Planet Formation in Binaries - Planetary Exploration and Science: Recent Results and Advances - page 328

Fig. 13.15 Same as Fig. 13.14 , with the F star as the primary

component A of this system is a G2V star with a mass of 1:1M Sun , luminosity
of 1:519L Sun and an effective temperature of 5,790 K. Its component B has a
spectral type of K1V, and its mass, luminosity and effective temperature are equal
to 0:934M Sun , 0:5L Sun and 5,214 K, respectively.
The announcement of a probable super-Earth planet with a mass larger than 1.13
Earth masses around Ǜ Cen B (Dumusque et al. 2012 ) indicates that unlike the
region around Ǜ Cen A where terrestrial planet formation encounters complications,
planet formation is efficient around this star (Guedes et al. 2008 ; Thebault et al.
2009 ) and it could also host a terrestrial planet in its HZ. Here we assume that
planet formation around both stars of this binary can proceed successfully, and they
both can host Earth-like planets. We calculate the spectral weight factors of both Ǜ
CenAandB(Table 13.2 ) and, using the minimum and maximum added flux of the
secondary star, estimate the limits of their binary HZs using Eq. ( 13.2 ).
Tab le 13.3 shows the estimates of the boundaries of the binary HZ around
each star. The terms Max and Min in this table correspond to the planet-binary
configurations of .;/ D .0;0/ and .0;180 ı / where the planet receives the
maximum and minimum total flux from the secondary star, respectively. As shown
here, each star of the Ǜ Centauri system contributes to increasing the limits of the
binary HZ around the other star. Although these contributions are small, they extend