ULF fluctuations of the geomagnetic field and ionospheric sounding measurements at low latitudes during the first CAWSES campaign

Villante, U.; Vellante, M.; Francia, P.; Lauretis, M. De; Meloni, A.; Palangio, P.; Zolesi, B.; Pezzopane, Michael; Förster, M.; Zhang, T. L.; Magnes, W.; Nenovski, P.; Cholakov, Iliya; Wesztergom, Viktor

doi:10.5194/angeo-24-1455-2006

Cited by 17 publications

(18 citation statements)

References 62 publications

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“…Additionally, the electron density of the ionosphere increased and then gradually recovered to the original level, which is a typical case of plasmasphere depletion in response to the solar wind dynamic pressure pulsation during a geomagnetically quiet period. This result is consistent with the findings that the plasmaspheric density decreased at mid-and low-latitude during the magnetic storm proposed by Chi et al [2] and Villante et al [15] and our previous result that showed a corresponding decrease of the plasmaspheric density during moderate magnetic storm events in 2011.…”

Section: Summary and Discussionsupporting

confidence: 93%

Plasma transport between the ionosphere and plasmasphere in response to solar wind dynamic pressure pulsation

Zhang

Wang

et al. 2013

Chin. Sci. Bull.

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The plasma transport between the plasmasphere and the ionosphere in response to the interplanetary conditions is still not fully understood until now. Simultaneous observations of the plasmasphere and ionosphere from the newly developed Chinese Meridian Project provide a new opportunity for understanding the characteristic of the plasma transport and the coupling mechanism between these two regions. We investigate the response of the plasmasphere (L≈2) and ionosphere to the solar wind dynamic pressure pulse during geomagnetically quiet period of 21-27 March 2011. The response of the plasmasphere shows a significant depletion. The plasmaspheric density nearly decreases by half in response to the solar wind dynamic pressure pulse, and subsequently recovers to the original level in 1-2 d. Meanwhile, the maximum electron density of the ionospheric F2 layer (NmF2) and the total electron content (TEC) increase by 13% and 21%, respectively, and then gradually recover, which is opposite to the behavior during magnetic storms. Preliminary analysis shows that the plasmaspheric depletion may be mainly caused by the southward interplanetary magnetic field and changing dawn-dusk electric field. The plasmaspheric density variations seem to be controlled by both the IMF and ionospheric conditions. solar wind dynamic pressure, ionosphere, plasmasphere, southward IMF, dawn-dusk electric field Citation:Zhang Q M, Wang C, Li H, et al. Plasma transport between the ionosphere and plasmasphere in response to solar wind dynamic pressure pulsation. Chin Sci Bull, 2013, 58: 41264132,

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Section: Summary and Discussionsupporting

confidence: 93%

Plasma transport between the ionosphere and plasmasphere in response to solar wind dynamic pressure pulsation

Zhang

Wang

et al. 2013

Chin. Sci. Bull.

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“…On the other hand, as noted earlier, the correspondence between spectral enhancements in the magnetospheric field and SW density led Kepko et al [2002] and Kepko and Spence [2003] to interpret the discrete frequencies in terms of an inherent property of the SW, not related to cavity or waveguide modes of the magnetosphere. Recently, Villante et al [2006] presented a case in which power enhancements ( f ≈ 1.4, 2.5, and 4.2 mHz) simultaneously occurred in the H component as well as in the radial component of the SW speed and IMF, while the SW density showed minor enhancements at different frequencies; they speculated, in that case, noncompressive “Alfvénic” fluctuations as possible drivers of geomagnetic field fluctuations at discrete frequencies.…”

Section: Summary and Discussionmentioning

confidence: 99%

Long‐period oscillations at discrete frequencies: A comparative analysis of ground, magnetospheric, and interplanetary observations

et al. 2007

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[1] The power spectra of remarkable events of long-period fluctuations of the geomagnetic field (as identified at a low-latitude station, L'Aquila, l % 36°) reveal a tendency for a repeated occurrence of power enhancements in the same frequency bands (f % 0.9-1.0, 1.2-1.4, 2.1-2.3, 2.5-2.7 mHz), often coincident with CMS frequencies. In four cases the data availability and the results of the spectral analysis allowed unambiguous conclusions on the correspondence between ground, magnetospheric, and solar wind fluctuations. For most wave packets, the comparative analysis reveals an unprecedented one-to-one correspondence in terms of frequency, onset, and duration; it suggests that geomagnetic fluctuations can be driven directly by fluctuations of the solar wind density at the same frequencies. On the other hand, the repeated occurrence in the same frequency bands and some evidence for amplification processes suggest additional contributions possibly related with cavity/waveguide resonances.Citation: Villante, U., P. Francia, M. Vellante, P. Di Giuseppe, A. Nubile, and M. Piersanti (2007), Long-period oscillations at discrete frequencies: A comparative analysis of ground, magnetospheric, and interplanetary observations,

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“…Though it is needed to further examine conditions to relate IMF fluctuations to magnetospheric variations, it is suggested that IMF Alfvénic fluctuations is an important source for the excitation of magnetospheric waves. Villante et al (2006) also speculated that Alfvénic fluctuations as possible drivers of geomagnetic field fluctuations at discrete frequencies.…”

Section: Discussionmentioning

confidence: 99%

“…As for IMF changes, multiple spectral peaks at 1.7, 2.1, 2.7 and 3.7 mHz were noted, which roughly correspond to those of magnetospheric oscillations. Villante et al (2006) have presented a case in which power enhancements (at 1.4, 2.5, and 4.2 mHz) simultaneously occurred in the H component on the low latitude ground as well as in the radial component of the SW speed and IMF, while the SW density showed minor enhancements at different frequencies. This observation is essentially similar to the case discussed above.…”

Section: August 20 1999mentioning

confidence: 99%

ULF waves in the outer magnetosphere: Geotail observation 1 transverse waves

Kokubun

2013

Earth Planet Sp

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A survey of ULF waves in the Pc 5 frequency range during the six year period (1995)(1996)(1997)(1998)(1999)(2000) has been made for the field line resonance waves in the outer magnetosphere, using plasma flow and magnetic field measurements with the Geotail spacecraft. On the morning side a series of wave trains often appears during several hours. In contrast such a series of wave trains with a long duration is rarely observed in the afternoon to evening sector. Most of waves in the afternoon sector are isolated, of which duration is approximately one hour. The existence of a set of preferential frequencies and the pronounced dawn-dusk asymmetry of wave occurrence and wave features, which were found in ground-based and ionospheric measurements of geomagnetic ULF pulsations, were statistically confirmed. It is also noted that the background plasma flow is sunward in the evening sector without exception. Transverse waves are generally observed in the condition of plasma β below 1.5. High β cases are mostly associated with events on the dusk side. As for the relation to solar wind conditions, Pc 5 waves tend to occur under the condition of more radial than the average IMF spiral angle, or of low cone angle.

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ULF fluctuations of the geomagnetic field and ionospheric sounding measurements at low latitudes during the first CAWSES campaign

Cited by 17 publications

References 62 publications

Plasma transport between the ionosphere and plasmasphere in response to solar wind dynamic pressure pulsation

Plasma transport between the ionosphere and plasmasphere in response to solar wind dynamic pressure pulsation

Long‐period oscillations at discrete frequencies: A comparative analysis of ground, magnetospheric, and interplanetary observations

ULF waves in the outer magnetosphere: Geotail observation 1 transverse waves

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