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LIBRIS Formathandbok  (Information om MARC21)
FältnamnIndikatorerMetadata
00005365naa a2200493 4500
001oai:DiVA.org:uu-358206
003SwePub
008180831s2018 | |||||||||||000 ||eng|
0247 a https://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-3582062 URI
0247 a https://doi.org/10.1029/2018JA0251832 DOI
040 a (SwePub)uu
041 a engb eng
042 9 SwePub
072 7a ref2 swepub-contenttype
072 7a art2 swepub-publicationtype
1001 a Ling, Yimingu Shandong Univ, Sch Space Sci & Phys, Shandong Prov Key Lab Opt Astron & Solar Terr Env, Weihai, Peoples R China;Chinese Acad Sci, NSSC, State Key Lab Space Weather, Beijing, Peoples R China;Univ Sci & Technol China, Sch Earth & Space Sci, CAS Key Lab Geospace Environm, Hefei, Anhui, Peoples R China4 aut
2451 0a Observations of Kelvin-Helmholtz Waves in the Earth's Magnetotail Near the Lunar Orbit
264 1c 2018
338 a electronic2 rdacarrier
520 a Kelvin‐Helmholtz waves (KHWs), which have been widely observed at the magnetopause in the region near the Earth, play an essential role in the transport of solar wind plasma and energy into the magnetosphere under dominantly northward interplanetary magnetic field (IMF) conditions. In this study, we present simultaneous observations of KHWs under the northward IMF observed by both the Acceleration, Reconnection, Turbulence, and Electrodynamics of Moon's Interaction with the Sun (ARTEMIS) spacecraft in the Earth's magnetotail around the lunar orbit (at X ~ −50RE, Y ~ 30RE, dusk side) and the Geotail in the near‐Earth space (at X ~ −5RE, Y ~ −10RE, dawn side). The KHWs are quantitatively characterized by their dominant period, phase velocity, and wavelength, utilizing wavelet analysis and an approximation of their center‐of‐mass velocity. Our results suggest that the phase velocity and spatial scale of KHWs may increase as they propagate along the boundary layer toward the tail. Alternatively, the differences between the ARTEMIS and Geotail observations may indicate the possibility of dawn‐dusk asymmetry in the excited KHWs in this study. Our results strongly evidence the existence of the development of KHWs in terms of their wave frequency and scale size in the magnetotail and provide insight to the time evolution of KHWs along the magnetopause.
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
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
7001 a Shi, Quanqiu Shandong Univ, Sch Space Sci & Phys, Shandong Prov Key Lab Opt Astron & Solar Terr Env, Weihai, Peoples R China4 aut
7001 a Shen, Xiao-Chenu Shandong Univ, Sch Space Sci & Phys, Shandong Prov Key Lab Opt Astron & Solar Terr Env, Weihai, Peoples R China4 aut
7001 a Tian, Anminu Shandong Univ, Sch Space Sci & Phys, Shandong Prov Key Lab Opt Astron & Solar Terr Env, Weihai, Peoples R China4 aut
7001 a Li, Wenyau Uppsala universitet,Institutet för rymdfysik, Uppsalaavdelningen,Chinese Acad Sci, NSSC, State Key Lab Space Weather, Beijing, Peoples R China4 aut0 (Swepub:uu)wenli806
7001 a Tang, Binbinu Chinese Acad Sci, NSSC, State Key Lab Space Weather, Beijing, Peoples R China4 aut
7001 a Degeling, A. W.u Shandong Univ, Sch Space Sci & Phys, Shandong Prov Key Lab Opt Astron & Solar Terr Env, Weihai, Peoples R China4 aut
7001 a Hasegawa, Hiroshiu Japan Aerosp Explorat Agcy JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa, Japan4 aut
7001 a Nowada, Motoharuu Shandong Univ, Sch Space Sci & Phys, Shandong Prov Key Lab Opt Astron & Solar Terr Env, Weihai, Peoples R China4 aut
7001 a Zhang, Huiu Univ Alaska, Geophys Inst, Fairbanks, AK 99701 USA4 aut
7001 a Rae, I. J.u Univ Coll London, Mullard Space Sci Lab, Dorking, Surrey, England4 aut
7001 a Zong, Qiu-Gangu Peking Univ, Sch Earth & Space Sci, Beijing, Peoples R China4 aut
7001 a Fu, Suiyanu Peking Univ, Sch Earth & Space Sci, Beijing, Peoples R China4 aut
7001 a Fazakerley, A. N.u Univ Coll London, Mullard Space Sci Lab, Dorking, Surrey, England4 aut
7001 a Pu, Zuyinu Peking Univ, Sch Earth & Space Sci, Beijing, Peoples R China4 aut
7102 a Shandong Univ, Sch Space Sci & Phys, Shandong Prov Key Lab Opt Astron & Solar Terr Env, Weihai, Peoples R China;Chinese Acad Sci, NSSC, State Key Lab Space Weather, Beijing, Peoples R China;Univ Sci & Technol China, Sch Earth & Space Sci, CAS Key Lab Geospace Environm, Hefei, Anhui, Peoples R Chinab Shandong Univ, Sch Space Sci & Phys, Shandong Prov Key Lab Opt Astron & Solar Terr Env, Weihai, Peoples R China4 org
7730 t Journal of Geophysical Research - Space Physicsg 123:5, s. 3836-3847q 123:5<3836-3847x 2169-9380x 2169-9402
8564 u https://doi.org/10.1029/2018JA025183y Fulltext
8564 u https://uu.diva-portal.org/smash/get/diva2:1244316/FULLTEXT01.pdfx primaryx Raw objecty fulltext:print
8564 8u https://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-358206
8564 8u https://doi.org/10.1029/2018JA025183

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