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LIBRIS Formathandbok  (Information om MARC21)
FältnamnIndikatorerMetadata
00006613naa a2200577 4500
001oai:DiVA.org:kth-219469
003SwePub
008171206s2017 | |||||||||||000 ||eng|
009oai:DiVA.org:uu-340160
0247 a https://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-2194692 URI
0247 a https://doi.org/10.1002/2017JA0245532 DOI
0247 a https://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-3401602 URI
040 a (SwePub)kthd (SwePub)uu
041 a engb eng
042 9 SwePub
072 7a ref2 swepub-contenttype
072 7a art2 swepub-publicationtype
1001 a Toledo-Redondo, Sergiou ESA ESAC, European Space Agcy, Madrid, Spain.4 aut
2451 0a Energy budget and mechanisms of cold ion heating in asymmetric magnetic reconnection
264 1b American Geophysical Union (AGU),c 2017
338 a print2 rdacarrier
500 a QC 20171206
520 a Cold ions (few tens of eV) of ionospheric origin are commonly observed on the magnetospheric side of the Earth's dayside magnetopause. As a result, they can participate in magnetic reconnection, changing locally the reconnection rate and being accelerated and heated. We present four events where cold ion heating was observed by the Magnetospheric Multiscale mission, associated with the magnetospheric Hall E field region of magnetic reconnection. For two of the events the cold ion density was small compared to the magnetosheath density, and the cold ions were heated roughly to the same temperature as magnetosheath ions inside the exhaust. On the other hand, for the other two events the cold ion density was comparable to the magnetosheath density and the cold ion heating observed was significantly smaller. Magnetic reconnection converts magnetic energy into particle energy, and ion heating is known to dominate the energy partition. We find that at least 10-25% of the energy spent by reconnection into ion heating went into magnetospheric cold ion heating. The total energy budget for cold ions may be even higher when properly accounting for the heavier species, namely helium and oxygen. Large E field fluctuations are observed in this cold ion heating region, i.e., gradients and waves, that are likely the source of particle energization. Plain Language Summary The magnetic field of Earth creates a natural shield that isolates and protects us from the particles and fields coming from our star, the Sun. This natural shield is called the magnetosphere and is filled by plasma. The particles coming from the Sun form another plasma called the solar wind and are usually deviated around the magnetosphere. However, under certain circumstances these two plasmas can reconnect (magnetic reconnection), and part of the energy and mass of the two plasmas is interchanged. Magnetic reconnection is the driver of storms and substorms inside the magnetosphere. In this work, we investigate what occurs to particles of very low energy (cold ions) of ionospheric origin when they reach the reconnecting boundary of the magnetosphere. It is found that they are energized and take an important part of the energy spent in reconnecting the plasmas. The plasma boundary develops spatial structures and emits waves that are able to heat the cold ions. Once heated, these cold ions irreversibly will escape the Earth's magnetosphere to never come back to Earth.
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 Geovetenskap och miljövetenskapx Geofysik0 (SwePub)105052 hsv//swe
650 7a NATURAL SCIENCESx Earth and Related Environmental Sciencesx Geophysics0 (SwePub)105052 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
7001 a André, Matsu Uppsala universitet,Institutet för rymdfysik, Uppsalaavdelningen4 aut0 (Swepub:uu)maand125
7001 a Khotyaintsev, Yuri V.u Uppsala universitet,Institutet för rymdfysik, Uppsalaavdelningen,Swedish Inst Space Phys, Uppsala, Sweden.4 aut0 (Swepub:uu)ykh28990
7001 a Lavraud, Benoitu Univ Toulouse, CNRS, Inst Rech Astrophys & Planetol, UPS, Toulouse, France.4 aut
7001 a Vaivads, Andrisu Uppsala universitet,Institutet för rymdfysik, Uppsalaavdelningen4 aut0 (Swepub:uu)anvai517
7001 a Graham, Daniel B.u Uppsala universitet,Institutet för rymdfysik, Uppsalaavdelningen4 aut0 (Swepub:uu)dangr618
7001 a Li, Wenyau Uppsala universitet,Institutet för rymdfysik, Uppsalaavdelningen4 aut0 (Swepub:uu)wenli806
7001 a Perrone, Deniseu ESA ESAC, European Space Agcy, Madrid, Spain.4 aut
7001 a Fuselier, Stephenu Southwest Res Inst, San Antonio, TX USA.;Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX USA.4 aut
7001 a Gershman, Daniel J.u NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.4 aut
7001 a Aunai, Nicolasu Univ Paris Sud, UPMC Univ Paris 06, Lab Phys Plasmas, Ecole Polytech,CNRS,UMR7648,Observ Paris, Paris, France.4 aut
7001 a Dargent, Jeremyu Univ Toulouse, CNRS, Inst Rech Astrophys & Planetol, UPS, Toulouse, France.;Univ Paris Sud, UPMC Univ Paris 06, Lab Phys Plasmas, Ecole Polytech,CNRS,UMR7648,Observ Paris, Paris, France.4 aut
7001 a Giles, Barbarau NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.4 aut
7001 a Le Contel, Olivieru Univ Paris Sud, UPMC Univ Paris 06, Lab Phys Plasmas, Ecole Polytech,CNRS,UMR7648,Observ Paris, Paris, France.4 aut
7001 a Lindqvist, Per-Arneu KTH,Rymd- och plasmafysik,Royal Inst Technol, Stockholm, Sweden.4 aut0 (Swepub:kth)u1yukyk9
7001 a Ergun, Robert E.u Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.4 aut
7001 a Russell, Christopher T.u Univ Calif Los Angeles, Earth Planetary & Space Sci, Los Angeles, CA USA.4 aut
7001 a Burch, James L.u Southwest Res Inst, San Antonio, TX USA.4 aut
7102 a ESA ESAC, European Space Agcy, Madrid, Spain.b Institutet för rymdfysik, Uppsalaavdelningen4 org
7730 t Journal of Geophysical Research - Space Physicsd : American Geophysical Union (AGU)g 122:9, s. 9396-9413q 122:9<9396-9413x 2169-9380x 2169-9402
8564 8u https://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-219469
8564 8u https://doi.org/10.1002/2017JA024553
8564 8u https://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-340160

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