2026-05-14T06:56:51Z https://api.figshare.com/v2/oai
oai:figshare.com:article/17082155 2021-12-07T15:25:05Z category_30091 category_30106 category_30259 category_30265 category_30109 portal_549 item_type_2 month_year_12_2021
10.5522/04/17082155.v1 https://figshare.com/articles/media/Fine_Scale_Structure_in_Cometary_Dust_Tails_-_Figure_5_23_-_Solar_Wind_adjusted_temporal_maps_of_McNaught_as_seen_by_HI-1A_with_MGN_enhancement/17082155 https://ndownloader.figshare.com/files/31584902 Price, Oliver Oliver Price Jones, Geraint Geraint Jones <![CDATA[Fine Scale Structure in Cometary Dust Tails - Figure 5.23 - Solar Wind adjusted temporal maps of McNaught as seen by HI-1A with MGN 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 HCS McNaught C/2006 P1 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 x-axis corresponds to the paths through the comet tail taken by solar wind features of the annotated speed. For a given solar wind speed, if all new combed features are at least vertical or slope diagonally to the top right, they are compatible with a potential formation from a solar wind structure moving at that particular speed.

Solar wind speeds of 500 km s-1 and above are compatible with the orientation of the combed features that form in McNaught's dust tail.

Note that features on the far left of the temporal maps are artefacts from the overexposed region near the comet's nucleus.
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