Energetic Electron Precipitation Driven by Electromagnetic Ion Cyclotron Waves from ELFIN’s Low Altitude Perspective

Abstract We review comprehensive observations of electromagnetic ion cyclotron (EMIC) wave-driven energetic electron precipitation using data collected by the energetic electron detector on the Electron Losses and Fields InvestigatioN (ELFIN) mission, two polar-orbiting low-altitude spinning CubeSats, measuring 50-5000 keV electrons with good pitch-angle and energy resolution. EMIC wave-driven precipitation exhibits a distinct signature in energy-spectrograms of the precipitating-to-trapped flux ratio: peaks at >0.5 MeV which are abrupt (bursty) (lasting ∼17 s, or $\Delta L\sim 0.56$) with significant substructure (occasionally down to sub-second timescale). We attribute the bursty nature of the precipitation to the spatial extent and structuredness of the wave field at the equator. Multiple ELFIN passes over the same MLT sector allow us to study the spatial and temporal evolution of the EMIC wave - electron interaction region. Case studies employing conjugate ground-based or equatorial observations of the EMIC waves reveal that the energy of moderate and strong precipitation at ELFIN approximately agrees with theoretical expectations for cyclotron resonant interactions in a cold plasma. Using multiple years of ELFIN data uniformly distributed in local time, we assemble a statistical database of ∼50 events of strong EMIC wave-driven precipitation. Most reside at $L\sim 5-7$ at dusk, while a smaller subset exists at $L\sim 8-12$ at post-midnight. The energies of the peak-precipitation ratio and of the half-peak precipitation ratio (our proxy for the minimum resonance energy) exhibit an $L$-shell dependence in good agreement with theoretical estimates based on prior statistical observations of EMIC wave power spectra. The precipitation ratio’s spectral shape for the most intense events has an exponential falloff away from the peak (i.e., on either side of $\sim 1.45$ MeV). It too agrees well with quasi-linear diffusion theory based on prior statistics of wave spectra. It should be noted though that this diffusive treatment likely includes effects from nonlinear resonant interactions (especially at high energies) and nonresonant effects from sharp wave packet edges (at low energies). Sub-MeV electron precipitation observed concurrently with strong EMIC wave-driven >1 MeV precipitation has a spectral shape that is consistent with efficient pitch-angle scattering down to ∼ 200-300 keV by much less intense higher frequency EMIC waves at dusk (where such waves are most frequent). At ∼100 keV, whistler-mode chorus may be implicated in concurrent precipitation. These results confirm the critical role of EMIC waves in driving relativistic electron losses. Nonlinear effects may abound and require further investigation. Ausführliche Beschreibung

Gespeichert in:

Autor*in:	Angelopoulos, V. [verfasserIn] Zhang, X.-J. Artemyev, A. V. Mourenas, D. Tsai, E. Wilkins, C. Runov, A. Liu, J. Turner, D. L. Li, W. Khurana, K. Wirz, R. E. Sergeev, V. A. Meng, X. Wu, J. Hartinger, M. D. Raita, T. Shen, Y. An, X. Shi, X. Bashir, M. F. Shen, X. Gan, L. Qin, M. Capannolo, L. Ma, Q. Russell, C. L. Masongsong, E. V. Caron, R. He, I. Iglesias, L. Jha, S. King, J. Kumar, S. Le, K. Mao, J. McDermott, A. Nguyen, K. Norris, A. Palla, A. Roosnovo, A. Tam, J. Xie, E. Yap, R. C. Ye, S. Young, C. Adair, L. A. Shaffer, C. Chung, M. Cruce, P. Lawson, M. Leneman, D. Allen, M. Anderson, M. Arreola-Zamora, M. Artinger, J. Asher, J. Branchevsky, D. Cliffe, M. Colton, K. Costello, C. Depe, D. Domae, B. W. Eldin, S. Fitzgibbon, L. Flemming, A. Frederick, D. M. Gilbert, A. Hesford, B. Krieger, R. Lian, K. McKinney, E. Miller, J. P. Pedersen, C. Qu, Z. Rozario, R. Rubly, M. Seaton, R. Subramanian, A. Sundin, S. R. Tan, A. Thomlinson, D. Turner, W. Wing, G. Wong, C. Zarifian, A.

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2023

Schlagwörter:	Relativistic electron precipitation Radiation belts Magnetosphere Electromagnetic ion cyclotron waves Whistler-mode chorus Plasma waves

Anmerkung:	© The Author(s) 2023

Übergeordnetes Werk:	Enthalten in: Space science reviews - Dordrecht [u.a.] : Springer Science + Business Media B.V, 1962, 219(2023), 5 vom: 11. Juli
Übergeordnetes Werk:	volume:219 ; year:2023 ; number:5 ; day:11 ; month:07

Links:	Volltext

DOI / URN:	10.1007/s11214-023-00984-w

Katalog-ID:	SPR052211800

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100	1		\|a Angelopoulos, V. \|e verfasserin \|0 (orcid)0000-0001-7024-1561 \|4 aut
245	1	0	\|a Energetic Electron Precipitation Driven by Electromagnetic Ion Cyclotron Waves from ELFIN’s Low Altitude Perspective
264		1	\|c 2023
336			\|a Text \|b txt \|2 rdacontent
337			\|a Computermedien \|b c \|2 rdamedia
338			\|a Online-Ressource \|b cr \|2 rdacarrier
500			\|a © The Author(s) 2023
520			\|a Abstract We review comprehensive observations of electromagnetic ion cyclotron (EMIC) wave-driven energetic electron precipitation using data collected by the energetic electron detector on the Electron Losses and Fields InvestigatioN (ELFIN) mission, two polar-orbiting low-altitude spinning CubeSats, measuring 50-5000 keV electrons with good pitch-angle and energy resolution. EMIC wave-driven precipitation exhibits a distinct signature in energy-spectrograms of the precipitating-to-trapped flux ratio: peaks at >0.5 MeV which are abrupt (bursty) (lasting ∼17 s, or $\Delta L\sim 0.56$) with significant substructure (occasionally down to sub-second timescale). We attribute the bursty nature of the precipitation to the spatial extent and structuredness of the wave field at the equator. Multiple ELFIN passes over the same MLT sector allow us to study the spatial and temporal evolution of the EMIC wave - electron interaction region. Case studies employing conjugate ground-based or equatorial observations of the EMIC waves reveal that the energy of moderate and strong precipitation at ELFIN approximately agrees with theoretical expectations for cyclotron resonant interactions in a cold plasma. Using multiple years of ELFIN data uniformly distributed in local time, we assemble a statistical database of ∼50 events of strong EMIC wave-driven precipitation. Most reside at $L\sim 5-7$ at dusk, while a smaller subset exists at $L\sim 8-12$ at post-midnight. The energies of the peak-precipitation ratio and of the half-peak precipitation ratio (our proxy for the minimum resonance energy) exhibit an $L$-shell dependence in good agreement with theoretical estimates based on prior statistical observations of EMIC wave power spectra. The precipitation ratio’s spectral shape for the most intense events has an exponential falloff away from the peak (i.e., on either side of $\sim 1.45$ MeV). It too agrees well with quasi-linear diffusion theory based on prior statistics of wave spectra. It should be noted though that this diffusive treatment likely includes effects from nonlinear resonant interactions (especially at high energies) and nonresonant effects from sharp wave packet edges (at low energies). Sub-MeV electron precipitation observed concurrently with strong EMIC wave-driven >1 MeV precipitation has a spectral shape that is consistent with efficient pitch-angle scattering down to ∼ 200-300 keV by much less intense higher frequency EMIC waves at dusk (where such waves are most frequent). At ∼100 keV, whistler-mode chorus may be implicated in concurrent precipitation. These results confirm the critical role of EMIC waves in driving relativistic electron losses. Nonlinear effects may abound and require further investigation.
