V923 Aquilae

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V923 Aquilae
V923AqlLightCurve.png
A photoelectric (yellow) light curve for V923 Aquilae, plotted from data presented by Lynds (1960). [1] The length of a full phase cycle is 0.8518 days.
Observation data
Epoch J2000       Equinox J2000
Constellation Aquila
Right ascension 19h 30m 33.12199s [2]
Declination +03° 26′ 39.8583″ [2]
Apparent magnitude  (V)6.06 [3]
5.98 to 6.18 [4]
Characteristics
Evolutionary stage Main sequence [5]
Spectral type B7III [6]
U−B color index −0.31 [3]
B−V color index −0.019±0.008 [7]
Variable type Be star [4]
Astrometry
Radial velocity (Rv)−26.0±7.4 [7]  km/s
Proper motion (μ)RA: 11.717 [2]   mas/yr
Dec.: 3.089 [2]   mas/yr
Parallax (π)3.6705 ± 0.0607  mas [2]
Distance 890 ± 10  ly
(272 ± 5  pc)
Absolute magnitude  (MV)−0.87 [7]
Details [5]
Primary
Mass 6.2±0.3  M☉
Luminosity 1517+158
−143  L☉
Surface gravity (log g)3.64±0.21  cgs
Temperature 16,580±400  K
Rotational velocity (v sin i)275±17 km/s
Secondary
Mass ~0.5  M☉
Other designations
V923 Aql, BD+03°4043, HD  183656, HIP  95929, HR  7415, SAO  0124704 [8]
Database references
SIMBAD data

V923 Aquilae is a variable binary star [9] system in the equatorial constellation of Aquila. It has the designation HD 183656 from the Henry Draper Catalogue ; V932 Aql is the variable star designation. The system is dimly visible to the naked eye with an apparent visual magnitude that fluctuates around 6.06. [3] It is located at a distance of approximately 890  light years from the Sun based on parallax, [2] but is drifting closer with a radial velocity of around −26 km/s. [7]

This system was first identified as a likely spectroscopic binary by W. E. Harper in 1937, who noted it showed "narrow intense lines of peculiar spectrum". [10] P. W. Merrill and C. G. Burwell identified it as a shell star in 1949. [11] [12] Merrill and A. L. Lowen showed in 1953 that the shell displayed large radial velocity variations. [13] A photometric study by C. R. Lynds in 1960 showed the system varied in brightness with an amplitude of more than 0.1 in magnitude and a characteristic period of 0.85 days, although it does not behave periodically over long time intervals. [1]

A more thorough investigation by P. Koubský and associates in 1989 using long-term radial velocity measurements determined this is a spectroscopic binary with an orbital period of 214.75 days. There is also an overlaying long-term cyclical variation of changing amplitude and period. The modelled binary system shows a primary with a class of around B5–7e and a low mass secondary separated by around 250 times the radius of the Sun (250  R☉ ). They hypothesized that the long-term variation was due to an envelope created by a mass transfer from the secondary component to the primary. [14] However, the mass transfer concept was later brought into question and remains unverified as of 2004. [9]

Related Research Articles

<span class="mw-page-title-main">V1494 Aquilae</span> Nova seen in 1999 in the constellation of Aquila

V1494 Aquilae or Nova Aquilae 1999 b was a nova which occurred during 1999 in the constellation Aquila and reached a brightness of magnitude 3.9 on 2 December 1999. making it easily visible to the naked eye. The nova was discovered with 14×100 binoculars by Alfredo Pereira of Cabo da Roca, Portugal at 18:50 UT on 1 December 1999, when it had a visual magnitude of 6.0.

<span class="mw-page-title-main">Delta Aquilae</span> Binary star system in the constellation Aquila

Delta Aquilae, Latinized from δ Aquilae, is a binary star system in the equatorial constellation of Aquila. It has an apparent visual magnitude of 3.4 and, based upon parallax measurements, is located at a distance of about 50.6 light-years from Earth. It is drifting closer with a radial velocity of −30 km/s. The system is predicted to come to within 25.4 ly (7.8 pc) of the Sun in around 335,000 years.

<span class="mw-page-title-main">Psi Aquilae</span> Star in the constellation Aquila

Psi Aquilae, Latinized as ψ Aquilae, is the Bayer designation for a star in the equatorial constellation of Aquila. It is a faint star with an apparent visual magnitude of 6.25, which, according to the Bortle Dark-Sky Scale, can be seen with the naked eye in dark rural skies. The orbit of the Earth causes an annual parallax shift of 2.83 mas, which indicates a distance of approximately 1,150 light-years.

70 Aquilae, abbreviated 70 Aql, is a single orange-hued star in the equatorial constellation of Aquila. 70 Aquilae is its Flamsteed designation. It is visible to the naked eye with an apparent visual magnitude of 4.90. The distance to 70 Aquilae, as determined from its annual parallax shift of 3.5 mas, is around 940 light years. The star is moving closer to the Earth with a heliocentric radial velocity of −9 km/s.

