参宿四的伙伴：双星性作为猎户座α长次周期起源
A Buddy for Betelgeuse: Binarity as the Origin of the Long Secondary Period in $α$ Orionis
AI总结：
本文提出参宿四存在低质量伴星参宿四B，用双星模型解释其2170天长次周期与视向速度变化，并给出伴星质量、轨道间距及观测验证条件。
摘要：
我们预言存在参宿四B，即一颗环绕参宿四运行的低质量伴星。这一预言由参宿四光变曲线中存在的2170天长次周期（LSP）所驱动，该周期约为该恒星416天基本径向脉动模式的5倍。虽然双星性目前是长次周期现象的一般性主流假说，但将参宿四中观测到的长次周期与视向速度变化结合起来考虑，就要求对当前的主流物理图像进行修正。光变曲线与视向速度之间的相位差要求伴星在长次周期光度最小时位于参宿四后方，与掩食所对应的系统取向相差180度。我们证明了该模型与现有观测约束的一致性，并指出了所有其他已提出的长次周期假说中存在的矛盾。在这一框架内，我们计算得到参宿四B的质量为$M\sin i =1.17\pm0.7\\,M_\odot$，轨道间距为$1850\pm70\\,R_\odot$，即参宿四半径的$2.43^{+0.21}_{-0.32}$倍。随后，我们描述了在参宿四基本参数及其轨道系统约束下伴星的特征，并讨论了从观测上确认该伴星存在所需的条件。
英文摘要：
We predict the existence of $α$ Ori B, a low-mass companion orbiting Betelgeuse. This is motivated by the presence of a 2170-day Long Secondary Period (LSP) in Betelgeuse's lightcurve, a periodicity $\approx5$ times longer than the star's 416 day fundamental radial pulsation mode. While binarity is currently the leading hypothesis for LSPs in general, the LSP and the radial velocity variation observed in Betelgeuse, taken together, necessitate a revision of the prevailing physical picture. The lightcurve-RV phase difference requires a companion to be behind Betelgeuse at the LSP luminosity minimum, 180 degrees out of phase with the system orientation associated with occultation. We demonstrate the consistency of this model with available observational constraints and identify tensions in all other proposed LSP hypotheses. Within this framework, we calculate a mass for $α$ Ori B of $M\sin i =1.17\pm0.7\,M_\odot$ and an orbital separation of $1850\pm70\,R_\odot$, or $2.43^{+0.21}_{-0.32}$ times the radius of Betelgeuse. We then describe the features of the companion as constrained by the fundamental parameters of Betelgeuse and its orbital system, and discuss what would be required to confirm the companion's existence observationally.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
