Orbital
Distance

(a=AUs)
Orbital
Period

(P=years)
Orbital
Eccentricity

(e)
Orbital
Inclination

(i=degrees)
Mass
Estimate

(Solar)

Diameter

(Solar)

Density

(Earths)
Surface
Gravity

(Earths)

Metallicity
(Solar)
AC-B Mass Center0.0........................
EZ Aquarii B0.432.250.437112.4~0.10.08-0.35.........
Inner H.Z. Edge B?0.0220.0100112.4...............
Outer H.Z. Edge B?0.0540.0400112.4...............
AC Mass Center0.792.250.437112.4...............
EZ Aquarii A0.0530.010112.4?~0.10.08-0.35.........
Inner H.Z. Edge A?0.0220.0100112.4?...............
Outer H.Z. Edge A?0.0540.0400112.4?...............
EZ Aquarii C0.0770.010112.4?~0.10.08-0.35.........
Inner H.Z. Edge C?0.0220.0100112.4?...............
Outer H.Z. Edge C?0.0540.0400112.4?...............


NOTE: This animation attempts to relate the orbits (and possible habitable zones) of Stars A, B, and C in the EZ Aquarii 3 system to their respective centers of mass. To enlarge the display, the orbits have been arbitrarily rotated by 45 degrees. While the initial display shows the AC-B System's actual orbital tilt (at an inclination of 112.4) from the visual perspective of an observer on Earth, the orbital inclination of any planet that may be discovered someday in this star system would likely be different from those of the habitable zone orbits depicted here.

According to the new Sixth Catalog of Orbits of Visual Binary Stars, Stars A and B have an "average" separation, or semi-major axis, of about 1.22 times the Earth-Sun distance (AU) in an eccentric orbit (e= 0.437), a period of about 2.25 years, and an inclination from the perspective of an observer on Earth of about 112.4 (Woitas et al, 2000). In addition, Star A is a spectroscopic binary (whose companion has been designated as star "C") with an orbit period of only 3.8 days (Defosse et al, 1999).


 

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