Orbital Distance (a=AUs)	Orbital Period (P=years)	Orbital Eccentricity (e)	Orbital Inclination (i=degrees)	Mass (Earths)	Diameter (Earths)	Density (Earths)	Surface Gravity (Earths)	Metallicity (Solar)
AB Mass Center	0.0	...	...	...	...	...	...	...	...
Eta Cassiopeiae A	27.2	480	0.497	34.76	300,000	107	...	...	0.63-0.68
Center of H.Z. A	1.13	1.15	0	34.76	...	...	...	...	...
Eta Cassiopeiae B	44.2	480	0.497	34.76	190,000	71	...	...	0.63-0.68
Center of H.Z. B	0.18	0.10	0	34.76	...	...	...	...	...

NOTE: This animation attempts to relate the orbits (and possible habitable zones) of Stars A and B in the Eta Cassiopeiae AB system to their common center of mass. The initial display does not show the system's actual orbital tilt (at an inclination of 34.76°) from the visual perspective of an observer on Earth. Indeed, the orbital inclination of any planet that may be discovered some day around either star would likely be different from those of the habitable zone orbits depicted here.

According to a 1969 article by Kaj Aage Gunnar Strand (1907-2000), Star A and B are separated by an "average" distance of 71 times the Earth-Sun distance (AU) (of a semi-major axis) in an eccentric orbit (e= 0.497) of about 480 years, so that the two stars get as close as 36 AU and as far away as 107 AU. However, Achird is no longer thought to have a spectroscopic binary with a nine-day orbital period (Morbey and Griffin, 1987; and Helmut Abt, 1987).