• 主题
高级搜索  >
历史搜索 清空历史
首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >Optical and Near-Infrared Photometric Observation during the Superoutburst of the WZ Sge-Type Dwarf Nova, V455 Andromedae
【24h】

Optical and Near-Infrared Photometric Observation during the Superoutburst of the WZ Sge-Type Dwarf Nova, V455 Andromedae

机译：WZ Sge型矮新星V455 Andromedae超爆发期间的光学和近红外测光观察。

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 report on optical and infrared photometric observations of a WZ Sge-type dwarf nova, V455 And during a superoutburst in 2007. These observations were performed with the KANATA (V, J, and K_sbands) and MITSuME (g', R_C, and I_C bands) telescopes. Our 6-band simultaneous observations allowed us to investigate the temporal variation of the temperature and the size of the emitting region associated with the superoutburst and short-term modulations, such as early and ordinary superhumps. A hot (> 11000 K) accretion disk suddenly disappeared when the superoutburst finished, while blackbody emission, probably from the disk, still remained dominant in the optical region with a moderately high temperature ( ～ 8000 K). This indicates that a substantial amount of gas was stored in the disk even after the outburst. This remnant matter may be a sign of an expected mass-reservoir, which can trigger echo outbursts observed in several WZ Sge stars. The color variation associated with superhumps indicates that viscous heating in a superhump source stopped on the way to the superhump maximum, and a subsequent expansion of a low-temperature region made the maximum. The color variation of early superhumps was totally different from that of superhumps: the object was bluest at the early superhump minimum. The temperature of the early superhump light source was lower than that of an underlying component, indicating that the early superhump light source was a vertically expanded low-temperature region at the outermost part of the disk.
机译：我们报告了WZ Sge型矮新星V455的光学和红外光度观测，并于2007年爆发了一次。这些观测是使用KANATA（V，J和K_sbands）和MITSuME（g'，R_C和I_C）进行的波段）望远镜。我们的6波段同时观测使我们能够研究温度的时间变化以及与超爆发和短期调制（例如早期和普通的超级驼峰）相关的发射区域的大小。当超爆发结束时，一个热的（> 11000 K）吸积盘突然消失，而黑体的发射（可能来自该盘）仍然在中等温度（〜8000 K）的光学区域中占主导地位。这表明即使在爆发后，仍在盘中存储了大量的气体。这种残留的物质可能表明存在一个预期的质量储层，它可能触发在几颗WZ Sge恒星中观测到的回波爆发。与超级峰相关的颜色变化表明，超级峰源中的粘性加热在达到最大峰的途中停止了，随后低温区域的扩展达到最大。早期超级峰的颜色变化与超级峰的颜色变化完全不同：对象在早期超级峰的最小值处最蓝。早期超级驼峰光源的温度低于其下层组件的温度，这表明早期超级驼峰光源是磁盘最外部垂直扩展的低温区域。

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