59 Serpentis

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59 Serpentis
59SerLightCurve.png
A light curve for 59 Serpentis, plotted from Hipparcos data [1]
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Serpens
Right ascension 18h 27m 12.50775s [2]
Declination 00° 11 45.9912 [2]
Apparent magnitude  (V)5.17 5.29 [3]
Characteristics
Spectral type A0Vs + G:III [2]
U−B color index +0.21 [4]
B−V color index +0.48 [4]
Variable type Irregular? [3]
Astrometry
Radial velocity (Rv)−23.3 [5]  km/s
Proper motion (μ)RA: −3.67 [6]   mas/yr
Dec.: −8.61 [6]   mas/yr
Parallax (π)6.95 ± 0.63  mas [6]
Distance 470 ± 40  ly
(140 ± 10  pc)
Absolute magnitude  (MV)−0.57 [7]
Details
Aa
Mass 6.32 [8]   M
Radius 13 [9]   R
Temperature 5,093 [10]   K
Age 316 [10]   Myr
Ab1
Mass 4.13 [8]   M
Radius 2.2 [9]   R
Temperature 9,700 [9]   K
Ab2
Mass 3.39 [8]   M
Radius 1.8 [9]   R
Temperature 9,700 [9]   K
Ba
Mass 3.17 [8]   M
Radius 1.7 [11]   R
Luminosity 10.1 [11]   L
Surface gravity (log g)4.28 [11]   cgs
Temperature 7,981 [11]   K
Other designations
59 Ser, d Ser, HIP 90441, HR  6918, BD+00°3936, ADS 11353, CCDM J18272+0012
A: HD  169985
B: HD  169985
Database references
SIMBAD data
A
B

59 Serpentis, also known as d Serpentis, is a multiple star in the constellation Serpens. [2] The system shows irregular variations in brightness between magnitudes 5.17 and 5.29. [3]

Components

59 Serpentis appears as a close pair of stars, of 5th magnitude and 7th magnitude respectively, separated by four arc-seconds. The brighter of the two is itself an even closer binary with the two stars separated by only 0.2 , and only 0.1″ when they were first detected. The stars are designated Aa, Ab, and B. [12]

The primary star, component Aa, is a G0 giant. Component Ab is spectroscopic binary with a period of 1.85 days; the two stars are very similar A-class main sequence stars. Component B is an F5V possible astrometric binary, but with little known about the orbit or the possible companion. [8]

A much fainter star 20″ away is also thought to be a member of the system, having a common proper motion and similar Gaia parallax, and is designated as component C. [8]

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References

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