Image Details
Caption: Figure 7.
N-body simulations of the HD 33142 system, including stellar evolution effects on the orbital evolution, in particular the planetary semimajor axis a (colored lines). Initial conditions from the N-body simulations were adopted from the stable median posterior values presented in Table 3. The evolution of the stellar radius (dashed curve and the underlying gray area) is expressed in astronomical units. The WD phase is off-scale, since the stellar radius at age 3.2 Gyr is only ∼4 × 10−5 au.
© 2022. The Author(s). Published by the American Astronomical Society.