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FältnamnIndikatorerMetadata
00006651naa a2200493 4500
001oai:DiVA.org:uu-525518
003SwePub
008240325s2024 | |||||||||||000 ||eng|
009oai:DiVA.org:umu-220870
0247 a https://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-5255182 URI
0247 a https://doi.org/10.1051/0004-6361/2023465662 DOI
0247 a https://urn.kb.se/resolve?urn=urn:nbn:se:umu:diva-2208702 URI
040 a (SwePub)uud (SwePub)umu
041 a engb eng
042 9 SwePub
072 7a ref2 swepub-contenttype
072 7a art2 swepub-publicationtype
1001 a Edberg, Niklas J. T.u Uppsala universitet,Institutet för rymdfysik, Uppsalaavdelningen,Swedish Institute of Space Physics (IRF), Uppsala, Sweden4 aut0 (Swepub:uu)niked861
2451 0a Scale size of cometary bow shocks
264 1b EDP Sciences,c 2024
338 a electronic2 rdacarrier
520 a Context. In past decades, several spacecraft have visited comets to investigate their plasma environments. In the coming years, Comet Interceptor will make yet another attempt. This time, the target comet and its outgassing activity are unknown and may not be known before the spacecraft has been launched into its parking orbit, where it will await a possible interception. If the approximate outgassing rate can be estimated remotely when a target has been identified, it is desirable to also be able to estimate the scale size of the plasma environment, defined here as the region bound by the bow shock.Aims. This study aims to combine previous measurements and simulations of cometary bow shock locations to gain a better understanding of how the scale size of cometary plasma environments varies. We compare these data with models of the bow shock size, and we furthermore provide an outgassing rate-dependent shape model of the bow shock. We then use this to predict a range of times and cometocentric distances for the crossing of the bow shock by Comet Interceptor, together with expected plasma density measurements along the spacecraft track.Methods. We used data of the location of cometary bow shocks from previous spacecraft missions, together with simulation results from previously published studies. We compared these results with an existing model of the bow shock stand-off distance and expand on this to provide a shape model of cometary bow shocks. The model in particular includes the cometary outgassing rate, but also upstream solar wind conditions, ionisation rates, and the neutral flow velocity.Results. The agreement between the gas-dynamic model and the data and simulation results is good in terms of the stand-off distance of the bow shock as a function of the outgassing rate. For outgassing rates in the range of 1027–1031–s-1, the scale size of cometary bow shocks can vary by four orders of magnitude, from about 102 km to 106 km, for an ionisation rate, flow velocity, and upstream solar wind conditions typical of those at 1 AU. The proposed bow shock shape model shows that a comet plasma environment can range in scale size from the plasma environment of Mars to about half of that of Saturn.Conclusions. The model-data agreement allows for the planning of upcoming spacecraft comet encounters, such as that of Comet Interceptor, when a target has been identified and its outgassing rate is determined. We conclude that the time a spacecraft can spend within the plasma environment during a flyby can range from minutes to days, depending on the comet that is visited and on the flyby speed. However, to capture most of the comet plasma environment, including pick-up ions and upstream plasma waves, and to ensure the highest possible scientific return, measurements should still start well upstream of the expected bow shock location. From the plasma perspective, the selected target should preferably be an active comet with the lowest possible flyby velocity.
650 7a NATURVETENSKAPx Fysikx Fusion, plasma och rymdfysik0 (SwePub)103032 hsv//swe
650 7a NATURAL SCIENCESx Physical Sciencesx Fusion, Plasma and Space Physics0 (SwePub)103032 hsv//eng
650 7a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe
650 7a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng
653 a comets: general
653 a plasmas
7001 a Eriksson, Anders I.u Uppsala universitet,Institutet för rymdfysik, Uppsalaavdelningen,Swedish Institute of Space Physics (IRF), Uppsala, Sweden4 aut0 (Swepub:uu)andeerik
7001 a Vigren, Eriku Uppsala universitet,Institutet för rymdfysik, Uppsalaavdelningen,Swedish Institute of Space Physics (IRF), Uppsala, Sweden4 aut0 (Swepub:uu)erivi300
7001 a Nilsson, H.u Swedish Inst Space Phys IRF, Kiruna, Sweden.,Swedish Institute of Space Physics (IRF), Kiruna, Sweden4 aut
7001 a Gunell, Herbertu Umeå universitet,Institutionen för fysik,Umeå Univ, Dept Phys, Umeå, Sweden.4 aut0 (Swepub:umu)hegu0051
7001 a Götz, C.u Northumbria Univ, Dept Math Phys & Elect Engn, Newcastle Upon Tyne, England.,Department of Mathematics, Physics and Electrical Engineering, Northumbria University, Newcastle-upon-Tyne, United Kingdom4 aut
7001 a Richter, I.u Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, Braunschweig, Germany.,Institut fur Geophysik und Extraterrestrische Physik, Technische Universität Braunschweig, Braunschweig, Germany4 aut
7001 a Henri, P.u CNRS, Lab Phys & Chim Environm & Espace, F-45071 Orleans, France.;Lab Lagrange, OCA, CNRS, UCA, F-06304 Nice, France.,Laboratoire de Physique et Chimie de l'Environnement et de l'Espace, Cnrs, Orléans, France; Laboratoire Lagrange, Oca, Cnrs, Uca, Nice, France4 aut
7001 a De Keyser, J.u Royal Belgian Inst Space Aeron, BIRA IASB, Brussels, Belgium.,Royal Belgian Institute for Space Aeronomy, BIRA-IASB, Brussels, Belgium4 aut
7102 a Uppsala universitetb Institutet för rymdfysik, Uppsalaavdelningen4 org
7730 t Astronomy and Astrophysicsd : EDP Sciencesg 682q 682x 0004-6361x 1432-0746
8564 u https://doi.org/10.1051/0004-6361/202346566y Fulltext
8564 u https://uu.diva-portal.org/smash/get/diva2:1846851/FULLTEXT01.pdfx primaryx Raw objecty fulltext:print
8564 u https://umu.diva-portal.org/smash/get/diva2:1838764/FULLTEXT01.pdfx primaryx Raw objecty fulltext:print
8564 8u https://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-525518
8564 8u https://doi.org/10.1051/0004-6361/202346566
8564 8u https://urn.kb.se/resolve?urn=urn:nbn:se:umu:diva-220870

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