Submillimeter-wave Survey of the Interaction of Supernova

超新星相互作用的亚毫米波勘测

基本信息

  • 批准号:
    11440067
  • 负责人:
  • 金额:
    $ 6.4万
  • 依托单位:
  • 依托单位国家:
    日本
  • 项目类别:
    Grant-in-Aid for Scientific Research (B)
  • 财政年份:
    1999
  • 资助国家:
    日本
  • 起止时间:
    1999 至 2001
  • 项目状态:
    已结题

项目摘要

We have made the survey of the interaction of supernova remnants with molecular clouds throughsubmillimeter-wave observations. By observing submillimeter 345-GHz carbon monoxicide (CO) and millimeter 115-GHz CO lines of rotational transitions, we have successfully obtained the evidence of the interaction observationally. For the supernova remnant W28, we detected the narrow-line velocity component dominant in the millimeter line and the broad velocity component dominant in the submillimeter line. The former represents the unshocked gas, and the latter represents the shock-accelerated gas. Such examples of the convincing evidence have been obtained so far in only three supernova remnants, and very important for research. By comparing with excitation calculations, we derived the physical parameters of the unshockd an shocked gas. By comparing the spatial distribution of them precisely, the unshocked gas is distributed 0.4-1.0 pc outer than the shocked gas with respect to the remnant center. This is the first observational example of the detailed structure of the shock front of the interaction zone of the supernova remnant and the molecular cloud. Furthermore, by using the Mt. Fuji Submillimeter-Wave Telescope, we have made a survey of the interaction in 345-GHz CO line and 492-GHz atomic carbon (CI) line. In three remnants, we have obtained observational results showing that the CI/CO intensity ratio tends to be high in the shocked gas. In W52SNR, we observed optically thinner 13CO line, and confirmed that larger intensity ratio represents larger abundance ratio. Such abundance enhancement has been reported in one supernova remnant 1C 443 previously, and our results provide very essential information of the interaction chemistry. We have developed a sensitive submillimeter receiver system for the survey of the interaction. It employs low-power-consumption (ikW) cryocooler. Its cryogenics performance has been confirmed as good as thatin the low-altitude laboratory.
我们用亚毫米波观测研究了超新星遗迹与分子云的相互作用。通过对亚毫米波345-GHz一氧化碳(CO)和毫米波115-GHz CO转动跃迁谱线的观测,我们成功地从观测上获得了相互作用的证据。对于超新星遗迹W28,我们检测到的窄线速度分量占主导地位的毫米线和广泛的速度分量占主导地位的亚毫米线。前者代表未受冲击的气体,后者代表受冲击加速的气体。这样的例子令人信服的证据迄今为止只在三个超新星遗迹中获得过,而且对研究非常重要。通过与激发计算的比较,我们导出了未激波和激波气体的物理参数。通过对它们空间分布的精确比较,发现未冲击气体比冲击气体在残余中心外的位置要远0.4- 1.0pc。这是第一次观测到超新星遗迹和分子云相互作用区的冲击波阵面的详细结构。此外,通过使用Mt。利用富士亚毫米波望远镜,我们对345-GHz CO谱线和492-GHz碳原子谱线的相互作用进行了测量。在三个残留物中,我们已经获得的观测结果表明,CI/CO强度比往往是高的冲击气体。在W52 SNR中,我们观察到光学上较细的13 CO线,并证实较大的强度比代表较大的丰度比。这种丰度的增加在超新星遗迹1C 443中已有报道,我们的结果提供了非常重要的相互作用化学信息。我们研制了一种灵敏的亚毫米波接收系统,用于测量这种相互作用。它采用低功耗(kW)制冷机。其低温性能已在低空实验室中得到证实。

项目成果

期刊论文数量(56)
专著数量(0)
科研奖励数量(0)
会议论文数量(0)
专利数量(0)
Y. Sekimoto et al: "Hard X-Ray Emission from Giant Molecular Cloud Cores in NGC 6334"Publ. Astron. Soc. Japan. 52. L31-L35 and Plate 45 (2000)
Y. Sekimoto 等人:“NGC 6334 中巨型分子云核心的硬 X 射线发射”Publ。
  • DOI:
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    0
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Yamamoto et al.: "Observation of the CI 3P_2 -3P_1 Line Toward the Orion Kleinmam-Low Region"Astrophys.J.. 547. L165-L169 (2001)
Yamamoto 等人:“对猎户座 Kleinmam-Low 区域的 CI 3P_2 -3P_1 线的观测”Astrophys.J.. 547. L165-L169 (2001)
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    0
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  • 通讯作者:
Y.Arikawa et al.: "Shocked Molecular Gas Associated with the Supernova Remnant W28"Publ. Astron. Soc. Japan. 51. L9-L10 (1999)
Y.Arikawa 等人:“与超新星遗迹 W28 相关的冲击分子气体”Publ。
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    0
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K.Tatematsu: "Atomic Carbon Is a Temperature Probe in Dark Clouds"Astrophys. J.. 524. 295-306 (1999)
K.Tatematsu:“原子碳是乌云中的温度探测器”天体物理学。
  • DOI:
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  • 影响因子:
    0
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  • 通讯作者:
Y. Arikawa: "Shocked Molecular Gas Associated with the Supernova Remnant W28"Publ. Astron. Soc. Japan. 51. L7-L10 (1999)
Y. Arikawa:“与超新星遗迹 W28 相关的冲击分子气体”Publ。
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