Search: onr:"swepub:oai:DiVA.org:kth-347116" > Statistical Observa...
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000 | 06114naa a2200601 4500 | |
001 | oai:DiVA.org:kth-347116 | |
003 | SwePub | |
008 | 240603s2024 | |||||||||||000 ||eng| | |
024 | 7 | a https://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-3471162 URI |
024 | 7 | a https://doi.org/10.1029/2024JA0325162 DOI |
040 | a (SwePub)kth | |
041 | a engb eng | |
042 | 9 SwePub | |
072 | 7 | a ref2 swepub-contenttype |
072 | 7 | a art2 swepub-publicationtype |
100 | 1 | a Toledo-Redondo, S.u Department of Electromagnetism and Electronics, University of Murcia, Murcia, Spain; Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, CNRS, UPS, CNES, Toulouse, France4 aut |
245 | 1 0 | a Statistical Observations of Proton-Band Electromagnetic Ion Cyclotron Waves in the Outer Magnetosphere: Full Wavevector Determination |
264 | 1 | b John Wiley and Sons Inc,c 2024 |
338 | a print2 rdacarrier | |
500 | a QC 20240605 | |
520 | a Electromagnetic Ion Cyclotron (EMIC) waves mediate energy transfer from the solar wind to the magnetosphere, relativistic electron precipitation, or thermalization of the ring current population, to name a few. How these processes take place depends on the wave properties, such as the wavevector and polarization. However, inferring the wavevector from in-situ measurements is problematic since one needs to disentangle spatial and time variations. Using 8 years of Magnetospheric Multiscale (MMS) mission observations in the dayside magnetosphere, we present an algorithm to detect proton-band EMIC waves in the Earth's dayside magnetosphere, and find that they are present roughly 15% of the time. Their normalized frequency presents a dawn-dusk asymmetry, with waves in the dawn flank magnetosphere having larger frequency than in the dusk, subsolar, and dawn near subsolar region. It is shown that the observations are unstable to the ion cyclotron instability. We obtain the wave polarization and wavevector by comparing Single Value Decomposition and Ampere methods. We observe that for most waves the perpendicular wavenumber (k⊥) is larger than the inverse of the proton gyroradius (ρi), that is, k⊥ρi > 1, while the parallel wavenumber is smaller than the inverse of the ion gyroradius, that is, k‖ρi < 1. Left-hand polarized waves are associated with small wave normal angles (θBk < 30°), while linearly polarized waves are associated with large wave normal angles (θBk > 30°). This work constitutes, to our knowledge, the first attempt to statistically infer the full wavevector of proton-band EMIC waves observed in the outer magnetosphere. | |
650 | 7 | a NATURVETENSKAPx Fysikx Fusion, plasma och rymdfysik0 (SwePub)103032 hsv//swe |
650 | 7 | a NATURAL SCIENCESx Physical Sciencesx Fusion, Plasma and Space Physics0 (SwePub)103032 hsv//eng |
653 | a ion cylotron waves | |
653 | a magnetosphere | |
653 | a plasma waves | |
700 | 1 | a Lee, J. H.u The Aerospace Corporation, Los Angeles, CA, USA4 aut |
700 | 1 | a Vines, S. K.u Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA4 aut |
700 | 1 | a Albert, I. F.u Department of Electromagnetism and Electronics, University of Murcia, Murcia, Spain4 aut |
700 | 1 | a André, M.u IRF Swedish Institute of Space Physics, Uppsala, Sweden4 aut |
700 | 1 | a Castilla, A.u Department of Electromagnetism and Electronics, University of Murcia, Murcia, Spain4 aut |
700 | 1 | a Dargent, J. P.u Institut für Theoretische Physik, Ruhr-Universität Bochum, Bochum, Germany4 aut |
700 | 1 | a Fu, H. S.u School of Space and Environment, Beihang University, Beijing, China; Key Laboratory of Space Environment Monitoring and Information Processing, Ministry of Industry and Information Technology, Beijing, China4 aut |
700 | 1 | a Fuselier, S. A.u Southwest Research Institute, San Antonio, TX, USA; University of Texas at San Antonio, San Antonio, TX, USA4 aut |
700 | 1 | a Genot, V.u Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, CNRS, UPS, CNES, Toulouse, France4 aut |
700 | 1 | a Graham, D. B.u IRF Swedish Institute of Space Physics, Uppsala, Sweden4 aut |
700 | 1 | a Kitamura, N.u Institute for Space-Earth Environmental Research (ISEE), Nagoya University, Nagoya, Japan4 aut |
700 | 1 | a Khotyaintsev, Yu V.u IRF Swedish Institute of Space Physics, Uppsala, Sweden4 aut |
700 | 1 | a Lavraud, B.u Laboratoire d'Astrophysique deBordeaux, Bordeaux, France4 aut |
700 | 1 | a Montagud-Camps, V.u Department of Electromagnetism and Electronics, University of Murcia, Murcia, Spain4 aut |
700 | 1 | a Navarro, E. A.u IRTIC Institute/ETSE, Universitat de València, Avd. Universitat, Burjassot, Spain4 aut |
700 | 1 | a Norgren, C.u IRF Swedish Institute of Space Physics, Uppsala, Sweden4 aut |
700 | 1 | a Perrone, D.u ASI—Italian Space Agency, Via del Politecnico snc, Rome, Italy4 aut |
700 | 1 | a Phan, T. D.u SSL, University of California, Berkeley, CA, USA4 aut |
700 | 1 | a Portí, J.u Department of Applied Physics, University of Granada, Granada, Spain4 aut |
700 | 1 | a Salinas, A.u Department of Electromagnetism and Matter Physics, University of Granada, Granada, Spain4 aut |
700 | 1 | a Stawarz, J. E.u Department of Mathematics, Physics, and Electrical Engineering, Northumbria University, Newcastle upon Tyne, UK4 aut |
700 | 1 | a Vaivads, Andrisu KTH,Rymd- och plasmafysik,Ventspils University of Applied Sciences, Ventspils, Latvia4 aut0 (Swepub:kth)u167dmzs |
710 | 2 | a Department of Electromagnetism and Electronics, University of Murcia, Murcia, Spain; Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, CNRS, UPS, CNES, Toulouse, Franceb The Aerospace Corporation, Los Angeles, CA, USA4 org |
773 | 0 | t Journal of Geophysical Research - Space Physicsd : John Wiley and Sons Incg 129:5q 129:5x 2169-9380x 2169-9402 |
856 | 4 | u https://doi.org/10.1029/2024JA032516y Fulltext |
856 | 4 8 | u https://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-347116 |
856 | 4 8 | u https://doi.org/10.1029/2024JA032516 |
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