HDE 316285

HDE 316285
Observation data
Epoch J2000      Equinox J2000
Constellation Sagittarius
Right ascension 17h 48m 14.03884s[1]
Declination −28° 00′ 53.1283″[1]
Apparent magnitude (V) 9.60[2]
Characteristics
Spectral type B0Ieq[3]
U−B color index +0.61[2]
B−V color index +1.67[2]
Variable type cLBV[4]
Astrometry
Proper motion (μ) RA: −0.09±1.64[1] mas/yr
Dec.: −5.18±1.12[1] mas/yr
Parallax (π)0.79 ± 1.29[1] mas
Distance1,900[4] pc
Absolute magnitude (MV)−8.4[5]
Details
Radius75[5] R☉
Luminosity275,000[6] L☉
Temperature15,000[6] K
Other designations
V4375 Sagittarii, HD 316285, HIP 87136, CD −27°11944, SAO 185776, GCRV 67373, MWC 272, AAVSO 1741-27B
Database references
SIMBADdata

HDE 316285 is a blue supergiant star in the constellation Sagittarius. It is a candidate Luminous Blue Variable and lies about 6,000 light years away in the direction of the galactic centre.

Discovery

HD 316285 was identified in 1925 as an unusual star having P Cygni lines in its spectrum, lines with both emission and absorption components offset by a doppler shift.[7] It was classified as a Be star although it is now known to be a supergiant and the class of Be stars excludes supergiants,[8] and was included in the Mount Wilson Observatory catalogue of B and A stars with bright lines of hydrogen (MWC) as entry 272.[9] In 1956, it was reported that the mission was due to an expanding atmosphere rather than the circumstellar discs of less evolved Be stars.[10] In 1972 it was discovered to have an infrared excess, an unusually high emission at infrared wavelengths due to surrounding warm dust.[11]

In 1961, HD 316285 was catalogued as planetary nebula Bl3-11,[12] although that classification was quickly cast into doubt.[13][14]

Variability

HD 316285 is listed in the General Catalogue of Variable Stars as a variable Be star with a range of about one tenth of a magnitude.[15] The International Variable Star Index classifies it as an S Doradus variable[16] and it is considered to be a candidate Luminous Blue Variable.[4]

Properties

The spectrum shows that HD 316285 has only 1.5 times as much hydrogen as helium and elevated levels of carbon, nitrogen, and oxygen, so it can be identified as a highly evolved star. It has been calculated to be losing mass at the rate of M☉ every four thousand years via its stellar wind.[5]

HD 316285 has been identified as a possible type II-b or type IIn supernova candidate in modelling of the fate of stars 20 to 25 times the mass of the Sun. It has been shown that these supernovae may explode directly from stars in an LBV phase after spending time as a red supergiant.[17]

A possible companion has been reported on the basis of a helical outflow of material apparently originating from HD 316285. This would be caused by a jet being twisted into a spiral shape by orbital motion.[18]

References

  1. 1 2 3 4 5 Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653. arXiv:0708.1752Freely accessible. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.
  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: 0. Bibcode:2002yCat.2237....0D.
  3. ↑ Lopes, D. F.; Damineli Neto, A.; De Freitas Pacheco, J. A. (1992). "A spectroscopic study of luminous peculiar B-type stars". Astronomy and Astrophysics. 261: 482. Bibcode:1992A&A...261..482L.
  4. 1 2 3 Nazé, Y.; Rauw, G.; Hutsemékers, D. (2012). "The first X-ray survey of Galactic luminous blue variables". Astronomy & Astrophysics. 538: A47. arXiv:1111.6375Freely accessible. Bibcode:2012A&A...538A..47N. doi:10.1051/0004-6361/201118040.
  5. 1 2 3 Hillier, D. J.; Crowther, P. A.; Najarro, F.; Fullerton, A. W. (1998). "An optical and near-IR spectroscopic study of the extreme P Cygni-type supergiant HDE 316285". Astronomy & Astrophysics. 340: 483–96. Bibcode:1998A&A...340..483H.
  6. 1 2 van Genderen, A. M. (2001). "S Doradus variables in the Galaxy and the Magellanic Clouds". Astronomy & Astrophysics. 366 (2): 508–31. Bibcode:2001A&A...366..508V. doi:10.1051/0004-6361:20000022.
  7. ↑ Merrill, P. W. (1925). "Two stellar spectra of the P Cygni type". Astrophysical Journal. 61: 418. Bibcode:1925ApJ....61..418M. doi:10.1086/142900.
  8. ↑ Merrill, P. W.; Humason, M. L.; Burwell, C. G. (1925). "Discovery and Observations of Stars of Class Be". Astrophysical Journal. 61: 389. Bibcode:1925ApJ....61..389M. doi:10.1086/142899.
  9. ↑ Merrill, Paul W.; Burwell, Cora G. (1933). "Catalogue and Bibliography of Stars of Classes B and a whose Spectra have Bright Hydrogen Lines". Astrophysical Journal. 78: 87. Bibcode:1933ApJ....78...87M. doi:10.1086/143490.
  10. ↑ Merrill, Paul W. (1956). "Stars with expanding atmospheres". Vistas in Astronomy. 2: 1375. Bibcode:1956VA......2.1375M. doi:10.1016/0083-6656(56)90065-4.
  11. ↑ Kleinmann, S.; Kuhi, L. V. (1972). "Mass Loss and Infrared Excesses in Hot Stars". Publications of the Astronomical Society of the Pacific. 84: 766. Bibcode:1972PASP...84..766K. doi:10.1086/129377.
  12. ↑ Blanco, V. M. (1961). "A catalogue of Half emission objects in the galactic center region". Contr. from the Bosscha Observ. Lembang. 13: 1. Bibcode:1961CoBos..13....1B.
  13. ↑ Vorontsov-Veliaminov, B. A.; Kostiakova, E. B.; Dokuchaeva, O. D.; Arkhipova, V. P. (1975). "Planetary nebulae near the galactic center". Soviet Astronomy. 19: 163. Bibcode:1975SvA....19..163V.
  14. ↑ Frew, D. J.; Bojicic, I. S.; Parker, Q. A. (2013). "A catalogue of integrated Halpha fluxes for 1258 Galactic planetary nebulae". Monthly Notices of the Royal Astronomical Society. 431 (1): 2–26. arXiv:1211.2505Freely accessible. Bibcode:2013MNRAS.431....2F. doi:10.1093/mnras/sts393.
  15. ↑ 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.
  16. ↑ Watson, C. L. (2006). "The International Variable Star Index (VSX)". The Society for Astronomical Sciences 25th Annual Symposium on Telescope Science. Held May 23–25. 25: 47. Bibcode:2006SASS...25...47W.
  17. ↑ Groh, J. H.; Meynet, G.; Ekström, S. (2013). "Massive star evolution: luminous blue variables as unexpected supernova progenitors". Astronomy & Astrophysics. 550: 4. arXiv:1301.1519Freely accessible. Bibcode:2013A&A...550L...7G. doi:10.1051/0004-6361/201220741. L7.
  18. ↑ Lau, R. M.; Hankins, M. J.; Herter, T. L.; Morris, M. R.; Mills, E. A. C.; Ressler, M. E. (2016). "An Apparent Precessing Helical Outflow from a Massive Evolved Star: Evidence for Binary Interaction". The Astrophysical Journal. 818 (2): 117. arXiv:1512.07639Freely accessible. Bibcode:2016ApJ...818..117L. doi:10.3847/0004-637X/818/2/117.
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