[ The annual parallax shift of {{Val|2.6|ul=mas}}[1] provides a distance estimate of around 1,200 light years. It is moving further away from Earth with a heliocentric radial velocity of +10 km/s.[5]]System
The Washington Double Star Catalog lists three visible components for this system. The brightest, component A, is of visual magnitude 4.50. Component B has a magnitude of 7.179,[25] and as of 2000 lies at an angular separation of {{Val|7.10|ul=arcsecond}} from A, along a position angle (PA) of 102°. Component C is a magnitude 9.125 star[25] at a separation of {{Val|36.20|u=arcsecond}} from A at a PA of 191°. The physical link between the stars was described on the basis of their dynamic parallax and mean velocities.[27] The three components A, B, and C have Gaia Data Release 2 parallaxes of {{val|2.6564|0.2314|ul=mas}}, {{val|2.1771|0.0490|u=mas}}, and {{val|1.6097|0.0400|u=mas}} respectively.[1]
Properties
Component A has a stellar classification of B3 III, and is categorized as a Be star. It shows photometric variations with multiple periods around 4.6 days and line-profile variations with a period of 2.318 days. The radial velocity of this star is constant.[4] It has 10[11] times the Sun's radius and shines with 3,082[5] times the Sun's luminosity from its photosphere at an effective temperature of 15,000 K.[11]
The component B shows a variation in spectra consistent with being a double-lined spectroscopic binary. The brighter member (Ba) is a silicon star with a class of A0 IVpSi, while the fainter component (Bb) is of type A2. Component C has a class of K0 III, indicating it is an evolved giant star. The measured effective temperature of C is 5,500 K. The fact that component A most likely shares a common origin with C suggests that the former is much older than expected, and may actually be a blue straggler formed from the merger of a close binary. This could have been caused by the gravitational influence of an unseen companion of A.[4]
References
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