V1429 Aquilae

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V1429 Aql
V1429AqlLightCurve.png
A visual band light curve for V1429 Aquilae adapted from Richardson et al. (2016) [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Aquila
Right ascension 19h 21m 33.977s [2]
Declination +14° 52′ 56.91″ [2]
Apparent magnitude  (V)9.79 - 10.1 [3]
Characteristics
Spectral type B3Ibe [4]
U−B color index 0.25 [5]
B−V color index 1.48 [5]
Variable type Eclipsing + cLBV [3]
Astrometry
Radial velocity (Rv)+30.7 [6]  km/s
Proper motion (μ)RA: −2.144 [2]   mas/yr
Dec.: −4.968 [2]   mas/yr
Parallax (π)0.2224 ± 0.0203  mas [2]
Distance 15,000 ± 1,000  ly
(4,500 ± 400  pc)
Absolute magnitude  (MV)−8.2 [7]
Orbit [6]
Period (P)60.737 ± 0.008 days
Eccentricity (e)0.244 ± 0.020
Periastron epoch (T)2449546.01 ± 1.10
Argument of periastron (ω)
(secondary)		218.7 ± 5.7°
Semi-amplitude (K1)
(primary)		89.7 ± 2.0 km/s
Details [8]
Mass 39.66  M☉
Radius 86.80  R☉
Luminosity 710,000  L☉
Surface gravity (log g)2.26  cgs
Temperature 18,000  K
Rotational velocity (v sin i)50 [4]  km/s
secondary
Mass 26.26  M☉
Radius 20.41  R☉
Surface gravity (log g)3.55  cgs
Temperature 6,227  K
Age 6 [9]   Myr
Other designations
V1429  Aql, BD+14°3887, MWC  314, 2MASS  J19213397+1452570, WISE  J192133.96+145257.0
Database references
SIMBAD data

V1429 Aquilae is a candidate luminous blue variable multiple star system located in the constellation of Aquila. It is often referred to by its Mount Wilson Observatory catalog number as MWC 314. It is a hot luminous star with strong emission lines in its spectrum.

Contents

Spectrum

V1429 Aql has a peculiar spectrum dominated by emission lines of hydrogen and many ionised metals, with Feii being particularly strong and numerous. There are also comparatively weak forbidden lines, primarily [Feii], but also [Nii]. Some absorption lines are present, but are either very weak or hidden by the emission. Many lines have variable profiles, particularly the hydrogen and helium series which vary during the orbit from emission to P Cygni profiles. The absorption lines are considered to be formed in the photosphere of the primary star, although some Feii absorption appears to be from gas between the stars. No lines of the secondary can be detected. The emission lines are formed in circumstellar material between and around the two stars [6] Overall, the spectral type is given as B3 Ibe. [4] [10]

In infrared spectra, the Pfund series of lines are strongly in emission, a very unusual feature characteristic of supergiant Be stars and LBVs. V1429 Aql is given a B2:e spectral type from analysis in the infrared. [9]

System

V1429 Aquilae is a single-lined spectroscopic binary. The existence of a companion is inferred from the highly periodic variations in the radial velocity of its spectral lines and by equally periodic variations in brightness and spectral line profiles. It is unclear whether there are partial eclipses of the larger star or just of gas surrounding the stars. [6]

The orbital period is well-defined at 60.7 days and it is moderately eccentric (0.244). The primary star fills its roche lobe for at least part of the orbit. The other characteristics of the orbit are disputed. The orbital velocity of the secondary is unknown, and the possible inclinations do not sufficiently restrict the possible models of the system. Assumptions based on broadly similar data produce wildly different results for the masses of the stars, from 5 M☉ to 40 M☉ for the primary. [6]

A third star is visible in infrared images just over one arc second away. It is statistically likely to be in a wide orbit around the spectroscopic pair, about 5,700 AU away. [11]

The system contains material being transferred from the primary to the secondary star as well as material surrounding both stars. A dense clump of gas near the centre of mass of the system, and co-rotating with the stars, produces the bulk of the emission lines. A more diffuse region of gas surrounds both stars and produces some absorption components in the spectrum. [6]

