude of 5.27, allowing it to be faintly visible to the naked eye. Based on parallax measurements from Gaia DR3, the star has been estimated to be 347 light years away. It appears to be approaching the Solar System, having a heliocentric radial velocity of −19.5 km/s.

<span class="mw-page-title-main">SY Equulei</span> High galactic latitude β Cephei variable

SY Equulei, also known as HD 203664, is a single variable star located in the equatorial constellation Equuleus. It has an average apparent magnitude of about 8.5, varying by a few hundredths of a magnitude, making it readily visible in binoculars and small telescopes, but not to the naked eye. The star is relatively far away at a distance of 8,000 light years and is receding with a heliocentric radial velocity of 48 km/s. At that distance, SY Equulei is dimmed by 0.19 magnitudes due to interstellar dust.

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 37289, also known as HR 1916, is a solitary, orange hued star located in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.61, making it faintly visible to the naked eye under ideal conditions. Based on parallax measurements from the Gaia spacecraft, the object is estimated to be 308 light years distant. It appears to be approaching the Sun, having a heliocentric radial velocity of −20.7 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.

<span class="mw-page-title-main">DR Chamaeleontis</span> Binary star in the constellation Chamaeleon

DR Chamaeleontis, also known as HD 93237, is a star located in the southern circumpolar constellation Chamaeleon. The system has an average apparent magnitude of 5.97, allowing it to be faintly visible to the naked eye. DR Cha is located relatively far at a distance of 1,060 light years based on Gaia DR3 parallax measurements, but is receding with a poorly constrained heliocentric radial velocity of 18 km/s.

<span class="mw-page-title-main">HD 36187</span> Star in the constellation of Columba

HD 36187, also known as HR 1835, is a solitary, bluish-white hued star located in the southern constellation Columba, the dove. It has an apparent magnitude of 5.55, making it faintly visible to the naked eye under ideal conditions. Based on parallax measurements from the Gaia spacecraft, it is estimated to be 282 light years away from the Solar System. However, it is receding rapidly with a heliocentric radial velocity of 50 km/s. At its current distance, HD 36187's brightness is diminished by 0.21 magnitude 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 117566</span> High proper motion star; Camelopardalis

HD 117566, also known as HR 5091, is a solitary yellow-hued star located in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.74, making it faintly visible to the naked eye. This object is relatively close at a distance of 291 light years based on Gaia DR3 parallax measurements but is receding with a heliocentric radial velocity of 14 km/s. At its current distance, HD 117566's brightness is diminished by 0.12 magnitudes due to interstellar dust.

<span class="mw-page-title-main">HD 167096</span> Binary star; Corona Australis

HD 167096, also known as HR 6818 or rarely 4 G. Coronae Australis, is a binary star located in the southern constellation Corona Australis. It has an apparent magnitude of 5.45, making it faintly visible to the naked eye. The system is located relatively close at a distance of 224 light years based on Gaia DR3 parallax measurements but is drifting closer with a poorly constrained heliocentric radial velocity of −27 km/s. At its current distance HD 167096's brightness is diminished by three tenths of a magnitudes due to interstellar dust and it has an absolute magnitude of +0.64.

HD 181295 is a star located in the southern constellation Telescopium. It has an apparent magnitude of 6.42, placing it near the limit of naked eye visibility, even under ideal conditions. The object is located relatively close at a distance of approximately 252 light-years based on Gaia DR3 parallax measurements, and it is currently drifting closer with a heliocentric radial velocity of −35.7 km/s. At its current distance, HD 181295's brightness is diminished by 0.22 magnitudes due to interstellar extinction and it has an absolute magnitude +2.14.

<span class="mw-page-title-main">HD 10390</span> B-type main-sequence star; Triangulum

HD 10390 is a solitary star located in the northern constellation Triangulum. It is faintly visible to the naked eye as a bluish-white hued point of light with an apparent magnitude of 5.64. The object is located relatively close at a distance of 292 light-years based on Gaia DR3 parallax measurements and it is drifting closer with a heliocentric radial velocity of −1.9 km/s. At its current distance, HD 10390's brightness is diminished by an interstellar extinction of only five-hundredths of a magnitude and it has an absolute magnitude of +1.00.

