We use the stellar evolution code MESA-binary and follow the evolution of three exoplanets and two brown dwarfs (BDs) to determine their potential role in the future evolution of their parent star on the red giant branch (RGB) and on the asymptotic giant branch (AGB). We limit this study to exoplanets and BDs with orbits that have semi-major axis of 1AU 0.25, and having a parent star of mass M>1Mo. We find that the star HIP 75458 will engulf its planet HIP 75458 b during its RGB phase. The planet will remove the envelope and terminate the RGB evolution, leaving a bare helium core of mass 0.4Mo that will evolve to form a helium white dwarf. Only in one system out of five, the planet beta Pic c will enter the envelope of its parent star during the AGB phase. For that to occur, we have to reduce the wind mass-loss rate by a factor of about four from its commonly used value. This strengthens an early conclusion, which was based on exoplanets with circular orbits, that states that to have a non-negligible fraction of AGB stars that engulf planets we should consider lower wind mass-loss rates of isolated AGB stars (before they are spun-up by a companion). Such an engulfed planet might lead to the shaping of the AGB mass-loss geometry to form an elliptical planetary nebula.

中文翻译：

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降低风质量损失率在使系外行星形成行星状星云中的作用

我们使用恒星演化代码 MESA-binary 并跟踪三颗系外行星和两颗棕矮星 (BD) 的演化，以确定它们在红巨星分支 (RGB) 和渐近巨星分支上的母星未来演化中的潜在作用(AGB)。我们将这项研究限制在轨道半长轴为 1AU 0.25 且母星质量 M>1Mo 的系外行星和 BD。我们发现恒星 HIP 75458 将在其 RGB 阶段吞没其行星 HIP 75458 b。这颗行星将移除外壳并终止 RGB 演化，留下质量为 0.4Mo 的裸氦核心，它将演化为氦白矮星。只有在五分之一的系统中，行星 beta Pic c 会在 AGB 阶段进入其母星的包层。为了发生这种情况，我们必须将风质量损失率从其常用值降低约四倍。这加强了早期的结论，该结论基于具有圆形轨道的系外行星，该结论指出，为了使吞噬行星的 AGB 恒星不可忽略，我们应该考虑较低的孤立 AGB 恒星的风质量损失率（在它们旋转之前）由同伴抬起）。这样一颗被吞没的行星可能会导致 AGB 质量损失几何形状的形成，从而形成一个椭圆形行星状星云。