650		4	\|a Relativistic electron precipitation \|7 (dpeaa)DE-He213
650		4	\|a Radiation belts \|7 (dpeaa)DE-He213
650		4	\|a Magnetosphere \|7 (dpeaa)DE-He213
650		4	\|a Electromagnetic ion cyclotron waves \|7 (dpeaa)DE-He213
650		4	\|a Whistler-mode chorus \|7 (dpeaa)DE-He213
650		4	\|a Plasma waves \|7 (dpeaa)DE-He213
700	1		\|a Zhang, X.-J. \|4 aut
700	1		\|a Artemyev, A. V. \|4 aut
700	1		\|a Mourenas, D. \|4 aut
700	1		\|a Tsai, E. \|4 aut
700	1		\|a Wilkins, C. \|4 aut
700	1		\|a Runov, A. \|4 aut
700	1		\|a Liu, J. \|4 aut
700	1		\|a Turner, D. L. \|4 aut
700	1		\|a Li, W. \|4 aut
700	1		\|a Khurana, K. \|4 aut
700	1		\|a Wirz, R. E. \|4 aut
700	1		\|a Sergeev, V. A. \|4 aut
700	1		\|a Meng, X. \|4 aut
700	1		\|a Wu, J. \|4 aut
700	1		\|a Hartinger, M. D. \|4 aut
700	1		\|a Raita, T. \|4 aut
700	1		\|a Shen, Y. \|4 aut
700	1		\|a An, X. \|4 aut
700	1		\|a Shi, X. \|4 aut
700	1		\|a Bashir, M. F. \|4 aut
700	1		\|a Shen, X. \|4 aut
700	1		\|a Gan, L. \|4 aut
700	1		\|a Qin, M. \|4 aut
700	1		\|a Capannolo, L. \|4 aut
700	1		\|a Ma, Q. \|4 aut
700	1		\|a Russell, C. L. \|4 aut
700	1		\|a Masongsong, E. V. \|4 aut
700	1		\|a Caron, R. \|4 aut
700	1		\|a He, I. \|4 aut
700	1		\|a Iglesias, L. \|4 aut
700	1		\|a Jha, S. \|4 aut
700	1		\|a King, J. \|4 aut
700	1		\|a Kumar, S. \|4 aut
700	1		\|a Le, K. \|4 aut
700	1		\|a Mao, J. \|4 aut
700	1		\|a McDermott, A. \|4 aut
700	1		\|a Nguyen, K. \|4 aut
700	1		\|a Norris, A. \|4 aut
700	1		\|a Palla, A. \|4 aut
700	1		\|a Roosnovo, A. \|4 aut
700	1		\|a Tam, J. \|4 aut
700	1		\|a Xie, E. \|4 aut
700	1		\|a Yap, R. C. \|4 aut
700	1		\|a Ye, S. \|4 aut
700	1		\|a Young, C. \|4 aut
700	1		\|a Adair, L. A. \|4 aut
700	1		\|a Shaffer, C. \|4 aut
700	1		\|a Chung, M. \|4 aut
700	1		\|a Cruce, P. \|4 aut
700	1		\|a Lawson, M. \|4 aut
700	1		\|a Leneman, D. \|4 aut
700	1		\|a Allen, M. \|4 aut
700	1		\|a Anderson, M. \|4 aut
700	1		\|a Arreola-Zamora, M. \|4 aut
700	1		\|a Artinger, J. \|4 aut
700	1		\|a Asher, J. \|4 aut
700	1		\|a Branchevsky, D. \|4 aut
700	1		\|a Cliffe, M. \|4 aut
700	1		\|a Colton, K. \|4 aut
700	1		\|a Costello, C. \|4 aut
700	1		\|a Depe, D. \|4 aut
700	1		\|a Domae, B. W. \|4 aut
700	1		\|a Eldin, S. \|4 aut
700	1		\|a Fitzgibbon, L. \|4 aut
700	1		\|a Flemming, A. \|4 aut
700	1		\|a Frederick, D. M. \|4 aut
700	1		\|a Gilbert, A. \|4 aut
700	1		\|a Hesford, B. \|4 aut
700	1		\|a Krieger, R. \|4 aut
700	1		\|a Lian, K. \|4 aut
700	1		\|a McKinney, E. \|4 aut
700	1		\|a Miller, J. P. \|4 aut
700	1		\|a Pedersen, C. \|4 aut
700	1		\|a Qu, Z. \|4 aut
700	1		\|a Rozario, R. \|4 aut
700	1		\|a Rubly, M. \|4 aut
700	1		\|a Seaton, R. \|4 aut
700	1		\|a Subramanian, A. \|4 aut
700	1		\|a Sundin, S. R. \|4 aut
700	1		\|a Tan, A. \|4 aut
700	1		\|a Thomlinson, D. \|4 aut
700	1		\|a Turner, W. \|4 aut
700	1		\|a Wing, G. \|4 aut
700	1		\|a Wong, C. \|4 aut
700	1		\|a Zarifian, A. \|4 aut
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allfields	10.1007/s11214-023-00984-w doi (DE-627)SPR052211800 (SPR)s11214-023-00984-w-e DE-627 ger DE-627 rakwb eng Angelopoulos, V. verfasserin (orcid)0000-0001-7024-1561 aut Energetic Electron Precipitation Driven by Electromagnetic Ion Cyclotron Waves from ELFIN’s Low Altitude Perspective 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © The Author(s) 2023 Abstract We review comprehensive observations of electromagnetic ion cyclotron (EMIC) wave-driven energetic electron precipitation using data collected by the energetic electron detector on the Electron Losses and Fields InvestigatioN (ELFIN) mission, two polar-orbiting low-altitude spinning CubeSats, measuring 50-5000 keV electrons with good pitch-angle and energy resolution. EMIC wave-driven precipitation exhibits a distinct signature in energy-spectrograms of the precipitating-to-trapped flux ratio: peaks at >0.5 MeV which are abrupt (bursty) (lasting ∼17 s, or $\Delta L\sim 0.56$) with significant substructure (occasionally down to sub-second timescale). We attribute the bursty nature of the precipitation to the spatial extent and structuredness of the wave field at the equator. Multiple ELFIN passes over the same MLT sector allow us to study the spatial and temporal evolution of the EMIC wave - electron interaction region. Case studies employing conjugate ground-based or equatorial observations of the EMIC waves reveal that the energy of moderate and strong precipitation at ELFIN approximately agrees with theoretical expectations for cyclotron resonant interactions in a cold plasma. Using multiple years of ELFIN data uniformly distributed in local time, we assemble a statistical database of ∼50 events of strong EMIC wave-driven precipitation. Most reside at $L\sim 5-7$ at dusk, while a smaller subset exists at $L\sim 8-12$ at post-midnight. The energies of the peak-precipitation ratio and of the half-peak precipitation ratio (our proxy for the minimum resonance energy) exhibit an $L$-shell dependence in good agreement with theoretical estimates based on prior statistical observations of EMIC wave power spectra. The precipitation ratio’s spectral shape for the most intense events has an exponential falloff away from the peak (i.e., on either side of $\sim 1.45$ MeV). It too agrees well with quasi-linear diffusion theory based on prior statistics of wave spectra. It should be noted though that this diffusive treatment likely includes effects from nonlinear resonant interactions (especially at high energies) and