|Aab Mass Center||0.0||...||...||...||...||...||...||...||...|
|CM Draconis Aa||0.0084||0.0035||0.005||89.8||0.23||0.25||...||...||...|
|CM Draconis Ab||0.0094||0.0035||0.005||89.8||0.21||0.062||...||...||...|
|Center of H.Z.||0.32||0.073||0||89.8||...||...||...||...||...|
NOTE: This animation attempts to relate the possible orbits of CM Draconis Aab (and their circumbinary habitable zone) to their common center of mass. Although the initial display shows the system's actual orbital tilt (at an inclination of 89.8°) from the visual perspective of an observer on Earth, the orbital inclination of any planet that may be discovered someday around either star could be different from that of the habitable zone orbits depicted here.
CM Draconis Aa has a close, double-lined spectroscopic companion Ab, with which it forms a non-contact, eclipsing binary, and a wide common-proper-motion companion B which is too far away to be depicted here (even if sufficient data were available). Stars Aab and B have an observed separation of about 420 AUs (25.7"). On the other hand, stars Aa and Ab have are separated by only 3.76 solar radii, which is about 14.9 times the radius of CM Draconis Aa (Claud H. Lacy, 1977), and have a mutual orbital period of just under 1.27 days (Deeg et al, 1998; Metcalfe et al, 1996); and Claud H. Lacy, 1977). Not surprisingly, their close orbit is high circular (e= 0.0050 +/- 0.0015) and is inclined by 89.8° from the perspective of an observer on Earth (see a TEP page on CM Draconis).
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