Astronomy:HD 116852

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Short description: Runaway star with ionizing gas
HD 116852
Observation data
Epoch J2000.0   Equinox (celestial coordinates)
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[1] mas/yr
Dec.: −7.736[1] mas/yr
Parallax (π)0.2823 ± 0.0293[1] mas
Distance6,309[6] pc
Absolute bolometric
magnitude (Mbol)		−9.0[7]
Details
Mass15±0.7[8] M☉
Radius18.9±1.0[9] R☉
Luminosity (bolometric)16,187[8] L☉
Surface gravity (log g)3.52±0.04[10] cgs
Temperature34,000±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
SIMBADdata

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]

References

  1. ↑ 1.0 1.1 1.2 1.3 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  2. ↑ 2.0 2.1 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system.". VizieR Online Data Catalog. Bibcode: 2002yCat.2237....0D. 
  3. ↑ 3.0 3.1 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. doi:10.1088/0067-0049/211/1/10. ISSN 0067-0049. Bibcode: 2014ApJS..211...10S. 
  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. doi:10.1093/mnras/168.3.451. ISSN 0035-8711. Bibcode: 1974MNRAS.168..451H. 
  5. ↑ 5.0 5.1 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. doi:10.1002/asna.200710776. ISSN 0004-6337. Bibcode: 2007AN....328..889K. 
  6. ↑ 6.0 6.1 6.2 Maíz Apellániz, J.; Barbá, R. H. (May 2018). "Optical-NIR dust extinction towards Galactic O stars". Astronomy & Astrophysics 613: A9. doi:10.1051/0004-6361/201732050. ISSN 0004-6361. Bibcode: 2018A&A...613A...9M. 
  7. ↑ 7.0 7.1 7.2 7.3 House, F.; Kilkenny, D. (July 1978). "On the origin of intermediate-latitude OB stars.". Astronomy and Astrophysics 67: 421–429. ISSN 0004-6361. Bibcode: 1978A&A....67..421H. 
  8. ↑ 8.0 8.1 8.2 8.3 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. doi:10.1002/asna.200911355. ISSN 0004-6337. Bibcode: 2010AN....331..349H. 
  9. ↑ 9.0 9.1 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. doi:10.1051/0004-6361:20035930. ISSN 0004-6361. Bibcode: 2004A&A...426..297K. 
  10. ↑ 10.0 10.1 10.2 Holgado, G.; Simón-Díaz, S.; Haemmerlé, L.; Lennon, D. J.; Barbá, R. H.; Cerviño, M.; Castro, N.; Herrero, A. et al. (June 2020). "The IACOB project. VI. On the elusive detection of massive O-type stars close to the ZAMS". Astronomy & Astrophysics 638: A157. doi:10.1051/0004-6361/202037699. ISSN 0004-6361. Bibcode: 2020A&A...638A.157H. 
  11. ↑ 11.0 11.1 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. doi:10.1051/0004-6361/202142369. ISSN 0004-6361. Bibcode: 2022A&A...658A..91A. 
  12. ↑ 12.0 12.1 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. doi:10.1093/mnras/284.2.265. ISSN 0035-8711. Bibcode: 1997MNRAS.284..265H. 
  13. ↑ "HD 116852". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+116852. 
  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. doi:10.1088/0004-6256/137/2/3358. ISSN 0004-6256. Bibcode: 2009AJ....137.3358M. 
  15. ↑ 15.0 15.1 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. doi:10.1086/174478. ISSN 0004-637X. Bibcode: 1994ApJ...431..201S. 
  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. doi:10.1086/344692. ISSN 0004-637X. Bibcode: 2003ApJ...582..793F. 
  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. et al. (March 1998). "Wolf-Rayet stars and O-star runaways with HIPPARCOS. I. Kinematics". Astronomy and Astrophysics 331: 949–958. ISSN 0004-6361. Bibcode: 1998A&A...331..949M. 
  18. ↑ Mdzinarishvili, T. G.; Chargeishvili, K. B. (February 2005). "New runaway OB stars with HIPPARCOS". Astronomy & Astrophysics 431 (2): L1–L4. doi:10.1051/0004-6361:200400134. ISSN 0004-6361. Bibcode: 2005A&A...431L...1M. 



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