Ground-based monitoring of comet 67P/Churyumov-Gerasimenko gas activity throughout the Rosetta mission

被引：14

作者：

Opitom, C. ^{[1
]}

Snodgrass, C. ^{[2
]}

Fitzsimmons, A. ^{[3
]}

Jehin, E. ^{[4
]}

Manfroid, J. ^{[4
]}

Tozzi, G. P. ^{[5
]}

Faggi, S. ^{[5
]}

Gillon, M. ^{[4
]}

机构：

[1] European Southern Observ, Avda Alonso de Cordova 3107 Vitacura, Santiago, Chile

[2] Open Univ, Sch Phys Sci, Milton Keynes MK7 6AA, Bucks, England

[3] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland

[4] Univ Liege, Space Sci Technol & Astrophys Res STAR Inst, Allee 6 Aout 17, B-4000 Liege, Belgium

[5] Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2017年 / 469卷

关键词：

comets:; individual:; 67P/Churyumov-Gerasimenko; NARROW-BAND PHOTOMETRY;

D O I：

10.1093/mnras/stx1591

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Simultaneously to the ESA Rosetta mission, a world-wide ground-based campaign provided measurements of the large scale activity of comet 67P/Churyumov-Gerasimenko through measurement of optically active gas species and imaging of the overall dust coma. We present more than 2 yr of observations performed with the FORS2 low-resolution spectrograph at the VLT, TRAPPIST and ACAM at the WHT. We focus on the evolution of the CN production as a tracer of the comet activity. We find that it is asymmetric with respect to perihelion and different from that of the dust. The CN emission is detected for the first time at 1.34 au pre-perihelion and production rates then increase steeply to peak about 2 weeks after perihelion at (1.00 +/- 0.10) x 10(25) molecules s(-1), while the post-perihelion decrease is more shallow. The evolution of the comet activity is strongly influenced by seasonal effects with enhanced CN production when the Southern hemisphere is illuminated.

引用

页码：S222 / S229

页数：8

共 32 条

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MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2016, 460 (04) :4268-4276

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MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2016, 462 :S184-S194

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