nonresonant effects from sharp wave packet edges (at low energies). Sub-MeV electron precipitation observed concurrently with strong EMIC wave-driven >1 MeV precipitation has a spectral shape that is consistent with efficient pitch-angle scattering down to ∼ 200-300 keV by much less intense higher frequency EMIC waves at dusk (where such waves are most frequent). At ∼100 keV, whistler-mode chorus may be implicated in concurrent precipitation. These results confirm the critical role of EMIC waves in driving relativistic electron losses. Nonlinear effects may abound and require further investigation. Relativistic electron precipitation (dpeaa)DE-He213 Radiation belts (dpeaa)DE-He213 Magnetosphere (dpeaa)DE-He213 Electromagnetic ion cyclotron waves (dpeaa)DE-He213 Whistler-mode chorus (dpeaa)DE-He213 Plasma waves (dpeaa)DE-He213 Zhang, X.-J. aut Artemyev, A. V. aut Mourenas, D. aut Tsai, E. aut Wilkins, C. aut Runov, A. aut Liu, J. aut Turner, D. L. aut Li, W. aut Khurana, K. aut Wirz, R. E. aut Sergeev, V. A. aut Meng, X. aut Wu, J. aut Hartinger, M. D. aut Raita, T. aut Shen, Y. aut An, X. aut Shi, X. aut Bashir, M. F. aut Shen, X. aut Gan, L. aut Qin, M. aut Capannolo, L. aut Ma, Q. aut Russell, C. L. aut Masongsong, E. V. aut Caron, R. aut He, I. aut Iglesias, L. aut Jha, S. aut King, J. aut Kumar, S. aut Le, K. aut Mao, J. aut McDermott, A. aut Nguyen, K. aut Norris, A. aut Palla, A. aut Roosnovo, A. aut Tam, J. aut Xie, E. aut Yap, R. C. aut Ye, S. aut Young, C. aut Adair, L. A. aut Shaffer, C. aut Chung, M. aut Cruce, P. aut Lawson, M. aut Leneman, D. aut Allen, M. aut Anderson, M. aut Arreola-Zamora, M. aut Artinger, J. aut Asher, J. aut Branchevsky, D. aut Cliffe, M. aut Colton, K. aut Costello, C. aut Depe, D. aut Domae, B. W. aut Eldin, S. aut Fitzgibbon, L. aut Flemming, A. aut Frederick, D. M. aut Gilbert, A. aut Hesford, B. aut Krieger, R. aut Lian, K. aut McKinney, E. aut Miller, J. P. aut Pedersen, C. aut Qu, Z. aut Rozario, R. aut Rubly, M. aut Seaton, R. aut Subramanian, A. aut Sundin, S. R. aut Tan, A. aut Thomlinson, D. aut Turner, W. aut Wing, G. aut Wong, C. aut Zarifian, A. aut Enthalten in Space science reviews Dordrecht [u.a.] : Springer Science + Business Media B.V, 1962 219(2023), 5 vom: 11. Juli (DE-627)315621222 (DE-600)2017804-9 1572-9672 nnns volume:219 year:2023 number:5 day:11 month:07 https://dx.doi.org/10.1007/s11214-023-00984-w kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 AR 219 2023 5 11 07
spelling	10.1007/s11214-023-00984-w doi (DE-627)SPR052211800 (SPR)s11214-023-00984-w-e DE-627 ger DE-627 rakwb eng Angelopoulos, V. verfasserin (orcid)0000-0001-7024-1561 aut Energetic Electron Precipitation Driven by Electromagnetic Ion Cyclotron Waves from ELFIN’s Low Altitude Perspective 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © The Author(s) 2023 Abstract We review comprehensive observations of electromagnetic ion cyclotron (EMIC) wave-driven energetic electron precipitation using data collected by the energetic electron detector on the Electron Losses and Fields InvestigatioN (ELFIN) mission, two polar-orbiting low-altitude spinning CubeSats, measuring 50-5000 keV electrons with good pitch-angle and energy resolution. EMIC wave-driven precipitation exhibits a distinct signature in energy-spectrograms of the precipitating-to-trapped flux ratio: peaks at >0.5 MeV which are abrupt (bursty) (lasting ∼17 s, or $\Delta L\sim 0.56$) with significant substructure (occasionally down to sub-second timescale). We attribute the bursty nature of the precipitation to the spatial extent and structuredness of the wave field at the equator. Multiple ELFIN passes over the same MLT sector allow us to study the spatial and temporal evolution of the EMIC wave - electron interaction region. Case studies employing conjugate ground-based or equatorial observations of the EMIC waves reveal that the energy of moderate and strong precipitation at ELFIN approximately agrees with theoretical expectations for cyclotron resonant interactions in a cold plasma. Using multiple years of ELFIN data uniformly distributed in local time, we assemble a statistical database of ∼50 events of strong EMIC wave-driven precipitation. Most reside at $L\sim 5-7$ at dusk, while a smaller subset exists at $L\sim 8-12$ at post-midnight. The energies of the peak-precipitation ratio and of the half-peak precipitation ratio (our proxy for the minimum resonance energy) exhibit an $L$-shell dependence in good agreement with theoretical estimates based on prior statistical observations of EMIC wave power spectra. The precipitation ratio’s spectral shape for the most intense events has an exponential falloff away from the peak (i.e., on either side of $\sim 1.45$ MeV). It too agrees well with quasi-linear diffusion theory based on prior statistics of wave spectra. It should be noted though that this diffusive treatment likely includes effects from nonlinear resonant interactions (especially at high energies) and nonresonant effects from sharp wave packet edges (at low energies). Sub-MeV electron precipitation observed concurrently with strong EMIC wave-driven >1 MeV precipitation has a spectral shape that is consistent with efficient pitch-angle scattering down to ∼ 200-300 keV by much less intense higher frequency EMIC waves at dusk (where such waves are most frequent). At ∼100 keV, whistler-mode chorus may be implicated in concurrent precipitation. These results confirm the critical role of EMIC waves in driving relativistic electron losses. Nonlinear effects may abound and require further investigation. Relativistic electron precipitation (dpeaa)DE-He213 Radiation belts (dpeaa)DE-He213 Magnetosphere (dpeaa)DE-He213 Electromagnetic ion cyclotron waves (dpeaa)DE-He213 Whistler-mode chorus (dpeaa)DE-He213 Plasma waves (dpeaa)DE-He213 Zhang, X.