X-Ray Observation on the Monoceros R2 Star-Forming Region with the Chandra ACIS-I Array
X-Ray Observation on the Monoceros R2 Star-Forming Region with the Chandra ACIS-I Array
复制标题
使用钱德拉 ACIS-I 阵列对麒麟座 R2 恒星形成区域进行 X 射线观测
DOI：
10.1093/pasj/55.3.635
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发表时间：
2003
影响因子：
2.3
通讯作者：
P. S. University
中科院分区：
文献类型：
--
作者：
H. Nakajima;K. Imanishi;S. Takagi;K. Koyama;M. H. D. O. Physics;Graduate School of Science;Kyoto University;D. Astronomy;Astrophysics;P. S. University
我们报告了钱德拉ACIS-I对麒麟座R2云中心区域（Mon R2）的观测结果，这是一个距离为830 pc的高质量恒星形成区（SFR）。在100 kS的深度曝光下，我们检测到368个X射线源，其中约80%与近红外（NIR）对应物相匹配。我们系统地分析了大多数X射线源的光谱和时间变化，并首次提供了一个全面的X射线源目录。使用J-，H-和K-波段的近红外对应的星等，我们估计的演化阶段（经典的金牛座T星和弱线金牛座T星）和质量的X射线发射源，并分析了X射线的性质作为年龄和质量的函数。我们发现了一个边缘暗示，经典金牛座T星的温度（2.4keV）略高于弱线金牛座T星（2.0keV）。相当一部分的高质量和中等质量的源具有类似于低质量源（2.0keV）的时间可变性和高等离子体温度（2.7keV）。我们对其他SFR，猎户座星云星团和猎户座分子云-2/3进行了相同的分析，并获得了与Mon R2相似的结果。这支持了Kohno等人（2002，ApJ，567，423）和Preibisch等人（2002，A&A，392，945）获得的早期观察结果，即高质量和中等质量的年轻恒星物体通过磁活动发射X射线。我们还发现了一个显着的差异，在空间分布之间的X射线和近红外光源。
We report on the results of the Chandra ACIS-I observation on the central region of the Monoceros R2 cloud (Mon R2), a high-mass star-forming region (SFR) at a distance of 830pc. With a deep exposure of ∼ 100ks, we detected 368 X-ray sources, ∼80% of which were identified with the near-infrared (NIR) counterparts. We systematically analyzed the spectra and time variability of most of the X-ray emitting sources and provided a comprehensive X-ray source catalog for the first time. Using the J-, H-, and K-band magnitudes of the NIR counterparts, we estimated the evolutionary phase (classical T Tauri stars and weak-lined T Tauri stars) and the mass of the X-ray emitting sources, and analyzed the X-ray properties as a function of the age and mass. We found a marginal hint that classical T Tauri stars have a slightly higher temperature (2.4keV) than that of weak-lined T Tauri stars (2.0keV). A significant fraction of the high- and intermediate-mass sources have a time variability and high plasma temperatures (2.7keV) similar to those of low-mass sources (2.0keV). We performed the same analysis for other SFRs, the Orion Nebula Cluster and Orion Molecular Cloud-2/3, and obtained similar results to Mon R2. This supports the earlier results of this observation obtained by Kohno et al. (2002, ApJ, 567, 423) and Preibisch et al. (2002, A&A, 392, 945) that high- and intermediate-mass young stellar objects emit X-rays via magnetic activity. We also found a significant difference in the spatial distribution between X-ray and NIR sources.
来自 O/I 类原恒星的 X 射线
DOI：
--
发表时间：
2004
期刊：
proceedings of IAU symposium "Star Formation at High Angular Resolution" 221
影响因子：
--
作者：
Tsuboi;Y.
通讯作者：
Y.