arXiv 1602.030682016-02-09astro-ph.SR

旋转母核随总质量增加碎裂的双星系统的形成质量

The Formation Mass of a Binary System via Fragmentation of a Rotating Parent Core with Increasing Total Mass

Guillermo Arreaga-Garcia

备注：: accepted for publication in Revista Mexicana de Astronomía y Astrofísica

摘要：

最近的VLA和CARMA观测以前所未有的分辨率显示了双星中的原恒星。具体来说，CB 230 IRS 1和L1165-SMM 1等系统的原恒星质量已经在$0.1-0.25 \, M_{\odot}$范围内被探测到。它们的质量比通常通过数值模拟得到的$0.01 \, M_{\odot}$周围双星形成的质量要大得多。受这些质量差异的影响，本文研究了双星系统的形成质量与母核总质量的关系。为了实现这一目标，我们提出了一套数值模拟的引力坍缩的一个统一的和旋转的核心，在方位角对称的质量种子最初实施，以有利于形成一个致密的灯丝，其中的一个二元系统可能会形成直接碎裂。我们首先观察到，当母核$M_0$的总质量增加时，这种二元形成过程会减少;然后，我们增加了最初提供给旋转核的动能与重力能之比的水平，用$β$表示，以实现所需的细丝直接碎裂。接下来，我们发现双星碎片的质量随着母核的质量而增加，正如预期的那样。在本文中，我们证实了这一预期，并测量了从初始$M_0$获得的二进制质量$M_f$。然后，我们显示了一个示意图$M_0$与$β$，其中所需的二元结构的位置，而热能与引力能$α$的比例保持不变。我们还报道了形成双星系统的原恒星碎片的一些基本物理数据，包括形成质量$M_f$，以及相应的$α_f$和$β_f$。

英文摘要：

Recent VLA and CARMA observations have shown proto-stars in binaries with unprecedented resolution. Specifically, the proto-stellar masses of systems such as CB230 IRS1 and L1165-SMM1 have been detected in the range of $0.1-0.25 \, M_{\odot}$. These are much more massive than the masses generally obtained by numerical simulations of binary formation, around $0.01 \, M_{\odot}$. Motivated by these discrepancies in mass, in this paper we study the formation mass of a binary system as a function of the total mass of its parent core. To achieve this objective, we present a set of numerical simulations of the gravitational collapse of a uniform and rotating core, in which azimuthal symmetric mass seeds are initially implemented in order to favor the formation of a dense filament, out of which a binary system may be formed by direct fragmentation. We first observed that this binary formation process is diminished when the total mass of the parent core $M_0$ is increased; then we increased the level of the ratio of kinetic energy to the gravitational energy, denoted by $β$, initially supplied to the rotating core, in order to achieve the desired direct fragmentation of the filament. Next, we found that the mass of the binary fragment increases with the mass of the parent core, as expected. In this paper we confirm this expectation and also measure the binary mass $M_f$ obtained from an initial $M_0$. We then show a schematic diagram $M_0$ vs $β$, where the desired binary configurations are located while the ratio of the thermal energy to the gravitational energy $α$ is kept fixed. We also report some basic physical data of the proto-stellar fragments that form the binary system, including the formation mass $M_f$, and its corresponding $α_f$ and $β_f$.

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