热木星在恒星主序阶段会发生潮汐瓦解吗？
Are Hot Jupiters Tidally Disrupted During Stellar Main Sequence?
浏览论文内容
中文总结 AI 辅助
针对热木星主序阶段是否会潮汐瓦解的问题，研究通过更可靠的垂直速度弥散指标重新分析过往数据，并结合TESS新发现样本验证，发现没有强运动学证据支持类太阳恒星周围多数热木星会在主序阶段被潮汐摧毁。
中文摘要 AI 辅助
热木星（HJs）一旦进入极近的轨道，预计会因与宿主恒星的潮汐相互作用而发生轨道衰减。然而，潮汐耗散的强度具有高度不确定性，热木星是否会在恒星主序阶段发生潮汐瓦解仍是一个悬而未决的问题。此前的一项研究发现，热木星宿主恒星的银河系总速度弥散小于同类型场星，研究者将其解读为潮汐瓦解的证据。我们重新审视了这项研究，发现在使用更可靠的垂直速度弥散（$σ_W$）作为年龄指标，并考虑到热木星样本的异质性和各向异性后，热木星宿主恒星与匹配场星之间的运动学年龄差异显著减小。作为独立验证，我们收集了TESS（凌日系外行星巡天卫星）新发现的热木星，发现它们的$σ_W$在统计学上与匹配场星的$σ_W$相似。我们还发现，场星与理论上易受瓦解影响、轨道周期$P<2$天的超热木星的宿主恒星之间，$σ_W$没有统计学上的显著差异。我们的结果表明，在考虑年龄-速度弥散关系中的系统误差后，恒星运动学没有提供统计学上的有力证据，证明类太阳恒星周围的大部分热木星会在恒星主序阶段被潮汐摧毁。
英文摘要
Once hot Jupiters (HJs) reach their very close orbits, they are expected to experience orbital decay due to tidal interactions with their host star. However, the strength of tidal dissipation is highly uncertain, and it remains an open question whether HJs are tidally disrupted during the stellar main sequence. A previous study found that HJ hosts have a smaller Galactic total velocity dispersion than their field star counterparts, which they interpreted as evidence of tidal disruption. We revisit this study and find that, after using the more reliable vertical velocity dispersion ($σ_W$) as the age indicator and accounting for the heterogeneity and anisotropy of their HJ sample, the kinematic age difference between their HJ hosts and matched field stars is significantly reduced. As an independent check, we collect HJs newly discovered by TESS and find that their $σ_W$ is statistically similar to that of matched field stars. We also find no statistically significant $σ_W$ difference between the field stars and the theoretically vulnerable ultra-hot Jupiters with $P<2$ d. Our results suggest that, after accounting for systematics in the age--velocity dispersion relation, there is no statistically strong evidence from the stellar kinematics that a large fraction of hot Jupiters around Sun-like stars are tidally destroyed during the stellar main sequence.
