Astronomy:V1936 Aquilae
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Aquila |
| Right ascension | 19h 23m 47.64119s[2] |
| Declination | 14° 36′ 39.0612″[2] |
| Apparent magnitude (V) | 15.1 |
| Characteristics | |
| Evolutionary stage | Blue supergiant |
| Spectral type | O4I[3] |
| Variable type | cLBV[4] |
| Astrometry | |
| Proper motion (μ) | RA: +6.500[2] mas/yr Dec.: −55.796[2] mas/yr |
| Parallax (π) | 0.1462 ± 0.0.598[2] mas |
| Distance | 6,000[5] pc |
| Details | |
| Mass | 25[5] M☉ |
| Radius | 48 - 145[6] R☉ |
| Luminosity | 562,000[5] L☉ |
| Temperature | 13,213[5] K |
| Age | 2.3 (3-6)[7] Myr |
| Other designations | |
LS1, 2MASS J19234764+1436391 | |
| Database references | |
| SIMBAD | data |
V1936 Aquilae is a blue supergiant and candidate Luminous blue variable located in the nebula Westerhout 51, in the constellation Aquila, about 20,000 light years away. The star was originally identified as a massive star in 2000,[3] and was thought to be an O-type supergiant. However, subsequent analyses have shown it to be not O but B-type,[5] as well as being possibly an LBV.[4]
Properties
V1936 Aquilae is a very luminous star. Recent measurements hint at a bolometric luminosity of around 560,000 L☉, assuming a distance of 6 kiloparsecs, consistent with the distance of Westerhout 51, the very large H II region (nebula) it is located in. The star likely has a temperature of around 13,200 K.[5] The Stefan-Boltzmann Law suggests a radius of around 143 times that of the Sun.
References
- ↑ "ASAS-SN Variable Stars Database". ASAS-SN. https://asas-sn.osu.edu/variables/lookup.
- ↑ 2.0 2.1 2.2 2.3 2.4 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.
- ↑ 3.0 3.1 Okumura, Shin-ichiro; Mori, Atsushi; Nishihara, Eiji; Watanabe, Etsuji; Yamashita, Takuya (2000-11-01). "The Initial Mass Function of a Massive Star-forming Region W51". The Astrophysical Journal 543 (2): 799–821. doi:10.1086/317116. ISSN 0004-637X. Bibcode: 2000ApJ...543..799O.
- ↑ 4.0 4.1 Smith, Nathan; Aghakhanloo, Mojgan; Murphy, Jeremiah W.; Drout, Maria R.; Stassun, Keivan G.; Groh, Jose H. (2019-09-01). "On the Gaia DR2 distances for Galactic luminous blue variables". Monthly Notices of the Royal Astronomical Society 488 (2): 1760–1778. doi:10.1093/mnras/stz1712. ISSN 0035-8711. Bibcode: 2019MNRAS.488.1760S.
- ↑ 5.0 5.1 5.2 5.3 5.4 5.5 Bik, A.; Henning, Th.; Wu, S. -W.; Zhang, M.; Brandner, W.; Pasquali, A.; Stolte, A. (2019-04-01). "Near-infrared spectroscopy of the massive stellar population of W51: evidence for multi-seeded star formation". Astronomy and Astrophysics 624: A63. doi:10.1051/0004-6361/201935061. ISSN 0004-6361. Bibcode: 2019A&A...624A..63B.
- ↑ Clark, J. S.; Davies, B.; Najarro, F.; MacKenty, J.; Crowther, P. A.; Messineo, M.; Thompson, M. A. (2009). "The P Cygni supergiant [OMN2000] LS1 - implications for the star formation history of W51". Astronomy and Astrophysics 504 (2): 429. doi:10.1051/0004-6361/200911980. Bibcode: 2009A&A...504..429C.
- ↑ Lim, Wanggi; De Buizer, James M. (2019). "Surveying the Giant H II Regions of the Milky Way with SOFIA. I. W51A". The Astrophysical Journal 873 (1): 51. doi:10.3847/1538-4357/ab0288. Bibcode: 2019ApJ...873...51L.
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