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WR 31a

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WR 31a

WR 31a is surrounded by a blue bubble nebula created by a powerful stellar wind impacting material expelled during earlier stages of the star's life.
Credit: ESA/Hubble & NASA; Acknowledgement: Judy Schmidt
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Carina
Right ascension 10h 53m 59.586s[1]
Declination −60° 26′ 44.31″[1]
Apparent magnitude (V) 10.85[1]
Characteristics
Spectral type WN11h[2]
B−V color index 0.79
J−H color index 0.60
J−K color index 1.23
Variable type cLBV[3][4][dubious – discuss]
Astrometry
Proper motion (μ) RA: −3.6[1] mas/yr
Dec.: 4.0[1] mas/yr
Parallax (π)0.80 ± 0.88 mas[5][6]
Distance8,000[2] pc
Absolute magnitude (MV)−6.71[7]
Details[3][8]
Luminosity1,820,000 [dubious – discuss] L☉
Temperature30,200 [dubious – discuss] K
Other designations
WR 31a, Hen 3-519, TYC 8928-1166-1, IRAS 10520-6010, GSC2 S1113013697, 2MASS J10535958-6026444, AAVSO 1050-59
Database references
SIMBADdata

WR 31a is a Wolf–Rayet (WR) star in the southern constellation of Carina that is surrounded by an expanding Wolf–Rayet nebula. It is commonly referred to as Hen 3-519. It is not a classical old stripped-envelope WR star, but a young massive star which still has some hydrogen left in its atmosphere.

History of observations

WR 31a was first published in 1952 as one of six peculiar emission line stars, but not given a designation at that time. It was described as having numerous P Cygni type lines with unusually broad emission components.[9] A year later it was listed as being associated with nebulosity, at the time thought to be a planetary nebula.[10]

In 1976 it was included in a catalogue of southern emission-line stars, the third catalogue of emission objects compiled by Karl Gordon Henize. The designation Hen 3-519, sometimes He 3-519, was adopted as the most common identifier for this star.[11] In 2001, it was listed in The Seventh Catalogue of Galactic Wolf-Rayet stars as entry 31a,[7] but it is still frequently called Hen 3-519.[4][3]

In 1994 WR 31a was first described as a candidate luminous blue variable (cLBV) after a detailed spectrographic study with the Anglo-Australian Telescope.[12]

Blue bubble

WR 31a is surrounded by a shell of ionised gas nearly eight light-years (2.5 pc) wide. The Hubble Space Telescope (HST) has captured a striking image of the nebula, rendering it as a thin blue bubble. In this false colour image, the blue colours represents red visible light (605 nm), while orange-red colours represent near infrared radiation at 814 nm.[13] Some media sources have wrongly claimed this deep-sky object was recently discovered by the HST,[14] but this nebula was originally found by Ellen Dorrit Hoffleit in 1953 and designated as the planetary nebula Hf 39.[10] Other planetary nebula catalogue names include ESO 128-18 and Wray 15-682.[10]

Since 2013, the nebula has been considered not as a planetary nebula, but rather as a much larger expanding gas shell, formally classified as a Wolf–Rayet nebula or WR nebula.[15] Its observed expansion velocity is 365 km/s (227 mi/s), and is estimated to be some 2.4 parsecs (7.8 ly) across.[16] The dynamical age of the nebula is estimated at 18,000 years and the total mass of ionised gas at 2-3 M☉.[12]

Properties

WR 31a itself, the highly luminous central star of the nebula, is invisible to the naked-eye at magnitude 10.85V. It has a spectral classification of WN11h, indicating a WR star with strong Nii emission but no Niii emission, and with hydrogen features visible in the spectrum.[16] The spectral classification WN11 was created for this star and AG Carinae since they did not fit into any existing spectral type and appeared to constitute an extension of the WR nitrogen sequence to cooler temperatures.[12] The progenitor's mass of the central star is estimated to have been about 45 times that of the Sun,[4] and this massive star will likely explode as a supernova, possibly of type Ib or type Ic in the future.[17][18] Its distance is estimated to be 8,000 to 9,200 parsecs (26,000 to 30,000 ly).[17][2]

The spectrum of WR 31a shows P Cygni profiles, most strongly on the dominant Hi, Hei, and Nii lines. These profiles may show dramatic changes on a timescale of weeks, with the absorption components of the lines sometimes disappearing completely.[12]

Variability

No significant brightness changes have been detected in WR 31a, but it has been listed as a candidate luminous blue variable because of its luminosity, temperature, and mass loss properties.[12] Van Genderen catalogued it as a dormant or ex-LBV because of the lack of characteristic LBV variations.[8] Possible small brightness changes have been seen in All Sky Automated Survey (ASAS) data,[19] WR 31a is included as a variable star in the International Variable Star Index,[20] although not in the General Catalogue of Variable Stars.[21]

