Sigma Aquilae

σ Aquilae
Location of σ Aquilae (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Aquila
Right ascension 19h 39m 11.64246s[1]
Declination +05° 23′ 51.9797″[1]
Apparent magnitude (V) +5.17[2]
Characteristics
Spectral type B3 V + B3 V:[3]
U−B color index −0.60[2]
B−V color index +0.03[2]
Variable type β Lyr[4]
Astrometry
Radial velocity (Rv)−4.8[5] km/s
Proper motion (μ) RA: +3.97[1] mas/yr
Dec.: −4.26[1] mas/yr
Parallax (π)4.18 ± 0.40 mas[1]
Distance780 ± 70 ly
(240 ± 20 pc)
Absolute magnitude (MV)−1.69[6]
Orbit[7]
Primaryσ Aql A
Companionσ Aql B
Period (P)1.95022±0.0001 d
Eccentricity (e)0
Periastron epoch (T)2420054.331±0.0031 JD
Semi-amplitude (K1)
(primary)		163.52±1.35 km/s
Semi-amplitude (K2)
(secondary)		199±4.1 km/s
Details
σ Aql A
Mass6.8±0.1[8] M☉
Radius4.22±0.06[8] R☉
Luminosity1,862[8] L☉
Temperature18,493[8] K
Rotational velocity (v sin i)36.1±8.9[9] km/s
Age140[10] Myr
σ Aql B
Mass5.4±0.1[8] M☉
Radius3.05±0.11[8] R☉
Luminosity524[8] L☉
Temperature15,848[8] K
Rotational velocity (v sin i)120[3] km/s
Other designations
σ Aql, 44 Aquilae, BD+05 4225, HD 185507, HIP 96665, HR 7474, SAO 124903.[11]
Database references
SIMBADdata

Sigma Aquilae, Latinized from σ Aquilae, is the Bayer designation for a binary star system in the equatorial constellation of Aquila. The baseline apparent magnitude of the pair is +5.17,[2] which, according to the Bortle Dark-Sky Scale, is bright enough to be seen with the naked eye from suburban skies. Because of the Earth's orbit about the Sun, this system has an annual parallax shift of 4.18 mas.[1] This provides a distance estimate of approximately 780 light-years (240 parsecs).

A light curve for Sigma Aquilae, plotted from Hipparcos data[12]

Sigma Aquilae is a double-lined[13] spectroscopic binary system consisting of two massive B-type main sequence stars; each has a stellar classification of B3 V.[3] They are detached components,[10] which means the two stars are sufficiently distant from each other that neither fills its Roche lobe.

Because the orbital plane lies close to the line of sight with the Earth, they form an eclipsing binary system.[4] The two components are each distorted by the gravity of the other star, and their shapes mean that the magnitude of the star system varies constantly even outside of the eclipses, an arrangement known as a Beta Lyrae variable. The brightness of the pair decreases during each eclipse, which occurs with a frequency determined by their orbital period of 1.95026 days. During the eclipse of the primary component the net magnitude decreases by 0.20 to 5.37; the eclipse of the secondary component results in a magnitude decrease of 0.10 to 5.27.[14]

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