...
  • 主题
高级搜索  >
历史搜索 清空历史
首页> 外文期刊>Astronomy letters >Symbiotic nova V1016 Cygni: Evolution of the dust envelope and the gaseous nebula
【24h】

Symbiotic nova V1016 Cygni: Evolution of the dust envelope and the gaseous nebula

机译：共生新星V1016 Cygni：尘埃包壳和气态星云的演变

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

As a result of the next cycle of our long-term monitoring, we present our UBV JHKLM photometry for the symbiotic nova V1016 Cyg in 2008-2014. The star continued to systematically fade and redden in UBV: over this period, the brightness declined by 0a(1)integral 1 in V and by 0a(1)integral 2 in B and U, the B-V color index increased by 0a(1)integral 1, and U-B barely changed. On the color-color (U-B, B-V) diagram, the star moved approximately horizontally rightward with a slight bluing in U-B starting from 2000. Our JHKLM photometry has shown a decline in the mean infrared (IR) brightness and a rise in the mean IR color indices after 2004 due to an increase in the optical depth of the dust envelope. The brightness decline and reddening of the Mira in the near infrared reached their extreme values over the entire period of the system's observations by the end of 2014. The pulsation period of the Mira is determined with confidence: P = 465 +/- 5 days. The distance to the Mira, D = 2.92 +/- 0.16 kpc, and its parameters, the radius R (*) = (470 +/- 50) R (aS (TM)) and luminosity L (*) = (9200 +/- 1900) L (aS (TM)), have been estimated from the observations of V1016 Cyg at its maximum J brightness and at its minimum J-H color index. The temperature of the star during its pulsations varied within the range T (*) = 2100-2700 K.We have estimated the parameters of the dust envelope near its maximum (in 2004) and minimum (in 2012-2014) IR brightness. The mass of the dust envelope almost doubled in ten years, with the rate of dust supply being Delta M (d) similar to 10(-7) M (aS (TM)) yr(-1). Using a low-resolution spectrograph, we performed absolute spectrophotometry for V1016 Cyg in 1995-2013 in the range lambda 4340-7130 . We have shown that almost all absolute fluxes in lines and in continuum at lambda 4400 decrease monotonically after 2000, while the relative intensities of [O III], [Fe VII], and [Ca VII] lines increase after the minimum that probably occurred in the 1990s. The significant (approximately by a factor of 10 from 1995 to 2013) decrease of the flux in the Raman O VI lambda 6825 line reflects a change of conditions in the formation zone of this line due to the absorption of some O VI lambda 1032 photons in the newly forming dust envelope of the cool component.
机译：作为下一轮长期监测的结果，我们于2008-2014年推出了针对共生新星V1016 Cyg的UBV JHKLM光度法。恒星在UBV中继续系统地褪色和变红：在此期间，亮度在V中下降了0a（1）积分1，在B和U中下降了0a（1）积分2，BV颜色指数增加了0a（1）整数1，UB几乎没有变化。在彩色（UB，BV）图上，恒星从2000年开始大约向右水平移动，并且在UB中略微发蓝。我们的JHKLM光度法显示平均红外（IR）亮度下降而平均红外（IR）上升颜色指数是由于尘封的光学深度增加而导致的2004年以后的颜色指数。到2014年底，在整个系统观测期间，Mira的近红外亮度下降和变红达到其极值。Mira的脉动周期确定为：P = 465 +/- 5天。到Mira的距离D = 2.92 +/- 0.16 kpc及其参数，半径R（*）=（470 +/- 50）R（aS（TM））和光度L（*）=（9200 + /-1900）L（aS（TM）），是根据V1016 Cyg在其最大J亮度和最小JH颜色指数下的观察值估计的。恒星在脉动过程中的温度在T（*）= 2100-2700 K范围内变化。我们估计了尘埃包络线的参数接近其最大（2004年）和最小（2012-2014年）IR亮度。尘封的质量在十年内几乎翻了一番，粉尘的供给速度为Delta M（d），类似于10（-7）M（aS（TM））yr（-1）。使用低分辨率光谱仪，我们在1995-2013年对Lambda 4340-7130范围内的V1016 Cyg进行了绝对分光光度法。我们已经表明，λ和λ4400处线和连续体中的几乎所有绝对通量都在2000年后单调减少，而[O III]，[Fe VII]和[Ca VII]线的相对强度在可能发生的最小值之后增加。 1990年代。拉曼O VIλ6825线的通量显着下降（从1995年到2013年大约减少了10倍），反映出该线形成区条件的变化是由于吸收了一些O VIλ1032光子。冷却部件新形成的防尘套。

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