References

  1. ^ a b c d e Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27. Bibcode:2000A&A...355L..27H.
  2. ^ a b c Toalá, J. A.; Guerrero, M. A.; Ramos-Larios, G.; Guzmán, V. (2015). "WISE morphological study of Wolf-Rayet nebulae". Astronomy & Astrophysics. 578: A66. arXiv:1503.06878. Bibcode:2015A&A...578A..66T. doi:10.1051/0004-6361/201525706.
  3. ^ a b c Nazé, Y.; Rauw, G.; Hutsemékers, D. (2012). "The first X-ray survey of Galactic luminous blue variables". Astronomy & Astrophysics. 538: A47. arXiv:1111.6375. Bibcode:2012A&A...538A..47N. doi:10.1051/0004-6361/201118040.
  4. ^ a b c Smith, Nathan; Tombleson, Ryan (2015). "Luminous blue variables are antisocial: Their isolation implies that they are kicked mass gainers in binary evolution". Monthly Notices of the Royal Astronomical Society. 447: 598. arXiv:1406.7431. Bibcode:2015MNRAS.447..598S. doi:10.1093/mnras/stu2430.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  5. ^ Gaia Collaboration (2016). "VizieR Online Data Catalog: Gaia DR1". Astronomy and Astrophysics. Bibcode:2016yCat.1337....0G.
  6. ^ Brown, A. G. A.; Vallenari, A.; Prusti, T.; de Bruijne, J.; Mignard, F.; et al. (2016). "Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties". Astronomy and Astrophysics. arXiv:1609.04172. Bibcode:2016arXiv160904172G. doi:10.1051/0004-6361/201629512.
  7. ^ a b Van Der Hucht, Karel A. (2001). "The VIIth catalogue of galactic Wolf-Rayet stars". New Astronomy Reviews. 45 (3): 135. Bibcode:2001NewAR..45..135V. doi:10.1016/S1387-6473(00)00112-3.
  8. ^ a b Van Genderen, A. M. (2001). "S Doradus variables in the Galaxy and the Magellanic Clouds". Astronomy and Astrophysics. 366 (2): 508. Bibcode:2001A&A...366..508V. doi:10.1051/0004-6361:20000022.Vizie database entry
  9. ^ Henize, Karl G. (1952). "Six Peculiar Hα-Emission Stars". Astrophysical Journal. 115: 133. Bibcode:1952ApJ...115..133H. doi:10.1086/145522.
  10. ^ a b c Hoffleit, Dorrit (1953). "A preliminary survey of nebulosities and associated B-stars in Carina". Annals of Harvard College Observatory. 119: 37. Bibcode:1953AnHar.119...37H.
  11. ^ Henize, K. G. (1976). "Observations of southern emission-line stars". Astrophysical Journal Supplement Series. 30: 491. Bibcode:1976ApJS...30..491H. doi:10.1086/190369.
  12. ^ a b c d e Smith, L. J.; Crowther, P. A.; Prinja, R. K. (1994). "A study of the luminous blue variable candidate He 3-519 and its surrounding nebula". Astronomy and Astrophysics. 281: 833. Bibcode:1994A&A...281..833S.
  13. ^ "Hubble's Blue Bubble". NASA. Retrieved 1 March 2016.
  14. ^ "Hubble Captures "Blue Bubble' Star - 20 Times Bigger, a Million Times Brighter than the Sun's". Inquisitr. Retrieved 2 March 2016.
  15. ^ Frew, D. J.; Bojicic, I. S.; Parker, Q. A. (2013). "A catalogue of integrated Hα fluxes for 1258 Galactic planetary nebulae". Monthly Notices of the Royal Astronomical Society. 431: 2. Bibcode:2013MNRAS.431....2F. doi:10.1093/mnras/sts393.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  16. ^ a b Toalá, J. A.; Guerrero, M. A.; Ramos-Larios, G.; Guzmán, V. (2015). "WISE morphological study of Wolf-Rayet nebulae". Astronomy & Astrophysics. 578: A66. arXiv:1503.06878v1. doi:10.1051/0004-6361/201525706.
  17. ^ a b "Blue bubble in Carina". NASA. Retrieved 2 March 2016.
  18. ^ Groh, Jose H.; Meynet, Georges; Georgy, Cyril; Ekström, Sylvia (2013). "Fundamental properties of core-collapse supernova and GRB progenitors: Predicting the look of massive stars before death". Astronomy & Astrophysics. 558: A131. arXiv:1308.4681. Bibcode:2013A&A...558A.131G. doi:10.1051/0004-6361/201321906.
  19. ^ Pojmanski, G. (2002). "The All Sky Automated Survey. Catalog of Variable Stars. I. 0 h - 6 h Quarter of the Southern Hemisphere". Acta Astronomica. 52: 397. arXiv:astro-ph/0210283. Bibcode:2002AcA....52..397P.
  20. ^ "Hen 3-519". International Variable Star Index. American Association of Variable Star Observers. 4 January 2010. Retrieved 30 September 2016.
  21. ^ 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.
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