Transport of transient solar wind particles in Earth’s cusps

Parks, G. K.; Lee, E.; Teste, A.; Wilber, M.; Lin, N.; Canu, P.; Dandouras, I.; Rème, H.; Fu, Song; Goldstein, M. L.

doi:10.1063/1.2965825

Cited by 11 publications

(4 citation statements)

References 24 publications

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“…This feature lends support to the conclusion that the observed wave is resonance‐converted KAW. The exterior cusp region is the interface between inner cusp and magnetosheath [ Parks et al , ; Savin et al , ], thus being able to provide the density inhomogeneity in this boundary area, which are favorable conditions for the resonance‐converted KAW.…”

Section: Discussionmentioning

confidence: 99%

Turbulence in the Earth's cusp region: The k‐filtering analysis

Wang

Cao

et al. 2014

JGR Space Physics

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The results show that the waves propagate quasi-perpendicularly to the background magnetic field. The similarity between the experimental and the theoretical dispersion relations indicates that the measured waves are kinetic Alfvén wave. The waves have right-handed elliptical polarization in the plane perpendicular to k. The main axis of polarization ellipse is perpendicular to the average magnetic field. These features furthermore indicate that the turbulence properties agree well with those of KAW mode. The observed KAW is much possibly produced through resonance mode conversion. We calculate the density gradient vector using multipoint density data and found that the waves propagate basically toward high-density region. The density gradient in the exterior cusp provides a favorable condition for the resonance converted KAW.

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Section: Discussionmentioning

confidence: 99%

Turbulence in the Earth's cusp region: The k‐filtering analysis

Wang

Cao

et al. 2014

JGR Space Physics

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“…In summary, we have two sources of ionization in the open field line regions: photoionization and charge exchange. Observations show that solar wind particles do reach the Earth's cusps and precipitate down the magnetic field lines (Chen & Fritz, 2005; Parks et al., 2008). It is likely that not all solar wind protons reach the exobase, but since we are interested in the upper layers of the atmosphere (exosphere), we assume the medium to be optically thin, so that the photoionization rate and the charge ionization rate can be kept constant.…”

Section: Methodsmentioning

confidence: 99%

Evolution of the Earth's Polar Outflow From Mid‐Archean to Present

et al. 2020

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The development of habitable conditions on Earth is tightly connected to the evolution of its atmosphere, which is strongly influenced by atmospheric escape. We investigate the evolution of the polar ion outflow from the open field line bundle, which is the dominant escape mechanism for the modern Earth. We perform Direct Simulation Monte Carlo (DSMC) simulations and estimate the upper limits on escape rates from the Earth's open field line bundle starting from 3 gigayears ago (Ga) to present assuming the present‐day composition of the atmosphere. We perform two additional simulations with lower mixing ratios of oxygen of 1% and 15% to account for the conditions shortly after the Great Oxydation Event (GOE). We estimate the maximum loss rates due to polar outflow 3 gigayears ago of 3.3×1027 s−1 and 2.4×1027 s−1 for oxygen and nitrogen, respectively. The total integrated mass loss equals to 39% and 10% of the modern atmosphere's mass, for oxygen and nitrogen, respectively. According to our results, the main factors that governed the polar outflow in the considered time period are the evolution of the XUV radiation of the Sun and the atmosphere's composition. The evolution of the Earth's magnetic field plays a less important role. We conclude that although the atmosphere with the present‐day composition can survive the escape due to polar outflow, a higher level of CO2 between 3.0 and 2.0 Ga was likely necessary to reduce the escape.

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“…Kelvin-Helmholtz instability at the flank magnetopause (Fujimoto et al 1998;Fairfield et al 2000;Hasegawa et al 2004), magnetic reconnection at the high-latitude cusp (Li et al 2005;Øieroset et al 2005), and direct entry through the cusp (Fritz & Chen 1999;Parks et al 2008) have been suggested as major candidates for the transport mechanism of the cold, dense magnetosheath plasmas into the magnetosphere. Wing et al (2006) estimated the plasma sheet filling rates by diffusion through the flank magnetopause and reconnection at the high-latitude cusp, but could not determine which one is more suitable because the filling rates from different mechanisms were comparable to each other.…”

Section: Introductionmentioning

confidence: 99%

“…Wing et al (2006) estimated the plasma sheet filling rates by diffusion through the flank magnetopause and reconnection at the high-latitude cusp, but could not determine which one is more suitable because the filling rates from different mechanisms were comparable to each other. Recently, Parks et al (2008) showed that the magnetosheath plasmas could directly penetrate deeply into low-altitude cusp and suggested that direct entry through cusp could be an efficient transport mechanism of magnetosheath plasmas into the magnetosphere. The transport mechanism is still under investigation.…”

Section: Introductionmentioning

confidence: 99%

Observation of Transition Boundary between Cold, Dense and Hot, Tenuous Plasmas in the Near-Earth Magnetotail

Kim¹,

Lee²

2020

Journal of Astronomy and Space Sciences

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Properties of plasmas that constitute the plasma sheet in the near-Earth magnetotail vary according to the solar wind conditions and location in the tail. In this case study, we present multi-spacecraft observations by Cluster that show a transition of plasma sheet from cold, dense to hot, tenuous state. The transition was associated with the passage of a spatial boundary that separates the plasma sheet into two regions with cold, dense and hot, tenuous plasmas. Ion phase space distributions show that the cold, dense ions have a Kappa distribution while the hot, tenuous ions have a Maxwellian distribution, implying that they have different origins or are produced by different thermalization processes. The transition boundary separated the plasma sheet in the dawn-dusk direction, and slowly moved toward the dawn flank. The hot, tenuous plasmas filled the central region while the cold, dense plasmas filled the outer region. The hot, tenuous plasmas were moving toward the Earth, pushing the cold, dense plasmas toward the flank. Different types of dynamical processes can be generated in each region, which can affect the development of geomagnetic activities.

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Transport of transient solar wind particles in Earth’s cusps

Cited by 11 publications

References 24 publications

Turbulence in the Earth's cusp region: The k‐filtering analysis

Turbulence in the Earth's cusp region: The k‐filtering analysis

Evolution of the Earth's Polar Outflow From Mid‐Archean to Present

Observation of Transition Boundary between Cold, Dense and Hot, Tenuous Plasmas in the Near-Earth Magnetotail

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