• 主题
高级搜索  >
历史搜索 清空历史
首页> 外文期刊>The Astrophysical journal >THE MID-INFRARED EVOLUTION OF NOVA V1974 CYGNI
【24h】

THE MID-INFRARED EVOLUTION OF NOVA V1974 CYGNI

机译：NOVA V1974 CYGNI的中红外进化

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 observed nova V1974 Cygni (1992) at mid-infrared wavelengths λ = 7.5-13 μm nine times between 1992 April (54 days after the outburst) and 1994 July (day 882). Low- and medium-resolution spectra recorded the evolution of hydrogen recombination lines, free-free continuum emission, and the [Ne Ⅱ] 12.8 μm, [Ne Ⅵ] 7.6 μm, and [Mg Ⅶ] 9.0 μm forbidden lines through the nebular and coronal line phases of this event. We interpret the spectra in terms of a series of CLOUDY models that evolve in a physically realistic way throughout the period of observation. The models indicate the presence in the ejecta of three major components of differing densities, but with masses, geometries, and expansion velocities that are consistent with values indicated by optical and UV observations of the nova. In our models the abundances of neon and magnesium relative to hydrogen are 50 and 5 times their solar values, respectively, and significant overabundances of other metals are also implied. We discuss many effects such as the increase of line widths with ionization and the origin of coronal line emission as they are represented by our modeling.
机译：在1992年4月（爆发后54天）至1994年7月（882天）之间，我们在中红外波长λ= 7.5-13μm处观测到了新星V1974 Cygni（1992）。低分辨率和中分辨率光谱记录了氢重组线的演化，自由-自由连续谱的发射以及[NeⅡ] 12.8μm，[NeⅥ] 7.6μm和[MgⅦ] 9.0μm禁带线通过星状核和核的演化。此事件的冠状线阶段。我们用一系列CLOUDY模型来解释光谱，这些模型在整个观察期间以物理逼真的方式演化。该模型表明，在射流中存在密度不同的三个主要成分，但它们的质量，几何形状和膨胀速度与该新星的光学和紫外线观测所表明的值一致。在我们的模型中，氖和镁相对于氢的丰度分别是其太阳值的50倍和5倍，并且还暗示了其他金属的明显丰度。我们讨论了许多影响，例如电离引起的线宽增加以及建模所代表的日冕线发射的起源。

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