• 主题
高级搜索  >
历史搜索 清空历史
首页> 外文期刊>The Astrophysical journal >THE DISPERSING CLOUD CORE AROUND T TAURI
【24h】

THE DISPERSING CLOUD CORE AROUND T TAURI

机译：陶里附近的分散云核心

获取原文
获取原文并翻译 | 示例
           
页面导航
  • 摘要
  • 著录项
  • 相似文献
  • 相关主题

摘要

We have made ~(13)CO (J = 1-0) observations of T Tauri with the Nobeyama Millimeter Array (NMA) and with the Nobeyama 45 m telescope. The ~(13)CO (J = 1-0) emission detected with the NMA shows three different features: (1) a pair of ringlike features surrounding T Tauri with a radius of 30″ (corresponding to 4200 AU at the distance of 140 pc to T Tauri) at the velocities blueshifted and red-shifted by less than 1 km s~(-1) from the systemic velocity, (2) a blueshifted compact feature 3″ east of T Tauri, and (3) another compact feature 7″ southwest of T Tauri at velocities redshifted by more than 1 km s~(-1). On the other hand, the ~(13)CO maps obtained with the 45 m telescope show a smoothly extended feature near the systemic velocity, which is missed in the NMA observations, as well as the above-mentioned three features. The total masses of gas detected with the NMA and the 45 m telescope are estimated to be (0.054-0.23) solar mass and (0.31-1.3) solar mass, respectively. The difference in the estimated mass between the two observations is mainly due to resolving out of the smoothly extended feature in the NMA observations. The ~(13)CO rings are interpreted as biconical outflowing shells in a nearly pole-on configuration. The high-velocity stellar wind ejected from T Tauri is estimated to be energetic enough to drive these outflowing shells. We have analyzed the three-dimensional structure of the shells by correcting for the projection effect on the plane of the sky, and we have found that the spatial extent of the shells is nearly equal to or slightly smaller than the typical size of the molecular cloud cores in the Taurus Molecular Cloud. This fact indicates that the outflowing shells are part of the parent cloud core that still remains around T Tauri, which is now dispersing under the influence of the stellar wind. Such an environment around T Tauri is quite different from those around typical T Tauri stars, which are associated only with compact gaseous components. These results suggest strongly that T Tauri is one of the objects in the transitional phase from the protostar stage, in which a central star is deeply embedded in an infalling envelope, to the T Tauri stage, in which a central star is surrounded by a compact circumstellar disk instead of a spatially extended envelope.
机译：我们已经用Nobeyama毫米阵列（NMA）和Nobeyama 45 m望远镜对T Tauri进行了〜（13）CO（J = 1-0）观测。用NMA检测到的〜（13）CO（J = 1-0）发射显示出三个不同的特征：（1）围绕T Tauri的一对环形特征，半径为30英寸（相当于140距离处的4200 AU） pc至T Tauri）的速度从系统速度向蓝移和红移的速度小于1 km s〜（-1），（2）在T Tauri以东3“处发生蓝移的紧缩特征，以及（3）另一个紧缩特征T Tauri西南7英寸处的速度红移了1 km s〜（-1）以上。另一方面，用45 m望远镜获得的〜（13）CO图显示了靠近系统速度的平滑扩展特征，这在NMA观测中是遗漏的，以及上述三个特征。用NMA和45 m望远镜检测到的气体总质量分别估计为（0.054-0.23）太阳质量和（0.31-1.3）太阳质量。两个观测值之间的估计质量差异主要是由于解决了NMA观测值中平滑扩展的特征。 〜（13）CO环被解释为接近极点配置的双锥形流出壳。从T Tauri喷出的高速恒星风估计能量足够大，足以驱动这些流出的炮弹。我们通过校正在天空平面上的投影效应来分析壳的三维结构，并且发现壳的空间范围几乎等于或略小于分子云的典型大小金牛座分子云的核心。这一事实表明，流出的壳层是母云核心的一部分，仍然保留在T Tauri周围，而T Tauri现在在恒星风的影响下正在散布。 T Tauri周围的环境与典型的T Tauri恒星周围的环境完全不同，后者仅与致密的气态成分有关。这些结果强烈表明，T Tauri是从原恒星阶段过渡阶段的物体之一，在该阶段中，原恒星深深嵌入到一个下降的包层中，而在T Tauri阶段中，中心恒星被紧凑的星团包围圆盘，而不是空间扩展的包膜。

著录项

相似文献

  • 外文文献
  • 中文文献
  • 专利
获取原文

客服邮箱：kefu@zhangqiaokeyan.com

京公网安备：11010802029741号 ICP备案号：京ICP备15016152号-6 六维联合信息科技 (北京) 有限公司©版权所有

  • 客服微信

  • 服务号