-J. aut Artemyev, A. V. aut Mourenas, D. aut Tsai, E. aut Wilkins, C. aut Runov, A. aut Liu, J. aut Turner, D. L. aut Li, W. aut Khurana, K. aut Wirz, R. E. aut Sergeev, V. A. aut Meng, X. aut Wu, J. aut Hartinger, M. D. aut Raita, T. aut Shen, Y. aut An, X. aut Shi, X. aut Bashir, M. F. aut Shen, X. aut Gan, L. aut Qin, M. aut Capannolo, L. aut Ma, Q. aut Russell, C. L. aut Masongsong, E. V. aut Caron, R. aut He, I. aut Iglesias, L. aut Jha, S. aut King, J. aut Kumar, S. aut Le, K. aut Mao, J. aut McDermott, A. aut Nguyen, K. aut Norris, A. aut Palla, A. aut Roosnovo, A. aut Tam, J. aut Xie, E. aut Yap, R. C. aut Ye, S. aut Young, C. aut Adair, L. A. aut Shaffer, C. aut Chung, M. aut Cruce, P. aut Lawson, M. aut Leneman, D. aut Allen, M. aut Anderson, M. aut Arreola-Zamora, M. aut Artinger, J. aut Asher, J. aut Branchevsky, D. aut Cliffe, M. aut Colton, K. aut Costello, C. aut Depe, D. aut Domae, B. W. aut Eldin, S. aut Fitzgibbon, L. aut Flemming, A. aut Frederick, D. M. aut Gilbert, A. aut Hesford, B. aut Krieger, R. aut Lian, K. aut McKinney, E. aut Miller, J. P. aut Pedersen, C. aut Qu, Z. aut Rozario, R. aut Rubly, M. aut Seaton, R. aut Subramanian, A. aut Sundin, S. R. aut Tan, A. aut Thomlinson, D. aut Turner, W. aut Wing, G. aut Wong, C. aut Zarifian, A. aut Enthalten in Space science reviews Dordrecht [u.a.] : Springer Science + Business Media B.V, 1962 219(2023), 5 vom: 11. Juli (DE-627)315621222 (DE-600)2017804-9 1572-9672 nnns volume:219 year:2023 number:5 day:11 month:07 https://dx.doi.org/10.1007/s11214-023-00984-w kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 AR 219 2023 5 11 07
allfields_unstemmed	10.1007/s11214-023-00984-w doi (DE-627)SPR052211800 (SPR)s11214-023-00984-w-e DE-627 ger DE-627 rakwb eng Angelopoulos, V. verfasserin (orcid)0000-0001-7024-1561 aut Energetic Electron Precipitation Driven by Electromagnetic Ion Cyclotron Waves from ELFIN’s Low Altitude Perspective 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © The Author(s) 2023 Abstract We review comprehensive observations of electromagnetic ion cyclotron (EMIC) wave-driven energetic electron precipitation using data collected by the energetic electron detector on the Electron Losses and Fields InvestigatioN (ELFIN) mission, two polar-orbiting low-altitude spinning CubeSats, measuring 50-5000 keV electrons with good pitch-angle and energy resolution. EMIC wave-driven precipitation exhibits a distinct signature in energy-spectrograms of the precipitating-to-trapped flux ratio: peaks at >0.5 MeV which are abrupt (bursty) (lasting ∼17 s, or $\Delta L\sim 0.56$) with significant substructure (occasionally down to sub-second timescale). We attribute the bursty nature of the precipitation to the spatial extent and structuredness of the wave field at the equator. Multiple ELFIN passes over the same MLT sector allow us to study the spatial and temporal evolution of the EMIC wave - electron interaction region. Case studies employing conjugate ground-based or equatorial observations of the EMIC waves reveal that the energy of moderate and strong precipitation at ELFIN approximately agrees with theoretical expectations for cyclotron resonant interactions in a cold plasma. Using multiple years of ELFIN data uniformly distributed in local time, we assemble a statistical database of ∼50 events of strong EMIC wave-driven precipitation. Most reside at $L\sim 5-7$ at dusk, while a smaller subset exists at $L\sim 8-12$ at post-midnight. The energies of the peak-precipitation ratio and of the half-peak precipitation ratio (our proxy for the minimum resonance energy) exhibit an $L$-shell dependence in good agreement with theoretical estimates based on prior statistical observations of EMIC wave power spectra. The precipitation ratio’s spectral shape for the most intense events has an exponential falloff away from the peak (i.e., on either side of $\sim 1.45$ MeV). It too agrees well with quasi-linear diffusion theory based on prior statistics of wave spectra. It should be noted though that this diffusive treatment likely includes effects from nonlinear resonant interactions (especially at high energies) and nonresonant effects from sharp wave packet edges (at low energies). Sub-MeV electron precipitation observed concurrently with strong EMIC wave-driven >1 MeV precipitation has a spectral shape that is consistent with efficient pitch-angle scattering down to ∼ 200-300 keV by much less intense higher frequency EMIC waves at dusk (where such waves are most frequent). At ∼100 keV, whistler-mode chorus may be implicated in concurrent precipitation. These results confirm the critical role of EMIC waves in driving relativistic electron losses. Nonlinear effects may abound and require further investigation. Relativistic electron precipitation (dpeaa)DE-He213 Radiation belts (dpeaa)DE-He213 Magnetosphere (dpeaa)DE-He213 Electromagnetic ion cyclotron waves (dpeaa)DE-He213 Whistler-mode chorus (dpeaa)DE-He213 Plasma waves (dpeaa)DE-He213 Zhang, X.