Ion and electron momentum flux observed by Rosetta

Creator/Principal investigator(s):

Hayley Williamson - Swedish Institute of Space Physics (IRF) orcid

Description:

Data from the Rosetta mission has been used to  study the momentum flux around comet 67P during the two years when the  Rosetta spacecraft followed the comet, between August 2014 and September 2016. During this period, the comet first approached the Sun and its atmosphere and ionosphere grew until perihelion was reached. Thereafter the comet move further away from the Sun, and its atmosphere and ionosphere shrunk again. We show how the solar wind affects the comet ionosphere and how its dynamic pressure interacts with the ionosphere of the comet. A significant pressure is built up, magnetic and electron pressure and the momentum flux of cometary ions all become important. Close to the comet the electron pressure dominate, corresponding to a region where an expanding ionosphere can push away the solar wind. Around perihelion a cavity in the solar wind formed, where no solar wind ions are present. There was still a magnetic field, as well as water ions of cometary origin, that had been picked up by the solar wind upstream, and been accelerated back towards the comet. In the solar wind ion cavity

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Responsible department/unit:

Swedish Institute of Space Physics, Solar System Physics and Space Technology

Creator/Principal investigator(s):

Hayley Williamson - Swedish Institute of Space Physics (IRF) orcid

Identifiers:

SND-ID: SND 1163

Description:

Data from the Rosetta mission has been used to  study the momentum flux around comet 67P during the two years when the  Rosetta spacecraft followed the comet, between August 2014 and September 2016. During this period, the comet first approached the Sun and its atmosphere and ionosphere grew until perihelion was reached. Thereafter the comet move further away from the Sun, and its atmosphere and ionosphere shrunk again. We show how the solar wind affects the comet ionosphere and how its dynamic pressure interacts with the ionosphere of the comet. A significant pressure is built up, magnetic and electron pressure and the momentum flux of cometary ions all become important. Close to the comet the electron pressure dominate, corresponding to a region where an expanding ionosphere can push away the solar wind. Around perihelion a cavity in the solar wind formed, where no solar wind ions are present. There was still a magnetic field, as well as water ions of cometary origin, that had been picked up by the solar wind upstream, and been accelerated back towards the comet. In the solar wind ion cavity

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Language:

English

Time period(s) investigated:

2014-08-01 — 2016-10-01

Contact for questions about the data:

Hayley Williamson

Download metadata:

Ion and electron momentum flux observed by Rosetta

Suggested citation:

Hayley Williamson. Swedish Institute of Space Physics, Solar System Physics and Space Technology (2020). Ion and electron momentum flux observed by Rosetta. Swedish National Data Service. Version 1. https://doi.org/10.5878/t0r1-2y39

Creator/Principal investigator(s):

Hayley Williamson - Swedish Institute of Space Physics (IRF) orcid

Description:

CSV table of the ion, electron, and magnetic pressure for the time period August 2014 to October 2016. Columns are: mission time, cometary ion x, y, and z components of momentum flux, solar wind ion x, y, and z components of momentum flux, electron pressure, and magnetic pressure. The cometary ion and solar wind ion data was calculated using data from the Rosetta Ion Composition Analyzer. Electron pressure data was calculated from Langmuir probe and Mutual Impedance Probe data. Magnetic pressure

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Data format / data structure:

Numeric

Data collection:

Time period(s) for data collection: 2014-08-01 — 2016-10-01

Time period(s) investigated:

2014-08-01 — 2016-10-01

Variables:

9

Published: 2020-06-30