V1429 Aquilae
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Aquila |
| Right ascension | 19h 21m 33.975s[1] |
| Declination | +14° 52′ 56.89″[1] |
| Apparent magnitude (V) | 9.88[2] |
| Characteristics | |
| Spectral type | B3Ibe[3] |
| U−B color index | 0.25[2] |
| B−V color index | 1.48[2] |
| Variable type | cLBV[4] |
| Astrometry | |
| Radial velocity (Rv) | +24.8[5] km/s |
| Proper motion (μ) | RA: −1.7[6] mas/yr Dec.: −7.9[6] mas/yr |
| Parallax (π) | 1.5 ± 14.9[7] mas |
| Distance | 3,000[8] pc |
| Absolute magnitude (MV) | −8.2[8] |
| Details | |
| Mass | 39.66/26.26[5] M☉ |
| Radius | 86.80/20.41[5] R☉ |
| Luminosity | 710,000[5] L☉ |
| Surface gravity (log g) | 2.26/3.55[5] cgs |
| Temperature | 18,000/6,227[5] K |
| Rotational velocity (v sin i) | 50[3] km/s |
| Age | 6,000,000[9] years |
| Orbit[5] | |
| Primary | A |
| Companion | B |
| Period (P) | 60.799977 ± 0.000014 days |
| Semi-major axis (a) | 98.7 ± 6 R☉ |
| Eccentricity (e) | 0.235 ± 0.003 |
| Inclination (i) | 72.79 ± 13.05° |
| Periastron epoch (T) | 2454959.76 |
| Argument of periastron (ω) (secondary) | 289 ± 1° |
| Semi-amplitude (K1) (primary) | 84.5 km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
V1429 Aquilae is a blue hypergiant variable star located in the constellation of Aquila. It is often referred to by its Mount Wilson Observatory catalog number as MWC 314.
Physical properties
V1429 Aquilae is sufficiently remote that its distance must be determined by indirect methods: estimations range between 3 and 4.3 kiloparsecs (9,800-14,000 light years), with the most likely value nearer to the former, lower figure.[10]
V1429 Aql is a single-line spectroscopic contact binary with a period of about 2 months. The system surrounded by a disk of gas[11] as well as a very extensive bipolar nebula.[12] The system shows partial eclipses which produce very small magnitude changes because the primary is so much hotter and brighter than the secondary. The surface brightness of the primary is 15 times higher and the eclipses change the brightness by about 0.1 magnitudes.[5]
The primary is a hot B-type star. Its total luminosity has been estimated to be as much as 1,200,000 times that of the Sun (L☉), with a radius 60 times larger than that of our star (R☉), and 80 times more massive than the Sun (M☉).[13] More recent calculations give a luminosity of 710,000 L☉, radius of 87 R☉, and mass of 40 M☉.[5]
The physical parameters of the star, and its spectrum, are comparable to a luminous blue variable (LBV). Although it has not shown the defining outbursts and spectral variations, the surrounding nebulae indicate episodes of heavy mass loss in the past.[5]
References
- 1 2 Hog, E.; Kuzmin, A.; Bastian, U.; Fabricius, C.; Kuimov, K.; Lindegren, L.; Makarov, V. V.; Roeser, S. (1998). "The TYCHO Reference Catalogue". Astronomy and Astrophysics 335: L65. Bibcode:1998A&A...335L..65H.
- 1 2 3 Moffat, Anthony F. J.; Reed, B. Cameron (1999). "Photometry of Intrinsically Luminous Stars in Galactic Fields at Longitudes". Publications of the Astronomical Society of the Pacific 111 (763): 1149–1156. Bibcode:1999PASP..111.1149M. doi:10.1086/316429. ISSN 0004-6280.
- 1 2 Carmona, A.; van den Ancker, M. E.; Audard, M.; Henning, Th.; Setiawan, J.; Rodmann, J. (2010). "New Herbig Ae/Be stars confirmed via high-resolution optical spectroscopy". Astronomy and Astrophysics 517: A67. Bibcode:2010A&A...517A..67C. doi:10.1051/0004-6361/200913800. ISSN 0004-6361.
- ↑ 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.
- 1 2 3 4 5 6 7 8 9 10 Lobel, A.; Groh, J. H.; Martayan, C.; Frémat, Y.; Torres Dozinel, K.; Raskin, G.; Van Winckel, H.; Prins, S.; Pessemier, W.; Waelkens, C.; Hensberge, H.; Dumortier, L.; Jorissen, A.; Van Eck, S.; Lehmann, H. (2013). "Modelling the asymmetric wind of the luminous blue variable binary MWC 314". Astronomy & Astrophysics 559: A16. Bibcode:2013A&A...559A..16L. doi:10.1051/0004-6361/201220421. ISSN 0004-6361.
- 1 2 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.
- ↑ Van Altena, W. F.; Lee, J. T.; Hoffleit, E. D. (1995). "The general catalogue of trigonometric [stellar] parallaxes". New Haven. Bibcode:1995gcts.book.....V.
- 1 2 van Genderen, A.M. (2001). "S Doradus variables in the Galaxy and the Magellanic Clouds". Astronomy & Astrophysics 366 (2): 508–531. Bibcode:2001A&A...366..508V. doi:10.1051/0004-6361:20000022.
- ↑ Liermann, A.; Schnurr, O.; Kraus, M.; Kreplin, A.; Arias, M. L.; Cidale, L. S. (2014). "A K-band spectral mini-survey of Galactic B[e] stars". Monthly Notices of the Royal Astronomical Society 443 (2): 947–956. Bibcode:2014MNRAS.443..947L. doi:10.1093/mnras/stu1174. ISSN 0035-8711.
- ↑ Miroshnichenko, A. S. (August 1996). "MWC 314: a high-luminosity peculiar Be star.". Astronomy and Astrophysics 312: 941–949. Bibcode:1996A&A...312..941M.
- ↑ Muratorio, G.; Rossi, C.; Friedjung, M. (August 2008). "Analysis of the variability of the luminous emission line star MWC 314". Astronomy and Astrophysics 487 (2): 637–644. Bibcode:2008A&A...487..637M. doi:10.1051/0004-6361:20078940.
- ↑ Marston, A. P.; McCollum, B. (August 2008). "Extended shells around B[e] stars. Implications for B[e] star evolution". Astronomy and Astrophysics 477 (1): 193–202. Bibcode:2008A&A...477..193M. doi:10.1051/0004-6361:20066086.
- ↑ Miroshnichenko, A. S.; Fremat, Y.; Houziaux, L.; Andrillat, Y.; Chentson, E. L.; Klochkova, V. G. (September 1998). "High resolution spectroscopy of the galactic candidate LBV MWC 314". Astronomy and Astrophysics Supplement 312 (3): 469–478. Bibcode:1998A&AS..131..469M. doi:10.1051/aas:1998283.
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