4 Aquilae, abbreviated 4 Aql, is a single, white-hued star in the equatorial constellation of Aquila. 4 Aquilae is the Flamsteed designation. It has an apparent visual magnitude of 5.02, making it a faint star visible to the naked eye. The distance to 4 Aql can be estimated from its annual parallax shift of 6.7 mas, yielding an estimated range of around 480 light years. It is moving closer to the Earth with a heliocentric radial velocity of −13 km/s.

<span class="mw-page-title-main">23 Aquilae</span> Binary star system in the constellation Aquila

23 Aquilae is a binary star system in the equatorial constellation of Aquila. 23 Aquilae is its Flamsteed designation. It is at a distance of about 400 light-years with an apparent visual magnitude of 5.10, which is bright enough to be faintly visible to the naked eye as an orange-hued star. The brightness of the star is diminished by 0.21 in magnitude because of extinction from interstellar dust and gas. The system is moving closer to the Earth with a heliocentric radial velocity of –23 km/s.

<span class="mw-page-title-main">21 Aquilae</span> Star in the constellation Aquila

21 Aquilae is a solitary variable star in the equatorial constellation of Aquila. It has the variable star designation V1288 Aql; 21 Aquilae is its Flamsteed designation. This object is visible to the naked eye as a dim, blue-white hued star with a baseline apparent visual magnitude of about 5.1. The star is located at a distance of around 680 light-years from Earth, give or take a 20 light-year margin of error. It is moving closer to the Earth with a heliocentric radial velocity of –5 km/s.

11 Aquilae is a single star in the equatorial constellation of Aquila. 11 Aquilae is the Flamsteed designation. It has an apparent visual magnitude of 5.2, which means it is faintly visible to the naked eye. Based upon an annual parallax shift of 20.9 mas, the distance to this star is approximately 156 light-years. The brightness of this star is diminished by 0.33 in magnitude because of extinction from interstellar gas and dust.

14 Aquilae is a probable spectroscopic binary star system in the equatorial constellation of Aquila. 14 Aquilae is the Flamsteed designation though it also bears the Bayer designation g Aquilae. It is visible to the naked eye as a dim, white-hued star with an apparent visual magnitude of 5.42, and it is located at a distance of approximately 500 light-years from Sun. The star is moving closer to the Earth with a heliocentric radial velocity of −39 km/s, and may come as close as 136 light-years in around 3.5 million years.

66 Aquilae, abbreviated 66 Aql, is a fifth-magnitude star in the constellation of Aquila. 66 Aquilae is its Flamsteed designation. It is visible to the naked eye, having an apparent visual magnitude of 5.44. The star shows an annual parallax shift of 4.4 mas, which provides a distance estimate of around 730 light years. It is moving closer to the Earth with a heliocentric radial velocity of −30 km/s. The motion of the star over time suggests some displacement, which may indicate it is a close binary system.

22 Aquilae, abbreviated 22 Aql, is a star in the equatorial constellation of Aquila. 22 Aquilae is its Flamsteed designation. It is a faint star but visible to the naked eye with an apparent visual magnitude of 5.59. The distance to 22 Aql can be estimated from its annual parallax shift of 4.74 mas, which yields a separation of 690 light years. It is moving closer to the Earth with a heliocentric radial velocity of −23 km/s.

HD 222582 is a multiple star system in the equatorial constellation of Aquarius. It is invisible to the naked eye with an apparent visual magnitude of 7.7, but can be viewed with binoculars or a small telescope. The system is located at a distance of 137 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +12 km/s. It is located close enough to the ecliptic that it is subject to lunar occultations.

<span class="mw-page-title-main">V Aquilae</span> Star in the constellation Aquila

V Aquilae is a carbon star and semiregular variable star in the constellation Aquila. It has an apparent magnitude which varies between 6.6 and 8.4 and is located around 400 parsecs (1,300 ly) away.

<span class="mw-page-title-main">V373 Cassiopeiae</span> Star system in the constellation Cassiopeia

V373 Cas is a binary star system in the northern constellation Cassiopeia. It is a suspected eclipsing binary with an apparent visual magnitude that decreases from a baseline of 6.03 down to 6.13. The system is located at a distance of approximately 6,200 light years from the Sun, but is drifting closer with a radial velocity of around −25.5 km/s.

<span class="mw-page-title-main">FF Aquilae</span> Star and possible star system in the constellation Aquila

FF Aquilae is a classical Cepheid variable star located in the constellation Aquila. It ranges from apparent magnitude 5.18 to 5.51 over a period of 4.470848 days, meaning it is faintly visible to the unaided eye in rural or suburban settings.

45 Aquilae, abbreviated 45 Aql, is a triple star system in the equatorial constellation of Aquila. 45 Aquilae is its Flamsteed designation. It is located 350 light-years away from Earth, give or take a 6 light-year margin of error, and has a combined apparent visual magnitude of 5.7. The system is moving closer to the Earth with a heliocentric radial velocity of -46 km/s.

