2026-05-15T16:02:02Z https://api.figshare.com/v2/oai
oai:figshare.com:article/17082317 2021-12-07T15:28:01Z category_30091 category_30106 category_30259 category_30265 category_30109 portal_549 item_type_2 month_year_12_2021
10.5522/04/17082317.v1 https://figshare.com/articles/media/Fine_Scale_Structure_in_Cometary_Dust_Tails_-_Figure_6_14_-_Localised_high_density_region_model_as_seen_by_SOHO_LASCO_C3_with_difference_enhancement_/17082317 https://ndownloader.figshare.com/files/31585088 Price, Oliver Oliver Price Jones, Geraint Geraint Jones <![CDATA[Fine Scale Structure in Cometary Dust Tails - Figure 6.14 - Localised high density region model (as seen by SOHO LASCO C3 with difference enhancement)]]> Astronomical instrumentation Planetary science (excl. solar system and planetary geology) Solar system planetary science (excl. planetary geology) Space sciences not elsewhere classified Solar physics Comet Dust Tail Finson Probstein Solar Wind Plasma NEAT C/2002 V1 CME Filament Instrumentation, Techniques, and Astronomical Observations Planetary Science Planetary Science (excl. Extraterrestrial Geology) Solar System, Solar Physics, Planets and Exoplanets Space Science Space and Solar Physics 2021-12-07 2021-12-07 Media 2021 University College London
The field of view of the instrument has been projected into the orbital plane of the comet, where it is shown in an unravelled radial plot.

A local region of the CME has been modelled as an area of high density, highlighted in green. This location corresponds with the part of the dust tail where the bright stria forms.
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