期刊
ASTRONOMICAL JOURNAL
卷 162, 期 4, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.3847/1538-3881/abfcbd
关键词
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资金
- National Aeronautics and Space Administration (NASA) [NNH14CK55B]
- NASA Planetary Astronomy/Solar System Observations Program [NNX12AG24G, 15-SSO15_2-0028, 18-SSO18_2-0040, 80NSSC17K0705]
- NASA Solar System Workings Program [NNX17AC86G]
- NASA Emerging Worlds Program [80NSSC20K0341]
- NASA Astrobiology Institute [13-13NAI7_2_0032]
- National Science Foundation [AST-2009398, AST-2009910, AST-1616306, AST-1615441]
- NASA Headquarters under the NASA Earth and Space Science Fellowship Program [NNX16AP49H]
- NASA [1003637, NNX17AC86G, NNX12AG24G, 75639] Funding Source: Federal RePORTER
Using the iSHELL spectrograph, researchers characterized the volatile composition and spatial distribution of Comet C/2015 ER61, finding variability in production rates and mixing ratios during pre- and post-perihelion observations. The relative abundances remained consistent before perihelion but tended to decrease afterwards, possibly due to seasonal effects in the comet.
Comet C/2015 ER61 (PanSTARRS) is a long-period Oort cloud comet whose favorable approach to the inner parts of the solar system in 2017 April-May enabled us to characterize its primary volatile composition using the iSHELL spectrograph mounted on the 3 m NASA Infrared Telescope Facility (IRTF) on Maunakea, Hawaii. We used three iSHELL settings (covering similar to 2.8-5.2 mu m) to sample fluorescent emissions from H2O, OH, CH3OH, HCN, C-2 H-2, NH3, CO, CH4, C-2 H-6, H2CO, and OCS on multiple dates ranging from UT 2017 April 15 (shortly after its April 4 outburst) to May 13, nearly 30 days before the detection of its double nucleus. Our observations also offered the opportunity to obtain sensitive 3 sigma upper limits for cyanoacetylene (HC3N). We report rotational temperatures (T-rot), production rates (Qs), abundance (mixing) ratios (relative to H2O and C-2 H-6), and spatial distributions in the coma. ER61 exhibits variability in production rates of many species on short (day-to-day) and long (pre- versus post-perihelion) timescales. The relative abundances of these volatile species remained consistent within uncertainties during our pre-perihelion observations but tended to decrease during our post-perihelion observations (with the exception of CH3OH and HCN). The short-timescale variability in the production rates of these volatiles could be due to diurnal effects (over the course of the rotation of the nucleus) and/or the effect of its outburst. The decrease in the production rates and hence the mixing ratios in some volatiles in post-perihelion dates could be due to the presence of seasonal effects in ER61.
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