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	...	...	...	...	...	...	...	...
Struve 2398 A	23.8	408	0.53	66.0	0.34-0.35	0.34	...	...	0.45-0.49
Inner H.Z. Edge A	0.123	0.073	0	66.0	...	...	...	...	...
Outer H.Z. Edge A	0.240	0.199	0	66.0	...	...	...	...	...
Struve 2398 B	32.0	408	0.53	66.0	0.26-0.27	0.27	...	...	0.42-0.45
Inner H.Z. Edge B	0.091	0.054	0	66.0	...	...	...	...	...
Outer H.Z. Edge B	0.146	0.054	0	66.0	...	...	...	...	...

NOTE: This animation attempts to relate the possible orbits of Struve 2398 AB (and their tiny habitable zones) 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 66.0°) 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.

Although the star and its stellar companion B are known to have an eccentric orbit, the specific orbital elements may still be uncertain. In 1958, Wilhelm F. Rabe (1893-1958) derived a period of 346 years with an average distance of 42 AUs (based on updated parallax) and an eccentricity of 0.55, so that the stars swing between 19.0 and 65.3 AUs apart. Using photographic plates from 1918 to 1987, however, (Wulff D. Heintz, 1987) subsequently calculated a period of 408 years with an eccentricity of 0.53, and an average distance of 56 AUs where the pair swings between 26 and 86 AUs apart.