Indeed, stable orbits may extend as far as one third of the closest separation between any two stars in a binary system, but according to NASA's Kepler Mission team, numerical integration models have shown that there is a range of
orbital radii between about 1/3 and 3.5 times the stellar separation for which stable orbits around two stars are not possible (Holman and Wiegert, 1999; Wiegert and Holman, 1997; and Donnison and Mikulskis, 1992).
Not exact matches
We find that 16.5 + / - 3.6 % of main - sequence FGK stars have at least one planet
between 0.8 and 1.25 Earth
radii with
orbital periods up to 85 days.
Multiple planets transiting the same star reveal more: period ratios determine stability and dynamics, mutual gravitational interactions reflect planet masses and
orbital shapes, and the fraction of transiting planets obs... ▽ More When an extrasolar planet passes in front of its star (transits), its
radius can be measured from the decrease in starlight and its
orbital period from the time
between transits.
Abstract: When an extrasolar planet passes in front of its star (transits), its
radius can be measured from the decrease in starlight and its
orbital period from the time
between transits.
Finally, we investigate tentative correlations
between host - star masses and planet candidate
radii,
orbital periods, and multiplicity, but caution that these results may be influenced by the small sample size and detection biases.