The entire system is surrounded by a shell of material about 0.8 parsecs across, assuming that MWC 314 is 3,000 parsecs away. This appears in infrared images as a circular ring 25 arc-seconds from the central star. [11] There is a much larger bipolar nebula detected by its Hα radiation. It is 13 parsecs from end to end. [12]

Variability

V1429 Aquilae shows brightness variations of about 0.3 magnitudes and a detectable period of 4.16 days. No longterm variations in brightness have been detected over several decades of observations. [13] The profiles of many spectral lines also vary with the same period, produced partly by radial velocity variations. [14] The absorption and emission lines show different radial velocity amplitudes, but with the same period. Most of these variations can be accounted for by the orbit of the two stars and material being transferred from the primary to the secondary, with the gas being involved in partial eclipses, [6] and possibly also partial eclipses of the stars themselves. [8] The two stars are also distorted into ellipsoidal shapes by their gravity and vary in brightness as they rotate. [6]

In addition to the orbital variations, two pulsation modes have been observed with amplitudes of a few thousandths of a magnitude and periods of 0.77 and 1.42 days. [1]

Physical properties

Estimates of the distance of V1429 Aquilae made by indirect methods range between 2.4 [1] and 4.3 kiloparsecs (9,800-14,000 light years), with 3 kpc usually being adopted. [14] The Gaia EDR3 parallax is 0.2224±0.0203  mas , suggesting a somewhat larger distance. [2]

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 the Sun (R☉), and 80 times more massive than the Sun (M☉). [15] More recent calculations give a luminosity of 710,000 L☉, radius of 87 R☉, and mass of 40 M☉. [8] Alternative assumptions about the orbit lead to lower values of 500,000 L☉, 73 R☉, and 5 M☉. [1]

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. [8] Alternatively, it may be a supergiant Be star. [14]

The secondary cannot be observed. Making some assumptions, primarily the existence of a partial eclipse of the primary star, allows its mass and some physical properties to be estimated, giving a mass of 26 M☉ and temperature of 6,227 K, [8] but these are speculative. [6]

A more recent survey of LBVs put V1429 Aquilae's luminosity at a much higher 3,800,000 L☉. [16]

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References

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  2. 1 2 3 4 5 6 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  3. 1 2 "V1429 Aql". International Variable Star Index. Retrieved 2021-03-02.
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  7. ↑ 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 .
  8. 1 2 3 4 5 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. arXiv: 1308.4638 . Bibcode:2013A&A...559A..16L. doi:10.1051/0004-6361/201220421. ISSN   0004-6361. S2CID   53372304.
  9. 1 2 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. arXiv: 1407.3900 . Bibcode:2014MNRAS.443..947L. doi: 10.1093/mnras/stu1174 . ISSN   0035-8711. S2CID   118446731.
  10. ↑ Chentsov, E. L.; Klochkova, V. G.; Tavolganskaya, N. S. (1999). "Spectral atlas of two peculiar supergiants: MWC 314 and IRC +10420". Bulletin of the Special Astrophysical Observatory. 48: 25. arXiv: 1602.04582 . Bibcode:1999BSAO...48...25C.
  11. 1 2 Martayan, Christophe; Lobel, Alex; Baade, Dietrich; Mehner, Andrea; Rivinius, Thomas; Boffin, Henri M. J.; Girard, Julien; Mawet, Dimitri; Montagnier, Guillaume; Blomme, Ronny; Kervella, Pierre; Sana, Hugues; Štefl, Stanislav; Zorec, Juan; Lacour, Sylvestre; Le Bouquin, Jean-Baptiste; Martins, Fabrice; Mérand, Antoine; Patru, Fabien; Selman, Fernando; Frémat, Yves (2016). "Luminous blue variables: An imaging perspective on their binarity and near environment⋆". Astronomy & Astrophysics. 587: A115. arXiv: 1601.03542 . Bibcode:2016A&A...587A.115M. doi:10.1051/0004-6361/201526578. S2CID   1755296.
  12. ↑ 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 .
  13. ↑ 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 .
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  15. ↑ 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" (PDF). Astronomy and Astrophysics Supplement. 312 (3): 469–478. Bibcode:1998A&AS..131..469M. doi: 10.1051/aas:1998283 .
  16. ↑ 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. arXiv: 1805.03298 . Bibcode:2019MNRAS.488.1760S. doi: 10.1093/mnras/stz1712 . ISSN   0035-8711.
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