<span class="mw-page-title-main">V1472 Aquilae</span> Binary star system in the constellation Aquila

V1472 Aquilae is a triple star system in the equatorial constellation of Aquila. It is a variable star that ranges in brightness from 6.36 down to 6.60. The system is located at a distance of approximately 780 light years from the Sun based on parallax. It is a high-velocity star system with a radial velocity of −112 km/s.

<span class="mw-page-title-main">V1401 Aquilae</span> Star in the constellation Aquila

V1401 Aquilae is a single, semi-regular pulsating star in the equatorial constellation of Aquila. It has the designation HD 190390 from the Henry Draper Catalogue, and was formerly designated 64 Sagittarii. The evolutionary status of the star is unclear, and it has been classified as a post-AGB object, a UU Herculis variable, or belonging to the W Virginis variable subclass of the type II Cepheids. It is dimly visible to the naked eye with an apparent visual magnitude that fluctuates around 6.38. Based on parallax measurements, it is located at a distance of approximately 2,380 light years. It lies 21.5° from the galactic plane.

<span class="mw-page-title-main">1 Delphini</span> Star in the constellation Delphinus

1 Delphini is the Flamsteed designation for a close binary star in the equatorial constellation Delphinus. With a combined apparent magnitude of 6.08, it is barely visible to the naked eye, even under ideal conditions. Parallax measurements put the components at a distance 703 and 780 light years respectively. However, its approaching the Solar System with a radial velocity of 15 km/s.

<span class="mw-page-title-main">CX Draconis</span> Binary star system in the constellation Draco

CX Draconis is an interacting binary star system in the northern constellation of Draco, abbreviated CX Dra. It has the designation HD 174237 in the Henry Draper Catalogue; CX Draconis is the variable star designation. This is a double-lined spectroscopic binary system with a near circular orbit. The brightness of the system undergoes long-term irregular fluctuations, ranging from an apparent visual magnitude of 5.68 down to 5.99. Based on parallax measurements, it is located at a distance of approximately 1,150 light years from the Sun.

References

  1. 1 2 Lynds, C. R. (March 1960), "The Light-Variations of HD 183656", Astrophysical Journal, 131: 390, Bibcode:1960ApJ...131..390L, doi: 10.1086/146842 .
  2. 1 2 3 4 5 6 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
  3. 1 2 3 Haupt, H. F.; Schroll, A. (1974), "Photoelektrische Photometrie von Shell-Sternen", Astronomy and Astrophysics Supplement Series, 15: 311, Bibcode:1974A&AS...15..311H.
  4. 1 2 Samus', N. N; et al. (2017). "General catalogue of variable stars". Astronomy Reports. GCVS 5.1. 61 (1): 80. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID   125853869.
  5. 1 2 Zorec, J.; et al. (November 2016), "Critical study of the distribution of rotational velocities of Be stars. I. Deconvolution methods, effects due to gravity darkening, macroturbulence, and binarity", Astronomy & Astrophysics, 595: 26, Bibcode:2016A&A...595A.132Z, doi: 10.1051/0004-6361/201628760 , hdl: 11336/37946 .
  6. ↑ Houk, N.; Swift, C. (1999), "Michigan catalogue of two-dimensional spectral types for the HD Stars", Michigan Spectral Survey, 5, Bibcode:1999MSS...C05....0H.
  7. 1 2 3 4 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv: 1108.4971 , Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID   119257644.
  8. ↑ "HD 183656". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2021-02-21.{{cite web}}: CS1 maint: postscript (link)
  9. 1 2 Arias, M. L.; et al. (April 2004), "The circumstellar environment of the star V923 Aquilae", Astronomy and Astrophysics, 417 (2): 679–688, Bibcode:2004A&A...417..679A, doi: 10.1051/0004-6361:20034435 , hdl: 11336/37035 .
  10. ↑ Harper, W. E. (1937), "The radial velocities of 917 stars", Publications of the Dominion Astrophysical Observatory Victoria, 7: 1–97, Bibcode:1937PDAO....7....1H.
  11. ↑ Merrill, Paul W.; Burwell, Cora G. (November 1949), "Second Supplement to the Mount Wilson Catalogue and Bibliography of Stars of Classes B and a whose Spectra have Bright Hydrogen Lines", Astrophysical Journal, 110: 387, Bibcode:1949ApJ...110..387M, doi:10.1086/145215.
  12. ↑ Bidelman, W. P. (April 1950), "The Spectrum of HR 7415", Publications of the Astronomical Society of the Pacific, 62 (364): 48, Bibcode:1950PASP...62...48B, doi: 10.1086/126224 , S2CID   119744604.
  13. ↑ Merrill, Paul W.; Lowen, A. Louise (July 1953), "Intercomparison of Shell Spectra", Astrophysical Journal, 118: 18, Bibcode:1953ApJ...118...18M, doi:10.1086/145723.
  14. ↑ Koubský, P.; et al. (February 1989), "Properties and Nature of Be Stars. 13. Radial-Velocity Variations of the Shell Star V 923 AQL (HD 183 656) In the Past Sixty Years", Bulletin of the Astronomical Institute of Czechoslovakia, 40: 31, Bibcode:1989BAICz..40...31K.
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