Planet Formation in Binaries - Planetary Exploration and Science: Recent Results and Advances - page 330

binary allow planet formation to proceed successfully around its primary star. We
assume that terrestrial planet formation can also successfully proceed around both
stars of this binary and can result in the formation of Earth-sized objects.
To estimate the boundaries of the binary HZ of this eccentric system, we ignore
its known giant planet and use Eq. ( 13.2 ) considering a fictitious Earth-like planet
in the HZ. We calculate the spectral weight factor W.f;T/ for both stars of this
system (Table 13.2 ) and estimate the locations of the inner and outer boundaries of
the binary's HZ (Table 13.3 ).
As expected (because of the large periastron distance of the binary and the
secondary star being a cool M dwarf), even the maximum flux from the secondary
star does not have a noticeable contribution to the location of the HZ around the
F8V primary of HD 196886. However, being a luminous F star, the primary shows a
small effect on the location of the HZ around the M1V secondary star (Table 13.3 ).
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