-J. aut Artemyev, A. V. aut Mourenas, D. aut Tsai, E. aut Wilkins, C. aut Runov, A. aut Liu, J. aut Turner, D. L. aut Li, W. aut Khurana, K. aut Wirz, R. E. aut Sergeev, V. A. aut Meng, X. aut Wu, J. aut Hartinger, M. D. aut Raita, T. aut Shen, Y. aut An, X. aut Shi, X. aut Bashir, M. F. aut Shen, X. aut Gan, L. aut Qin, M. aut Capannolo, L. aut Ma, Q. aut Russell, C. L. aut Masongsong, E. V. aut Caron, R. aut He, I. aut Iglesias, L. aut Jha, S. aut King, J. aut Kumar, S. aut Le, K. aut Mao, J. aut McDermott, A. aut Nguyen, K. aut Norris, A. aut Palla, A. aut Roosnovo, A. aut Tam, J. aut Xie, E. aut Yap, R. C. aut Ye, S. aut Young, C. aut Adair, L. A. aut Shaffer, C. aut Chung, M. aut Cruce, P. aut Lawson, M. aut Leneman, D. aut Allen, M. aut Anderson, M. aut Arreola-Zamora, M. aut Artinger, J. aut Asher, J. aut Branchevsky, D. aut Cliffe, M. aut Colton, K. aut Costello, C. aut Depe, D. aut Domae, B. W. aut Eldin, S. aut Fitzgibbon, L. aut Flemming, A. aut Frederick, D. M. aut Gilbert, A. aut Hesford, B. aut Krieger, R. aut Lian, K. aut McKinney, E. aut Miller, J. P. aut Pedersen, C. aut Qu, Z. aut Rozario, R. aut Rubly, M. aut Seaton, R. aut Subramanian, A. aut Sundin, S. R. aut Tan, A. aut Thomlinson, D. aut Turner, W. aut Wing, G. aut Wong, C. aut Zarifian, A. aut Enthalten in Space science reviews Dordrecht [u.a.] : Springer Science + Business Media B.V, 1962 219(2023), 5 vom: 11. Juli (DE-627)315621222 (DE-600)2017804-9 1572-9672 nnns volume:219 year:2023 number:5 day:11 month:07 https://dx.doi.org/10.1007/s11214-023-00984-w kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 AR 219 2023 5 11 07
allfieldsGer	10.1007/s11214-023-00984-w doi (DE-627)SPR052211800 (SPR)s11214-023-00984-w-e DE-627 ger DE-627 rakwb eng Angelopoulos, V. verfasserin (orcid)0000-0001-7024-1561 aut Energetic Electron Precipitation Driven by Electromagnetic Ion Cyclotron Waves from ELFIN’s Low Altitude Perspective 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © The Author(s) 2023 Abstract We review comprehensive observations of electromagnetic ion cyclotron (EMIC) wave-driven energetic electron precipitation using data collected by the energetic electron detector on the Electron Losses and Fields InvestigatioN (ELFIN) mission, two polar-orbiting low-altitude spinning CubeSats, measuring 50-5000 keV electrons with good pitch-angle and energy resolution. EMIC wave-driven precipitation exhibits a distinct signature in energy-spectrograms of the precipitating-to-trapped flux ratio: peaks at >0.5 MeV which are abrupt (bursty) (lasting ∼17 s, or $\Delta L\sim 0.56$) with significant substructure (occasionally down to sub-second timescale). We attribute the bursty nature of the precipitation to the spatial extent and structuredness of the wave field at the equator. Multiple ELFIN passes over the same MLT sector allow us to study the spatial and temporal evolution of the EMIC wave - electron interaction region. Case studies employing conjugate ground-based or equatorial observations of the EMIC waves reveal that the energy of moderate and strong precipitation at ELFIN approximately agrees with theoretical expectations for cyclotron resonant interactions in a cold plasma. Using multiple years of ELFIN data uniformly distributed in local time, we assemble a statistical database of ∼50 events of strong EMIC wave-driven precipitation. Most reside at $L\sim 5-7$ at dusk, while a smaller subset exists at $L\sim 8-12$ at post-midnight. The energies of the peak-precipitation ratio and of the half-peak precipitation ratio (our proxy for the minimum resonance energy) exhibit an $L$-shell dependence in good agreement with theoretical estimates based on prior statistical observations of EMIC wave power spectra. The precipitation ratio’s spectral shape for the most intense events has an exponential falloff away from the peak (i.e., on either side of $\sim 1.45$ MeV). It too agrees well with quasi-linear diffusion theory based on prior statistics of wave spectra. It should be noted though that this diffusive treatment likely includes effects from nonlinear resonant interactions (especially at high energies) and nonresonant effects from sharp wave packet edges (at low energies). Sub-MeV electron precipitation observed concurrently with strong EMIC wave-driven >1 MeV precipitation has a spectral shape that is consistent with efficient pitch-angle scattering down to ∼ 200-300 keV by much less intense higher frequency EMIC waves at dusk (where such waves are most frequent). At ∼100 keV, whistler-mode chorus may be implicated in concurrent precipitation. These results confirm the critical role of EMIC waves in driving relativistic electron losses. Nonlinear effects may abound and require further investigation. Relativistic electron precipitation (dpeaa)DE-He213 Radiation belts (dpeaa)DE-He213 Magnetosphere (dpeaa)DE-He213 Electromagnetic ion cyclotron waves (dpeaa)DE-He213 Whistler-mode chorus (dpeaa)DE-He213 Plasma waves (dpeaa)DE-He213 Zhang, X.