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	...	...	...	...	...	...	...	...
Xi Scorpii A	~9.5	45.6	0.671	42.3	>1	1.5	...	...	...
Disrupted H.Z. A?	~2.9	...	0	42.3	...	...	...	...	...
Xi Scorpii B	~9.5	45.6	0.671	42.3	>1	>1	...	...	...
Disrupted H.Z. B?	~2.5	...	0	42.3	...	...	...	...	...

NOTE: This animation attempts to relate the possible orbits of Xi Scopii A and B (and possibly disrupted habitable zones around both stars) to their common center of mass, assuming that both stars have a very similar mass. To enlarge the display, the orbits have been arbitrarily rotated by 135 degrees. Although the initial display shows the system's actual orbital tilt (at an inclination of 42.3°) from the visual perspective of an observer on Earth, the orbital inclination of any planet that may be discovered someday around Stars A or B would likely be different from that of the habitable zone orbit depicted here.

The orbit of Stars A and B takes about 45.648 years to complete and is inclined by i=42.3 +/- 1.1° from the perspective of an observer on Earth. Although the binary has an average separation of 19.0 AUs (semi-major axis a = 0.6712 +/- 0.0027"), the extremely high eccentricity (e= 0.7126 +/- 0.0079) of their orbit brings them as close together as 5.5 AUs and as as far apart as 32.6 AUs (Mason et al, 1999; Robert Sutton Harrington, 1987; and Karl Schwarzschild, 1896). Stars C and the binary pair D and E (for which most orbital elements are unknown) are located to far away to be visible in this animation.