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 Center	0.0	...	...	...	...	...	...	...	...
EZ Aquarii B	0.43	2.25	0.437	112.4	~0.1	...	...	...	...
Center of H.Z. B	0.06	...	0	112.4	...	...	...	...	...
AC Mass Center	0.79	2.25	0.437	112.4	...	...	...	...	...
EZ Aquarii A	0.053	0.01	0	?	~0.1	0.08-0.35	...	...	...
Disrupted H.Z. A	0.09	...	0	?	...	...	...	...	...
EZ Aquarii C	0.077	0.01	0	?	~0.1	...	...	...	...
Disrupted H.Z. C	<0.06	...	0	?	...	...	...	...	...

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. 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, Indeed, 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. (For the purposes of this animation, the masses of Stars A, B, and C are assumed to be 0.13, 0.12, and 0.09 Solar, respectively.)

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).