-J. aut Artemyev, A. V. aut Mourenas, D. aut Tsai, E. aut Wilkins, C. aut Runov, A. aut Liu, J. aut Turner, D. L. aut Li, W. aut Khurana, K. aut Wirz, R. E. aut Sergeev, V. A. aut Meng, X. aut Wu, J. aut Hartinger, M. D. aut Raita, T. aut Shen, Y. aut An, X. aut Shi, X. aut Bashir, M. F. aut Shen, X. aut Gan, L. aut Qin, M. aut Capannolo, L. aut Ma, Q. aut Russell, C. L. aut Masongsong, E. V. aut Caron, R. aut He, I. aut Iglesias, L. aut Jha, S. aut King, J. aut Kumar, S. aut Le, K. aut Mao, J. aut McDermott, A. aut Nguyen, K. aut Norris, A. aut Palla, A. aut Roosnovo, A. aut Tam, J. aut Xie, E. aut Yap, R. C. aut Ye, S. aut Young, C. aut Adair, L. A. aut Shaffer, C. aut Chung, M. aut Cruce, P. aut Lawson, M. aut Leneman, D. aut Allen, M. aut Anderson, M. aut Arreola-Zamora, M. aut Artinger, J. aut Asher, J. aut Branchevsky, D. aut Cliffe, M. aut Colton, K. aut Costello, C. aut Depe, D. aut Domae, B. W. aut Eldin, S. aut Fitzgibbon, L. aut Flemming, A. aut Frederick, D. M. aut Gilbert, A. aut Hesford, B. aut Krieger, R. aut Lian, K. aut McKinney, E. aut Miller, J. P. aut Pedersen, C. aut Qu, Z. aut Rozario, R. aut Rubly, M. aut Seaton, R. aut Subramanian, A. aut Sundin, S. R. aut Tan, A. aut Thomlinson, D. aut Turner, W. aut Wing, G. aut Wong, C. aut Zarifian, A. aut Enthalten in Space science reviews Dordrecht [u.a.] : Springer Science + Business Media B.V, 1962 219(2023), 5 vom: 11. Juli (DE-627)315621222 (DE-600)2017804-9 1572-9672 nnns volume:219 year:2023 number:5 day:11 month:07 https://dx.doi.org/10.1007/s11214-023-00984-w kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 AR 219 2023 5 11 07
allfieldsSound	10.1007/s11214-023-00984-w doi (DE-627)SPR052211800 (SPR)s11214-023-00984-w-e DE-627 ger DE-627 rakwb eng Angelopoulos, V. verfasserin (orcid)0000-0001-7024-1561 aut Energetic Electron Precipitation Driven by Electromagnetic Ion Cyclotron Waves from ELFIN’s Low Altitude Perspective 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © The Author(s) 2023 Abstract We review comprehensive observations of electromagnetic ion cyclotron (EMIC) wave-driven energetic electron precipitation using data collected by the energetic electron detector on the Electron Losses and Fields InvestigatioN (ELFIN) mission, two polar-orbiting low-altitude spinning CubeSats, measuring 50-5000 keV electrons with good pitch-angle and energy resolution. EMIC wave-driven precipitation exhibits a distinct signature in energy-spectrograms of the precipitating-to-trapped flux ratio: peaks at >0.5 MeV which are abrupt (bursty) (lasting ∼17 s, or $\Delta L\sim 0.56$) with significant substructure (occasionally down to sub-second timescale). We attribute the bursty nature of the precipitation to the spatial extent and structuredness of the wave field at the equator. Multiple ELFIN passes over the same MLT sector allow us to study the spatial and temporal evolution of the EMIC wave - electron interaction region. Case studies employing conjugate ground-based or equatorial observations of the EMIC waves reveal that the energy of moderate and strong precipitation at ELFIN approximately agrees with theoretical expectations for cyclotron resonant interactions in a cold plasma. Using multiple years of ELFIN data uniformly distributed in local time, we assemble a statistical database of ∼50 events of strong EMIC wave-driven precipitation. Most reside at $L\sim 5-7$ at dusk, while a smaller subset exists at $L\sim 8-12$ at post-midnight. The energies of the peak-precipitation ratio and of the half-peak precipitation ratio (our proxy for the minimum resonance energy) exhibit an $L$-shell dependence in good agreement with theoretical estimates based on prior statistical observations of EMIC wave power spectra. The precipitation ratio’s spectral shape for the most intense events has an exponential falloff away from the peak (i.e., on either side of $\sim 1.45$ MeV). It too agrees well with quasi-linear diffusion theory based on prior statistics of wave spectra. It should be noted though that this diffusive treatment likely includes effects from nonlinear resonant interactions (especially at high energies) and nonresonant effects from sharp wave packet edges (at low energies). Sub-MeV electron precipitation observed concurrently with strong EMIC wave-driven >1 MeV precipitation has a spectral shape that is consistent with efficient pitch-angle scattering down to ∼ 200-300 keV by much less intense higher frequency EMIC waves at dusk (where such waves are most frequent). At ∼100 keV, whistler-mode chorus may be implicated in concurrent precipitation. These results confirm the critical role of EMIC waves in driving relativistic electron losses. Nonlinear effects may abound and require further investigation. Relativistic electron precipitation (dpeaa)DE-He213 Radiation belts (dpeaa)DE-He213 Magnetosphere (dpeaa)DE-He213 Electromagnetic ion cyclotron waves (dpeaa)DE-He213 Whistler-mode chorus (dpeaa)DE-He213 Plasma waves (dpeaa)DE-He213 Zhang, X.-J. aut Artemyev, A. V. aut Mourenas, D. aut Tsai, E. aut Wilkins, C. aut Runov, A. aut Liu, J. aut Turner, D. L. aut Li, W. aut Khurana, K. aut Wirz, R. E. aut Sergeev, V. A. aut Meng, X. aut Wu, J. aut Hartinger, M. D. aut Raita, T. aut Shen, Y. aut An, X. aut Shi, X. aut Bashir, M. F. aut Shen, X. aut Gan, L. aut Qin, M. aut Capannolo, L. aut Ma, Q. aut Russell, C. L. aut Masongsong, E. V. aut Caron, R. aut He, I. aut Iglesias, L. aut Jha, S. aut King, J. aut Kumar, S. aut Le, K. aut Mao, J. aut McDermott, A. aut Nguyen, K. aut Norris, A. aut Palla, A. aut Roosnovo, A. aut Tam, J. aut Xie, E. aut Yap, R. C. aut Ye, S. aut Young, C. aut Adair, L. A. aut Shaffer, C. aut Chung, M. aut Cruce, P. aut Lawson, M. aut Leneman, D. aut Allen, M. aut Anderson, M. aut Arreola-Zamora, M. aut Artinger, J. aut Asher, J. aut Branchevsky, D. aut Cliffe, M. aut Colton, K. aut Costello, C. aut Depe, D. aut Domae, B. W. aut Eldin, S. aut Fitzgibbon, L. aut Flemming, A. aut Frederick, D. M. aut Gilbert, A. aut Hesford, B. aut Krieger, R. aut Lian, K. aut McKinney, E. aut Miller, J. P. aut Pedersen, C. aut Qu, Z. aut Rozario, R. aut Rubly, M. aut Seaton, R. aut Subramanian, A. aut Sundin, S. R. aut Tan, A. aut Thomlinson, D. aut Turner, W. aut Wing, G. aut Wong, C. aut Zarifian, A. aut Enthalten in Space science reviews Dordrecht [u.a.] : Springer Science + Business Media B.V, 1962 219(2023), 5 vom: 11. Juli (DE-627)315621222 (DE-600)2017804-9 1572-9672 nnns volume:219 year:2023 number:5 day:11 month:07 https://dx.doi.org/10.1007/s11214-023-00984-w kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 AR 219 2023 5 11 07
