T Ori C 中的三重诱导并合：解决 proplyd 寿命问题与 M42 异常年轻的外壳
A triple-induced merger in T Ori C, solves the proplyd lifetime problem and the curiously young shell of M42
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中文总结 AI 辅助
提出 θ¹ Ori C1 由三重系统诱导并合形成，其增亮解释了猎户座星云 proplyd 寿命与年轻外壳的矛盾，并用蒙特卡洛模拟验证了该情景。
中文摘要 AI 辅助
猎户座星云星团中的恒星年龄与其原行星盘快速的外部光蒸发之间长期存在矛盾。最近，猎户座星云的外壳也被发现其动力学年龄比恒星年轻。我们提出了一种新情景来解决这两个年龄问题。在我们的情景中，ONC 中最庞大的恒星 θ¹ Ori C1 是由当前双星伴星 θ¹ Ori C2 引起的 vZLK 振荡所诱导的两颗双星之间的并合形成的。这次并合发生在最近一次恒星形成事件与今天之间，导致光度增加，从而增强了外部光蒸发并加速了外壳的膨胀。我们使用蒙特卡洛模拟来探索两方面：θ¹ Ori C1 的突然增亮是否能调和恒星年龄与外壳膨胀，以及 θ¹ Ori C 的三重前身星能否在相关时间尺度上导致恒星并合。几十万年前 θ¹ Ori C1 的突然增亮可以重现今天的外壳，同时保持系统年龄接近恒星年龄。然而，所需的恒星风光度增加量大于简单并合所能解释的。在较低光度下，将相对较多的冷光蒸发风物质混合到热气泡中可能导致所需的增加，我们确定了这一效应所需强度的下限。此外，我们发现前身星三重系统很容易并合，其时间尺度甚至比情景所需的更短。这些并合可能因前主序潮汐效应、自转以及与其他星团成员的扰动遭遇而延迟。我们提出的由 von Zeipel-Lidov-Kozai 演化驱动的并合情景解决了两个问题：猎户座星云的 proplyd 问题和外壳寿命问题。
英文摘要
There has long been a tension between the stellar ages in the Orion Nebula Cluster and the rapid external photoevaporation of its protoplanetary discs. Recently, the shell of the Orion Nebula has similarly been found to be dynamically younger than the stars. We propose a new scenario to resolve both age problems. In our scenario the ONC's most massive star, $θ^1$~Ori~C1, formed from the merger between two binary stars induced by vZLK oscillations due to the present-day binary companion $θ^1$~Ori~C2. This merger, happening between the last episode of star formation and today, resulted in an increased luminosity, leading to stronger external photoevaporation and accelerated expansion of the shell. {We use Monte Carlo simulations to explore both whether a sudden brightening of $θ^1$~Ori~C1 could reconcile the stellar ages and shell expansion, and whether triple progenitors to $θ^1$~Ori~C\, could result in stellar mergers on the relevant timescale. A sudden brightening of $θ^1$~Ori~C1 a few hundred thousand years ago can reproduce today's shell while maintaining a system age close to the stellar age. However, the required increase in stellar wind luminosity is greater than a simple merger can explain. At lower luminosity, the mixing of a relatively greater amount of cool photoevaporative wind material into the hot bubble could result in the required increase, and we identify a lower limit on the required strength of this effect. Additionally, we find that progenitor triples merge readily, on timescales even shorter than the scenario would require. These mergers could be deferred by increased pre-main sequence tidal effects, rotation, and perturbing encounters with other cluster members. Our proposed scenario with a merger driven by von Zeipel-Lidov-Kozai evolution solves two problems; the Orion Nebula's proplyd problem and the shell lifetime problems.
发表机构
- Leiden University（莱顿大学）
- University of Concepción（康塞普西翁大学）
- National Institute for Nuclear Physics – INFN, Sezione di Trieste（意大利国家核物理研究所-的里雅斯特分部）
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