Alpha Volantis

Alpha Volantis (Alpha Vol), Latinized from α Volantis, is a binary star^[12] system located in the southern constellation Volans. It has an apparent visual magnitude of +4.00, which is bright enough to be seen with the naked eye. Based upon parallax measurements made with the Hipparcos spacecraft, it is located at a distance of 125 light years from the Sun. As of 2010, the two components of this system had an angular separation of 0.0318″ along a position angle of 286.9°. The magnitude difference between the two components is 0.1.^[13] It is considered a member of the Sirius supercluster.^[5]

α Volantis

Location of α Volantis (circled)
Observation data Epoch J2000.0      Equinox J2000.0
Constellation	Volans
Right ascension	09h 02m 26.79592s[1]
Declination	−66° 23′ 45.8727″[1]
Apparent magnitude (V)	+4.00[2]
Characteristics
Spectral type	kA3hA5mA5 V[3]
U−B color index	+0.13[2]
B−V color index	+0.14[2]
Astrometry
Radial velocity (Rv)	+4.9[4] km/s
Proper motion (μ)	RA: −2.00[1] mas/yr Dec.: +95.51[1] mas/yr
Parallax (π)	26.11±0.12 mas[1]
Distance	124.9 ± 0.6 ly (38.3 ± 0.2 pc)
Absolute magnitude (MV)	+1.60[5]
Orbit[6]
Period (P)	0.652 ± 0.001 yr
Semi-major axis (a)	0.0321 ± 0.0013″
Eccentricity (e)	0.041 ± 0.038
Inclination (i)	101.9 ± 2.3°
Longitude of the node (Ω)	105.3 ± 1.4°
Periastron epoch (T)	2015.593 ± 0.063
Argument of periastron (ω) (secondary)	248.5 ± 34.2°
Details
Mass	1.87[7] M☉
Radius	1.9[8] R☉
Surface gravity (log g)	4.09[3] cgs
Temperature	8,198[3] K
Metallicity [Fe/H]	+0.19[3] dex
Rotational velocity (v sin i)	30.6±0.4[9] km/s
Age	427+183 −377[10] Myr
Other designations
CPD−65°1065, FK5 343, GJ 333.3, GJ 9284, HD 78045, HIP 44382, HR 3615, SAO 250422[11]
Database references
SIMBAD	data

The primary component is an Am star with a stellar classification of kA3hA5mA5 V.^[3] This notation indicates the star has the weak calcium II K-line of an A3 star, and the hydrogen and metallic lines of an A5 star.^[14] It has an estimated age of 427 million years.^[10] In 1992, it was found to be emitting an infrared excess, suggesting the presence of a circumstellar disk of dust.^[15] However, subsequent observations have not confirmed this.^[16]