Optical low-dispersion spectroscopic observations of Comet 103P/Hartley 2 at Koyama Astronomical Observatory during the EPOXI flyby
Optical low-dispersion spectroscopic observations of Comet 103P/Hartley 2 at Koyama Astronomical Observatory during the EPOXI flyby
复制标题
EPOXI 飞越期间在小山天文台对彗星 103P/Hartley 2 进行光学低色散光谱观测
DOI：
10.1016/j.icarus.2012.08.001
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发表时间：
2013
期刊：
影响因子：
3.2
通讯作者：
Yuji
中科院分区：
文献类型：
--
作者：
Shinnaka;Yoshiharu; Kawakita;Hideyo; Kobayashi;Hitomi; Naka;Chiharu; Arai;Akira; Arasaki;Takayuki; Kitao;Eiji; Taguchi;Gaku; Ikeda;Yuji
我们于2010年11月4日利用安装在UT小山天文台1.3m-Araki望远镜上的LOSA/F2在光学波长上对103P/Hartley 2彗星进行了低色散光谱观测。期间，深度撞击航天器在EPOXI任务飞越中接近103P/Hartley 2彗星的核心。我们的观测揭示了在光学波长上的彗发的化学；包括CN，C3，C2和NH2，以及在6300ä的[OI]发射的H2O。这些自由基的合成混合比使彗星在化学成分上属于正常群。观测得到的H2O混合比与A‘Hain等人1991年对103P/Hartley 2彗星的分光光度观测结果基本一致。(A‘Hain，M.F.，Millis，R.L.，Schleicher，D.G.，Osip，D.J.，Birch，P.V.[1995]。Icarus 118,223-270)，Fink在1998年的光学光谱观测(Fink，U[2009])。伊卡洛斯201,311-334)，也与拉拉等人在2010年10月27日和29日在UT的观察一致。(Lara，L.M.，Lin，Z.-Y.，Meech，K.[2011]。阿斯特龙。占星术。532，A87)(但仅限于相对于CN的比率)。
We performed low-dispersion spectroscopic observations of Comet 103P/Hartley 2 in optical wavelengths using the LOSA/F2 mounted on the 1.3m-Araki telescope at Koyama Astronomical Observatory on UT 2010 November 4 during the close approach of the Deep Impact spacecraft to the nucleus of Comet 103P/Hartley 2 in the EPOXI mission flyby. Our observations have revealed the chemistry of the coma at optical wavelengths; including CN, C3, C2and NH2along with H2O from [OI] emission at 6300Å. Resultant mixing ratios of these radicals put the comet into the normal group in chemical composition. The mixing ratios with respect to H2O obtained in our observations are basically consistent with the previous optical spectro-photometric observations of Comet 103P/Hartley 2 in 1991 by A’Hearn et al. (A’Hearn, M.F., Millis, R.L., Schleicher, D.G., Osip, D.J., Birch, P.V. [1995]. Icarus 118, 223–270), the optical spectroscopic observations in 1998 by Fink (Fink, U. [2009]. Icarus 201, 311–334) and also consistent with the observations on UT 2010 October 27 and 29 by Lara et al. (Lara, L.M., Lin, Z.-Y., Meech, K. [2011]. Astron. Astrophys. 532, A87) (but only for the ratio relative to CN).