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 Center	0.0	...	...	...	...	...	...	...	...
Mu Cassiopeiae A	0.27	21.75	0.56	106.8	0.74	0.82	...	...	0.13-0.28
Disrupted H.Z. A	0.68	0.48	0	106.8	...	...	...	...	...
Mu Cassiopeiae B	1.17	21.75	0.56	106.8	0.17	0.29	...	...	0.13-0.28
Center of H.Z. B	0.08	0.052	0	106.8	...	...	...	...	...

NOTE: This animation attempts to relate the orbits (and possible habitable zones) of Stars A and B in the Mu Cassiopeiae AB system to their common center of mass. To enlarge the display, the orbits have been arbitrarily rotated by 45 degrees. Although the initial display shows the system's actual orbital tilt (at an inclination of 110.0°) 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.

The Sixth Catalog of Orbits of Visual Binary Stars appears to be undecided over the merits of alternative orbit estimates. Here, we will use those derived from adaptive optical images as well as historical data (Drummond et al, 1995). In those calculations, Star A was found to have 74 percent of Sol's mass, 82 percent of its diameter, 46 percent of its bolometric luminosity, and to be around 10 billion years old based on a low estimate of helium content. Star A appears to be separated from its companion by a semi-major axis of 1.44 AUs (a= 0.1908 +/- 0.0043 arcseconds) and moving in a highly eccentric orbit (e=0.561 +/- 0.017) that takes 21.753 +/ 0.059 years to complete. Moving as close as 0.63 AUs but as far apart as 2.25 AUs, their orbit is inclined at 106.8° +/-0.9° from the perspective of an observer on Earth.

Alternatively, studies of observations between 1937 and 1980 by Sarah Lee Lippincott (1981) and updated to 1993 by Heintz and Cantor (1994) found that the primary star has an "average" separation from its companion star B of about 1.42 AUs (of a semi-major axis) in an orbit that takes about 21.4 years to complete and is inclined at 110.0° from the perspective of an observer on Earth (Heintz Orbit Table, 12/1997). The pair has a highly eccentric orbit (e= 0.62) and so the separation between the two stars varies between 0.54 and 2.3 AUs. According to Heintz and Cantor (1994), orbit calculations using photographic exposures from 1933 to 1978 by Russell and Gatewood (1984) "agree quite well."