Orbital
Distance

(a=AUs)
Orbital
Period

(P=years)
Orbital
Eccentricity

(e)
Orbital
Inclination

(i=degrees)

Mass

(Solar)

Diameter

(Solar)

Density

(Earths)
Surface
Gravity

(Earths)

Metallicity
(Solar)
AB Mass Center0.0........................
Chi1 Orionis A0.8414.20.459311.45......0.89-1.78
Disrupted H.Z. A?~1~1093...............
Chi1 Orionis B5.614.20.45930.15.........0.89-1.78


NOTE: This animation attempts to relate the orbits (and possible habitable zones) of Stars A and B in the Chi1 Orionis AB system to their common center of mass. To enlarge the display, the orbits have been arbitrarily rotated 135 degrees. Although the initial display shows the system's actual orbital tilt (at an inclination of 93) from the visual perspective of an observer on Earth, the orbital inclination of any planet that may be discovered someday around either star would likely be different from those of the habitable zone orbits depicted here.

Spectroscopic, astrometric and radial-velocity analyses reveal a companion with an average separation of 6.4 AUs (a semi-major axis derived from a photocentric estimate of 0.0969" times [1 + (mass A of 1.00 / mass B of 0.15)] -- and a HIPPARCOS parallax of 0.11543 +/- 0.00108"), varying between 3.5 and 9.3 AUs. The two stars move in an elliptical (e= 0.45) orbit that takes about 14.2 years to complete and is inclined at about 93 from the perspective of an observer on Earth (George G. Gatewood, 1994 and Irwin et al, 1992).


 

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