Planet Formation in Binaries - Planetary Exploration and Science: Recent Results and Advances - page 314

1.0 and 1.5 solar masses, and the semimajor axis and eccentricity of the binary
were varied in the range of 20-40 AU and 0-0.4, respectively. For each value of
the mass of the primary, Haghighipour and Raymond ( 2007 ) used the planetary
orbit stability criterion, given by Rabl and Dvorak ( 1988 ) and Holman and Wiegert
( 1999 ), and identified the combination of the mass, semimajor axis and eccentricity
of the binary for which the giant planet would maintain a stable orbit at 5 AU. They
then considered a disc of 115 Moon-to-Mars-sized bodies with masses ranging from
0.01 to 0.1 Earth masses.
Figure 13.7 shows the results of a sample of their simulations for a binary with a
mass ratio of 0.5 and for different values of its semimajor axis and eccentricity. The
grey area corresponds to the boundaries of the habitable zone of the primary star
(Kasting et al. 1993 ). As a point of comparison, the inner planets of the solar system
are also shown. As shown here, many planets of the same or similar size as Earth
and with substantial amount of water formed in and around 1 AU. Figure 13.8 shows
Fig. 13.7 Late stages of planet formation: terrestrial planet formation and water delivery in the
presence of an already formed giant planet. Results of simulations in a binary system with a mass
ratio of 0.5 and for different values of the eccentricity .e b / and semimajor axis .a b / of the binary.
The solar system's configuration is given as a comparison (Taken from Haghighipour and Raymond
2007 , courtesy of the Astrophysical Journal)