V923 Aquilae

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Template:Short description

V923 Aquilae
File: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 Template:RA[2]
Declination Template:DEC[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 Template:Engvar −0.31[3]
B−V Template:Engvar Script error: No such module "val".[7]
Variable type Be star[4]
Astrometry
Radial velocity (Rv)Script error: No such module "val".[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]
DistanceTemplate:Rnd ± Template:Rnd ly
(Template:Rnd ± Template:Rnd pc)
Absolute magnitude (MV)−0.87[7]
Details[5]
Primary
MassScript error: No such module "val". Template:Solar mass
LuminosityScript error: No such module "val". Template:Solar luminosity
Surface gravity (log g)Script error: No such module "val". cgs
TemperatureScript error: No such module "val". K
Rotational velocity (v sin i)Script error: No such module "val". km/s
Secondary
Mass~0.5 Template:Solar mass
Metallicity [Fe/H]{{{metal_fe2}}} dex
Other designations
Template:Odlist[8]
Database references
SIMBADdata

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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 (Script error: No such module "val".). 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]

References

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  2. a b c d e f Template:Cite Gaia DR2
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  7. a b c d Script error: No such module "citation/CS1".
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  13. Script error: No such module "citation/CS1".
  14. Script error: No such module "citation/CS1".

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External links

Template:Stars of Aquila