References

  1. 1 2 3 4 5 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. 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 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". VizieR Online Data Catalog. 2237. Bibcode:2002yCat.2237....0D.
  3. 1 2 Sota, A.; Apellániz, J. Maíz; Morrell, N. I.; Barbá, R. H.; Walborn, N. R.; Gamen, R. C.; Arias, J. I.; Alfaro, E. J. (25 February 2014). "The Galactic O-Star Spectroscopic Survey (GOSSS). II. Bright Southern Stars". The Astrophysical Journal Supplement Series. 211 (1): 10. arXiv: 1312.6222 . Bibcode:2014ApJS..211...10S. doi: 10.1088/0067-0049/211/1/10 . eISSN   1538-4365. ISSN   0067-0049.
  4. ↑ Hill, P. W.; Kilkenny, D.; van Breda, I. G. (September 1974). "UBV Photometry of Southern Early-type Stars at Intermediate Galactic Latitudes". Monthly Notices of the Royal Astronomical Society. 168 (3): 451–462. Bibcode:1974MNRAS.168..451H. doi: 10.1093/mnras/168.3.451 . eISSN   1365-2966. ISSN   0035-8711.
  5. 1 2 Kharchenko, N.V.; Scholz, R.-D.; Piskunov, A.E.; Röser, S.; Schilbach, E. (November 2007). "Astrophysical supplements to the ASCC-2.5: Ia. Radial velocities of ~55000 stars and mean radial velocities of 516 Galactic open clusters and associations". Astronomische Nachrichten. 328 (9): 889–896. arXiv: 0705.0878 . Bibcode:2007AN....328..889K. doi:10.1002/asna.200710776. eISSN   1521-3994. ISSN   0004-6337. S2CID   119323941.
  6. 1 2 3 Maíz Apellániz, J.; Barbá, R. H. (May 2018). "Optical-NIR dust extinction towards Galactic O stars". Astronomy & Astrophysics. 613: A9. arXiv: 1712.09228 . Bibcode:2018A&A...613A...9M. doi: 10.1051/0004-6361/201732050 . eISSN   1432-0746. ISSN   0004-6361.
  7. 1 2 3 4 House, F.; Kilkenny, D. (July 1978). "On the origin of intermediate-latitude OB stars". Astronomy and Astrophysics. 67: 421–429. Bibcode:1978A&A....67..421H. ISSN   0004-6361.
  8. 1 2 3 4 Hohle, M.M.; Neuhäuser, R.; Schutz, B.F. (April 2010). "Masses and luminosities of O- and B-type stars and red supergiants". Astronomische Nachrichten. 331 (4): 349–360. arXiv: 1003.2335 . Bibcode:2010AN....331..349H. doi:10.1002/asna.200911355. eISSN   1521-3994. ISSN   0004-6337. S2CID   111387483.
  9. 1 2 Kervella, P.; Thévenin, F.; Di Folco, E.; Ségransan, D. (October 2004). "The angular sizes of dwarf stars and subgiants". Astronomy & Astrophysics. 426 (1): 297–307. arXiv: astro-ph/0404180 . Bibcode:2004A&A...426..297K. doi: 10.1051/0004-6361:20035930 . eISSN   1432-0746. ISSN   0004-6361.
  10. 1 2 3 Holgado, G.; Simón-Díaz, S.; Haemmerlé, L.; Lennon, D. J.; Barbá, R. H.; Cerviño, M.; Castro, N.; Herrero, A.; Meynet, G.; Arias, J. I. (June 2020). "The IACOB project. VI. On the elusive detection of massive O-type stars close to the ZAMS". Astronomy & Astrophysics. 638: A157. arXiv: 2005.05446 . Bibcode:2020A&A...638A.157H. doi: 10.1051/0004-6361/202037699 . eISSN   1432-0746. ISSN   0004-6361.
  11. 1 2 Anders, F.; et al. (February 2022). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia EDR3 stars brighter than G = 18.5". Astronomy & Astrophysics. 658: A91. arXiv: 2111.01860 . Bibcode:2022A&A...658A..91A. doi: 10.1051/0004-6361/202142369 . eISSN   1432-0746. ISSN   0004-6361.
  12. 1 2 Howarth, Ian D.; Siebert, Kaj W.; Hussain, Gaitee A. J.; Prinja, Raman K. (January 1997). "Cross-correlation characteristics of OB stars from IUE spectroscopy". Monthly Notices of the Royal Astronomical Society. 284 (2): 265–285. Bibcode:1997MNRAS.284..265H. doi: 10.1093/mnras/284.2.265 . eISSN   1365-2966. ISSN   0035-8711.
  13. ↑ "HD 116852". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved January 28, 2023.
  14. ↑ Mason, Brian D.; Hartkopf, William I.; Gies, Douglas R.; Henry, Todd J.; Helsel, John W. (29 January 2009). "The High Angular Resolution Multiplicity of Massive Stars". The Astronomical Journal. 137 (2): 3358–3377. arXiv: 0811.0492 . Bibcode:2009AJ....137.3358M. doi: 10.1088/0004-6256/137/2/3358 . eISSN   1538-3881. ISSN   0004-6256.
  15. 1 2 Sembach, Kenneth R.; Savage, Blair D. (August 1994). "Gas kinematics and ionization along the extended sight line to HD 116852". The Astrophysical Journal. 431: 201. Bibcode:1994ApJ...431..201S. doi: 10.1086/174478 . eISSN   1538-4357. ISSN   0004-637X.
  16. ↑ Fox, Andrew J.; Savage, Blair D.; Sembach, Kenneth R.; Fabian, Dirk; Richter, Philipp; Meyer, David M.; Lauroesch, James; Howk, J. Christopher (10 January 2003). "Origins of the Highly Ionized Gas along the Line of Sight toward HD 116852". The Astrophysical Journal. 582 (2): 793–809. arXiv: astro-ph/0209566 . Bibcode:2003ApJ...582..793F. doi: 10.1086/344692 . eISSN   1538-4357. ISSN   0004-637X.
  17. ↑ Moffat, A. F. J.; Marchenko, S. V.; Seggewiss, W.; van der Hucht, K. A.; Schrijver, H.; Stenholm, B.; Lundstrom, I.; Setia Gunawan, D. Y. A.; Sutantyo, W.; van den Heuvel, E. P. J.; de Cuyper, J. -P.; Gomez, A. E. (March 1998). "Wolf-Rayet stars and O-star runaways with HIPPARCOS. I. Kinematics". Astronomy and Astrophysics. 331: 949–958. Bibcode:1998A&A...331..949M. ISSN   0004-6361.
  18. ↑ Mdzinarishvili, T. G.; Chargeishvili, K. B. (February 2005). "New runaway OB stars with HIPPARCOS". Astronomy & Astrophysics. 431 (2): L1 –L4. Bibcode:2005A&A...431L...1M. doi: 10.1051/0004-6361:200400134 . eISSN   1432-0746. ISSN   0004-6361.
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