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首页> 外文期刊>The Astrophysical Journal. Letters >Outgassing behavior of C/2012 S1 (ISON) from 2011 September to 2013 June
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Outgassing behavior of C/2012 S1 (ISON) from 2011 September to 2013 June

机译：2011年9月至2013年6月C / 2012 S1（ISON）的脱气行为

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摘要

We report photometric observations for comet C/2012 S1 (ISON) obtained during the time period immediately after discovery (r = 6.28 AU) until it moved into solar conjunction in mid-2013 June using the UH2.2 m, and Gemini North 8 m telescopes on Mauna Kea, the Lowell 1.8 m in Flagstaff, the Calar Alto 1.2 m telescope in Spain, the VYSOS-5 telescopes on Mauna Loa Hawaii and data from the CARA network. Additional pre-discovery data from the Pan STARRS1 survey extends the light curve back to 2011 September 30 (r = 9.4 AU). The images showed a similar tail morphology due to small micron sized particles throughout 2013. Observations at submillimeter wavelengths using the James Clerk Maxwell Telescope on 15 nights between 2013 March 9 (r = 4.52 AU) and June 16 (r = 3.35 AU) were used to search for CO and HCN rotation lines. No gas was detected, with upper limits for CO ranging between 3.5-4.5 × 10~(27) molecules s~(-1). Combined with published water production rate estimates we have generated ice sublimation models consistent with the photometric light curve. The inbound light curve is likely controlled by sublimation of CO_2. At these distances water is not a strong contributor to the outgassing. We also infer that there was a long slow outburst of activity beginning in late 2011 peaking in mid-2013 January (r ～ 5 AU) at which point the activity decreased again through 2013 June. We suggest that this outburst was driven by CO injecting large water ice grains into the coma. Observations as the comet came out of solar conjunction seem to confirm our models.
机译：我们报告在发现之后立即进行的彗星C / 2012 S1（ISON）的光度学观测（r = 6.28 AU），直到它在2013年6月中旬使用UH2.2 m和Gemini North 8 m进入太阳交会为止Mauna Kea上的望远镜，弗拉格斯塔夫的Lowell 1.8 m望远镜，西班牙的Calar Alto 1.2 m望远镜，夏威夷Mauna Loa的VYSOS-5望远镜以及CARA网络的数据。 Pan STARRS1调查的其他发现前数据将光曲线延长至2011年9月30日（r = 9.4 AU）。由于整个2013年都有小颗粒的微粒，图像显示出相似的尾部形态。使用James Clerk Maxwell望远镜在2013年3月9日（r = 4.52 AU）和6月16日（r = 3.35 AU）之间的亚毫米波长观察。搜索CO和HCN旋转线。未检测到气体，CO的上限范围为3.5-4.5×10〜（27）分子s〜（-1）。结合已公布的产水率估算值，我们生成了与光度学光曲线一致的冰升华模型。入光曲线很可能受CO_2升华的控制。在这样的距离下，水并不是除气的重要因素。我们还可以推断，从2011年底开始的活动爆发时间很长，在2013年1月中旬（r〜5 AU）达到顶峰，到2013年6月活动再次减少。我们认为这种爆发是由CO向昏迷中注入大量水冰粒驱动的。彗星从太阳联合中出来的观察似乎证实了我们的模型。

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