论文标题
早期型星的对流穿透
Convective Penetration in Early-Type Stars
论文作者
论文摘要
观察结果表明，恒星的对流核心必须从上覆的辐射区域摄入大量材料，但是这种混合的程度和导致其的机制仍然不确定。最近，Anders等。 （2021）开发了一种对流渗透理论，并通过3D数值流体动力学模拟对其进行了校准。在这里，我们采用该理论来预测早期型主要序列恒星中对流边界混合的程度。我们发现，对流穿透会产生足够的混合，以解释从星空学和黯然失色的二进制研究推断出的核心质量，并匹配观察到的质量和年龄趋势。虽然该理论仍然存在不确定性，但该协议表明，早期型主序列恒星中最对流的边界混合是由对流穿透引起的。最后，我们为质量恒星的核心对流穿透程度提供了一个拟合公式，质量范围为$ 1.1-60 m_ \ odot $。
Observations indicate that the convective cores of stars must ingest a substantial amount of material from the overlying radiative zone, but the extent of this mixing and the mechanism which causes it remain uncertain. Recently, Anders et al. (2021) developed a theory of convective penetration and calibrated it with 3D numerical hydrodynamics simulations. Here we employ that theory to predict the extent of convective boundary mixing in early-type main-sequence stars. We find that convective penetration produces enough mixing to explain core masses inferred from asteroseismology and eclipsing binary studies, and matches observed trends in mass and age. While there are remaining uncertainties in the theory, this agreement suggests that most convective boundary mixing in early-type main-sequence stars arises from convective penetration. Finally, we provide a fitting formula for the extent of core convective penetration for main-sequence stars in the mass range from $1.1-60 M_\odot$.