language	English
source	Enthalten in Space science reviews 219(2023), 5 vom: 11. Juli volume:219 year:2023 number:5 day:11 month:07
sourceStr	Enthalten in Space science reviews 219(2023), 5 vom: 11. Juli volume:219 year:2023 number:5 day:11 month:07
format_phy_str_mv	Article
institution	findex.gbv.de
topic_facet	Relativistic electron precipitation Radiation belts Magnetosphere Electromagnetic ion cyclotron waves Whistler-mode chorus Plasma waves
isfreeaccess_bool	true
container_title	Space science reviews
authorswithroles_txt_mv	Angelopoulos, V. @@aut@@ Zhang, X.-J. @@aut@@ Artemyev, A. V. @@aut@@ Mourenas, D. @@aut@@ Tsai, E. @@aut@@ Wilkins, C. @@aut@@ Runov, A. @@aut@@ Liu, J. @@aut@@ Turner, D. L. @@aut@@ Li, W. @@aut@@ Khurana, K. @@aut@@ Wirz, R. E. @@aut@@ Sergeev, V. A. @@aut@@ Meng, X. @@aut@@ Wu, J. @@aut@@ Hartinger, M. D. @@aut@@ Raita, T. @@aut@@ Shen, Y. @@aut@@ An, X. @@aut@@ Shi, X. @@aut@@ Bashir, M. F. @@aut@@ Shen, X. @@aut@@ Gan, L. @@aut@@ Qin, M. @@aut@@ Capannolo, L. @@aut@@ Ma, Q. @@aut@@ Russell, C. L. @@aut@@ Masongsong, E. V. @@aut@@ Caron, R. @@aut@@ He, I. @@aut@@ Iglesias, L. @@aut@@ Jha, S. @@aut@@ King, J. @@aut@@ Kumar, S. @@aut@@ Le, K. @@aut@@ Mao, J. @@aut@@ McDermott, A. @@aut@@ Nguyen, K. @@aut@@ Norris, A. @@aut@@ Palla, A. @@aut@@ Roosnovo, A. @@aut@@ Tam, J. @@aut@@ Xie, E. @@aut@@ Yap, R. C. @@aut@@ Ye, S. @@aut@@ Young, C. @@aut@@ Adair, L. A. @@aut@@ Shaffer, C. @@aut@@ Chung, M. @@aut@@ Cruce, P. @@aut@@ Lawson, M. @@aut@@ Leneman, D. @@aut@@ Allen, M. @@aut@@ Anderson, M. @@aut@@ Arreola-Zamora, M. @@aut@@ Artinger, J. @@aut@@ Asher, J. @@aut@@ Branchevsky, D. @@aut@@ Cliffe, M. @@aut@@ Colton, K. @@aut@@ Costello, C. @@aut@@ Depe, D. @@aut@@ Domae, B. W. @@aut@@ Eldin, S. @@aut@@ Fitzgibbon, L. @@aut@@ Flemming, A. @@aut@@ Frederick, D. M. @@aut@@ Gilbert, A. @@aut@@ Hesford, B. @@aut@@ Krieger, R. @@aut@@ Lian, K. @@aut@@ McKinney, E. @@aut@@ Miller, J. P. @@aut@@ Pedersen, C. @@aut@@ Qu, Z. @@aut@@ Rozario, R. @@aut@@ Rubly, M. @@aut@@ Seaton, R. @@aut@@ Subramanian, A. @@aut@@ Sundin, S. R. @@aut@@ Tan, A. @@aut@@ Thomlinson, D. @@aut@@ Turner, W. @@aut@@ Wing, G. @@aut@@ Wong, C. @@aut@@ Zarifian, A. @@aut@@
publishDateDaySort_date	2023-07-11T00:00:00Z
hierarchy_top_id	315621222
id	SPR052211800
language_de	englisch
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author	Angelopoulos, V.
spellingShingle	Angelopoulos, V. misc Relativistic electron precipitation misc Radiation belts misc Magnetosphere misc Electromagnetic ion cyclotron waves misc Whistler-mode chorus misc Plasma waves Energetic Electron Precipitation Driven by Electromagnetic Ion Cyclotron Waves from ELFIN’s Low Altitude Perspective
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topic_title	Energetic Electron Precipitation Driven by Electromagnetic Ion Cyclotron Waves from ELFIN’s Low Altitude Perspective Relativistic electron precipitation (dpeaa)DE-He213 Radiation belts (dpeaa)DE-He213 Magnetosphere (dpeaa)DE-He213 Electromagnetic ion cyclotron waves (dpeaa)DE-He213 Whistler-mode chorus (dpeaa)DE-He213 Plasma waves (dpeaa)DE-He213
topic	misc Relativistic electron precipitation misc Radiation belts misc Magnetosphere misc Electromagnetic ion cyclotron waves misc Whistler-mode chorus misc Plasma waves
topic_unstemmed	misc Relativistic electron precipitation misc Radiation belts misc Magnetosphere misc Electromagnetic ion cyclotron waves misc Whistler-mode chorus misc Plasma waves
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title	Energetic Electron Precipitation Driven by Electromagnetic Ion Cyclotron Waves from ELFIN’s Low Altitude Perspective
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title_full	Energetic Electron Precipitation Driven by Electromagnetic Ion Cyclotron Waves from ELFIN’s Low Altitude Perspective
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author_browse	Angelopoulos, V. Zhang, X.-J. Artemyev, A. V. Mourenas, D. Tsai, E. Wilkins, C. Runov, A. Liu, J. Turner, D. L. Li, W. Khurana, K. Wirz, R. E. Sergeev, V. A. Meng, X. Wu, J. Hartinger, M. D. Raita, T. Shen, Y. An, X. Shi, X. Bashir, M. F. Shen, X. Gan, L. Qin, M. Capannolo, L. Ma, Q. Russell, C. L. Masongsong, E. V. Caron, R. He, I. Iglesias, L. Jha, S. King, J. Kumar, S. Le, K. Mao, J. McDermott, A. Nguyen, K. Norris, A. Palla, A. Roosnovo, A. Tam, J. Xie, E. Yap, R. C. Ye, S. Young, C. Adair, L. A. Shaffer, C. Chung, M. Cruce, P. Lawson, M. Leneman, D. Allen, M. Anderson, M. Arreola-Zamora, M. Artinger, J. Asher, J. Branchevsky, D. Cliffe, M. Colton, K. Costello, C. Depe, D. Domae, B. W. Eldin, S. Fitzgibbon, L. Flemming, A. Frederick, D. M. Gilbert, A. Hesford, B. Krieger, R. Lian, K. McKinney, E. Miller, J. P. Pedersen, C. Qu, Z. Rozario, R. Rubly, M. Seaton, R. Subramanian, A. Sundin, S. R. Tan, A. Thomlinson, D. Turner, W. Wing, G. Wong, C. Zarifian, A.
