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

Villante, U.; Francia, P.; Vellante, M.; Giuseppe, P. Di; Nubile, A.; Piersanti, Mirko

doi:10.1029/2006ja011896

Cited by 28 publications

(36 citation statements)

References 32 publications

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“…Their event occurred under a solar wind condition of stable northward IMF direction (almost tangential to the magnetopause), and high solar wind speed (620 km/sec). December 13 event was not associated with large solar wind disturbances as the event examined by Shimazu et al (1995) and other events examined by Villante et al (2007). Geomagnetic responses in low latitudes are essentially similar to events analyzed by them.…”

Section: December 13 1999supporting

confidence: 58%

“…Villante et al (2007) 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.…”

Section: December 13 1999mentioning

confidence: 99%

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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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Section: December 13 1999supporting

confidence: 58%

Section: December 13 1999mentioning

confidence: 99%

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

Kokubun

2013

Earth Planet Sp

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“…On the other hand, a clear correlation between the variations of the H component and the variations of the SW dynamical pressure on time scales of few minutes was found in a case study by Francia et al (1999). This aspect has been corroborated recently by Villante et al (2005b), who presented a joint analysis of SW, magnetospheric and ground observations, and showed that remarkable ground events at "selected" frequencies found a clear correspondence in the magnetospheric field at geostationary orbit, as well as in the SW density (and dynamical pressure). In addition, Kessel et al (2004) found ULF fluctuations in the Pc5 range in high speed streams, compressional in the leading edge and Alfvènic in the central region.…”

Section: Low Frequency Magnetospheric Modes During the Stormsupporting

confidence: 55%

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

Villante¹,

Vellante²,

Francia³

et al. 2006

Ann. Geophys.

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Abstract.We present an analysis of ULF geomagnetic field fluctuations at low latitudes during the first CAWSES campaign (29 March-3 April 2004). During the whole campaign, mainly in the prenoon sector, a moderate Pc3-4 pulsation activity is observed, clearly related to interplanetary upstream waves. On 3 April, in correspondence to the Earth's arrival of a coronal mass ejection, two SIs are observed whose waveforms are indicative of a contribution of the high-latitude ionospheric currents to the low-latitude ground field. During the following geomagnetic storm, low frequency (Pc5) waves are observed at discrete frequencies. Their correspondence with the same frequencies detected in the radial components of the interplanetary magnetic field and solar wind speed suggests that Alfvénic solar wind fluctuations may act as direct drivers of magnetospheric fluctuations. A cross-phase analysis, using different pairs of stations, is also presented for identifying field line resonant frequencies and monitoring changes in plasmaspheric mass density. Lastly, an analysis of ionospheric vertical soundings, measured at the Rome ionosonde station (41.8 • N, 12.5 • E), and vertical TEC measurements deduced from GPS signals within an European network shows the relation between the ULF resonances in the inner magnetosphere and thermal plasma density variations during geomagnetically quiet conditions, in contrast to various storm phases at the end of the CAWSES campaign.

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“…Other studies have shown similarities between individual discrete solar wind compressional oscillations and global magnetospheric pulsations observed in geosynchronous magnetic fields [Kepko and Spence, 2003] and in low latitude ground based magnetometer measurements [Villante et al, 2007]. Kessel et al [2004] reported that total Pc5 power of Alfvenic and compressional fluctuations in high speed solar wind streams was correlated with total Pc5 power of ground-based magnetic field pulsations.…”

Section: Introductionmentioning

confidence: 79%

“…Furthermore, during individual high speed events they observed discrete frequency ULF fluctuations in the 1 -4 mHz band in the solar wind but no one-to-one correspondence with the ground-based frequencies. Except for Villante et al [2007] who included some coherence spectra results, all of these studies have used frequency, amplitude, and direct time series comparisons. However, spectral cross-phase is an additional parameter which can be exploited.…”

Section: Introductionmentioning

confidence: 99%

Phase coherence analysis of a field line resonance and solar wind oscillation

Fenrich

Waters

2008

Geophysical Research Letters

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Discrete field line resonances (FLRs) are a common occurrence in the magnetosphere. However, the source of the stable, discrete FLR frequencies is still an unresolved problem. Recent work has proposed that discrete, continuous oscillations in the solar wind directly drive magnetospheric FLRs. However, these studies have only concentrated on common frequency and amplitude comparisons. This paper presents a new technique which utilizes either Fast Fourier Transform or wavelet cross‐phase measurements to demonstrate a high degree of phase coherence between a 1.7 mHz FLR observed with the SuperDARN Kodiak radar and ACE SWE oscillations in solar wind plasma density. A statistical analysis which simulates the solar wind as red noise indicates with 99% confidence that the FLR oscillation is the same as the solar wind plasma density variation.

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

Cited by 28 publications

References 32 publications

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

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

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

Phase coherence analysis of a field line resonance and solar wind oscillation

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