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title_sort	energetic electron precipitation driven by electromagnetic ion cyclotron waves from elfin’s low altitude perspective
title_auth	Energetic Electron Precipitation Driven by Electromagnetic Ion Cyclotron Waves from ELFIN’s Low Altitude Perspective
abstract	Abstract We review comprehensive observations of electromagnetic ion cyclotron (EMIC) wave-driven energetic electron precipitation using data collected by the energetic electron detector on the Electron Losses and Fields InvestigatioN (ELFIN) mission, two polar-orbiting low-altitude spinning CubeSats, measuring 50-5000 keV electrons with good pitch-angle and energy resolution. EMIC wave-driven precipitation exhibits a distinct signature in energy-spectrograms of the precipitating-to-trapped flux ratio: peaks at >0.5 MeV which are abrupt (bursty) (lasting ∼17 s, or $\Delta L\sim 0.56$) with significant substructure (occasionally down to sub-second timescale). We attribute the bursty nature of the precipitation to the spatial extent and structuredness of the wave field at the equator. Multiple ELFIN passes over the same MLT sector allow us to study the spatial and temporal evolution of the EMIC wave - electron interaction region. Case studies employing conjugate ground-based or equatorial observations of the EMIC waves reveal that the energy of moderate and strong precipitation at ELFIN approximately agrees with theoretical expectations for cyclotron resonant interactions in a cold plasma. Using multiple years of ELFIN data uniformly distributed in local time, we assemble a statistical database of ∼50 events of strong EMIC wave-driven precipitation. Most reside at $L\sim 5-7$ at dusk, while a smaller subset exists at $L\sim 8-12$ at post-midnight. The energies of the peak-precipitation ratio and of the half-peak precipitation ratio (our proxy for the minimum resonance energy) exhibit an $L$-shell dependence in good agreement with theoretical estimates based on prior statistical observations of EMIC wave power spectra. The precipitation ratio’s spectral shape for the most intense events has an exponential falloff away from the peak (i.e., on either side of $\sim 1.45$ MeV). It too agrees well with quasi-linear diffusion theory based on prior statistics of wave spectra. It should be noted though that this diffusive treatment likely includes effects from nonlinear resonant interactions (especially at high energies) and nonresonant effects from sharp wave packet edges (at low energies). Sub-MeV electron precipitation observed concurrently with strong EMIC wave-driven >1 MeV precipitation has a spectral shape that is consistent with efficient pitch-angle scattering down to ∼ 200-300 keV by much less intense higher frequency EMIC waves at dusk (where such waves are most frequent). At ∼100 keV, whistler-mode chorus may be implicated in concurrent precipitation. These results confirm the critical role of EMIC waves in driving relativistic electron losses. Nonlinear effects may abound and require further investigation. © The Author(s) 2023
abstractGer	Abstract We review comprehensive observations of electromagnetic ion cyclotron (EMIC) wave-driven energetic electron precipitation using data collected by the energetic electron detector on the Electron Losses and Fields InvestigatioN (ELFIN) mission, two polar-orbiting low-altitude spinning CubeSats, measuring 50-5000 keV electrons with good pitch-angle and energy resolution. EMIC wave-driven precipitation exhibits a distinct signature in energy-spectrograms of the precipitating-to-trapped flux ratio: peaks at >0.5 MeV which are abrupt (bursty) (lasting ∼17 s, or $\Delta L\sim 0.56$) with significant substructure (occasionally down to sub-second timescale). We attribute the bursty nature of the precipitation to the spatial extent and structuredness of the wave field at the equator. Multiple ELFIN passes over the same MLT sector allow us to study the spatial and temporal evolution of the EMIC wave - electron interaction region. Case studies employing conjugate ground-based or equatorial observations of the EMIC waves reveal that the energy of moderate and strong precipitation at ELFIN approximately agrees with theoretical expectations for cyclotron resonant interactions in a cold plasma. Using multiple years of ELFIN data uniformly distributed in local time, we assemble a statistical database of ∼50 events of strong EMIC wave-driven precipitation. Most reside at $L\sim 5-7$ at dusk, while a smaller subset exists at $L\sim 8-12$ at post-midnight. The energies of the peak-precipitation ratio and of the half-peak precipitation ratio (our proxy for the minimum resonance energy) exhibit an $L$-shell dependence in good agreement with theoretical estimates based on prior statistical observations of EMIC wave power spectra. The precipitation ratio’s spectral shape for the most intense events has an exponential falloff away from the peak (i.e., on either side of $\sim 1.45$ MeV). It too agrees well with quasi-linear diffusion theory based on prior statistics of wave spectra. It should be noted though that this diffusive treatment likely includes effects from nonlinear resonant interactions (especially at high energies) and nonresonant effects from sharp wave packet edges (at low energies). Sub-MeV electron precipitation observed concurrently with strong EMIC wave-driven >1 MeV precipitation has a spectral shape that is consistent with efficient pitch-angle scattering down to ∼ 200-300 keV by much less intense higher frequency EMIC waves at dusk (where such waves are most frequent). At ∼100 keV, whistler-mode chorus may be implicated in concurrent precipitation. These results confirm the critical role of EMIC waves in driving relativistic electron losses. Nonlinear effects may abound and require further investigation. © The Author(s) 2023
abstract_unstemmed	Abstract We review comprehensive observations of electromagnetic ion cyclotron (EMIC) wave-driven energetic electron precipitation using data collected by the energetic electron detector on the Electron Losses and Fields InvestigatioN (ELFIN) mission, two polar-orbiting low-altitude spinning CubeSats, measuring 50-5000 keV electrons with good pitch-angle and energy resolution. EMIC wave-driven precipitation exhibits a distinct signature in energy-spectrograms of the precipitating-to-trapped flux ratio: peaks at >0.5 MeV which are abrupt (bursty) (lasting ∼17 s, or $\Delta L\sim 0.56$) with significant substructure (occasionally down to sub-second timescale). We attribute the bursty nature of the precipitation to the spatial extent and structuredness of the wave field at the equator. Multiple ELFIN passes over the same MLT sector allow us to study the spatial and temporal evolution of the EMIC wave - electron interaction region. Case studies employing conjugate ground-based or equatorial observations of the EMIC waves reveal that the energy of moderate and strong precipitation at ELFIN approximately agrees with theoretical expectations for cyclotron resonant interactions in a cold plasma. Using multiple years of ELFIN data uniformly distributed in local time, we assemble a statistical database of ∼50 events of strong EMIC wave-driven precipitation. Most reside at $L\sim 5-7$ at dusk, while a smaller subset exists at $L\sim 8-12$ at post-midnight. The energies of the peak-precipitation ratio and of the half-peak precipitation ratio (our proxy for the minimum resonance energy) exhibit an $L$-shell dependence in good agreement with theoretical estimates based on prior statistical observations of EMIC wave power spectra. The precipitation ratio’s spectral shape for the most intense events has an exponential falloff away from the peak (i.e., on either side of $\sim 1.45$ MeV). It too agrees well with quasi-linear diffusion theory based on prior statistics of wave spectra. It should be noted though that this diffusive treatment likely includes effects from nonlinear resonant interactions (especially at high energies) and nonresonant effects from sharp wave packet edges (at low energies). Sub-MeV electron precipitation observed concurrently with strong EMIC wave-driven >1 MeV precipitation has a spectral shape that is consistent with efficient pitch-angle scattering down to ∼ 200-300 keV by much less intense higher frequency EMIC waves at dusk (where such waves are most frequent). At ∼100 keV, whistler-mode chorus may be implicated in concurrent precipitation. These results confirm the critical role of EMIC waves in driving relativistic electron losses. Nonlinear effects may abound and require further investigation. © The Author(s) 2023
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title_short	Energetic Electron Precipitation Driven by Electromagnetic Ion Cyclotron Waves from ELFIN’s Low Altitude Perspective
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Energetic Electron Precipitation Driven by Electromagnetic Ion Cyclotron Waves from ELFIN’s Low Altitude Perspective

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