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A statistical correlation of Pc5 pulsations and solar wind pressure oscillations
KTH, School of Electrical Engineering (EES), Centres, Alfvén Laboratory Centre for Space and Fusion Plasma Physics.
School of Pure and Applied Physics, University of KwaZulu-Natal, Durban, South Africa.
School of Pure and Applied Physics, University of KwaZulu-Natal, Durban, South Africa.
2006 (English)In: Advances in Space Research, ISSN 0273-1177, Vol. 38, no 8, 1763-1771 p.Article in journal (Refereed) Published
Abstract [en]

The SHARE high frequency (HF) radar in Antarctica is used to compare ionospheric plasma flow oscillations in the Pc5 frequency range with low-frequency oscillations in the solar wind pressure measured by the ACE spacecraft. Ten different days in 2000 and 2001 are analysed with respect to different frequencies and geomagnetic latitudes. Both data sets are bandpass filtered and a complex demodulation technique is used to calculate the correlation in each band. On a number of occasions the wave packet structure of the Pc5 pulsations is in good or excellent agreement with the wave packet structure of the solar wind pressure oscillations. This strongly suggests that the oscillations were directly driven by the solar wind. Particularly good correlation is found in the frequency band 0.8-1.2 mHz. Pulsations in this frequency range are hard to reconcile with the magnetospheric cavity mode model. We conclude that, at least on some occasions, Pc5 pulsations may be directly driven and the magnetosphere cavity/waveguide then assumes a more passive role.

Place, publisher, year, edition, pages
2006. Vol. 38, no 8, 1763-1771 p.
Keyword [en]
ULF waves; Pc5 pulsations; solar wind waves; magnetospheric waveguide
National Category
Fusion, Plasma and Space Physics
Identifiers
URN: urn:nbn:se:kth:diva-5812DOI: 10.1016/j.asr.2005.08.023ISI: 000202988500029Scopus ID: 2-s2.0-33845982221OAI: oai:DiVA.org:kth-5812DiVA: diva2:10318
Note

QC 20100707. Uppdaterad från Accepted till Published 2010707. Konferens: 35th COSPAR Scientific Assembly Paris, FRANCE, JUL 18-25, 2004 Comm Space Res

Available from: 2005-08-25 Created: 2005-08-25 Last updated: 2012-09-17Bibliographically approved
In thesis
1. Resonant Waves in the Terrestrial Magnetosphere
Open this publication in new window or tab >>Resonant Waves in the Terrestrial Magnetosphere
2005 (English)Licentiate thesis, comprehensive summary (Other scientific)
Abstract [en]

Waves in the mHz frequency range are a prominent feature in the terrestrial magnetosphere. In this frequency range the waves have wavelengths comparable to the lengths of the geomagnetic field lines. The waves are then standing waves along closed field lines with endpoints in the southern and northern ionosphere. Waves play an important role in the distribution of energy in the magnetosphere and mHz waves can accelerate electrons to MeV energies and have been proposed as a driver of auroral arcs. They can also be used as a diagnostic tool for determining the plasma density. There are two important classes of these low frequency waves. One has large azimuthal wavelength and is usually associated with driving mechanisms outside the magnetosphere, such as the Kelvin-Helmholtz instability at the magnetopause. The other has small azimuthal wavelength and is associated with plasma instabilities inside the magnetosphere. Both types of waves are studied in this thesis with an emphasis on the small azimuthal wavelength waves. For the type of wave with large azimuthal wavelength there is however, a considerable debate about the driving mechanism. One recently suggested driver is coherent magnetohydrodynamic waves in the solar wind. Part of this thesis studies this experimentally and we conclude that, at least on some occasions, this driving mechanism come into play. The Cluster satellites are used to study the morphology of the waves. We demonstrate the ability of Cluster to determine the azimuthal wave number of the waves and also how the structure along the magnetic field lines can be determined. This gives information regarding the harmonic number of the standing waves, which in turn says something about the driver of the waves. We also look at possible excitation mechanisms for the small azimuthal wavelength waves.

Place, publisher, year, edition, pages
Stockholm: KTH, 2005. xi, 45 p.
Series
Trita-ALP, ISSN 1103-6613 ; 2005:05
National Category
Fusion, Plasma and Space Physics
Identifiers
urn:nbn:se:kth:diva-400 (URN)91-7178-105-6 (ISBN)
Presentation
2005-09-12, Seminarierummet, Teknikringen 31, Stockholm, 13:00
Opponent
Supervisors
Note
QC 20101129Available from: 2005-08-25 Created: 2005-08-25 Last updated: 2010-11-29Bibliographically approved
2. Multi-point Measurements of Ultra Low Frequency Waves in the Terrestrial Magnetosphere
Open this publication in new window or tab >>Multi-point Measurements of Ultra Low Frequency Waves in the Terrestrial Magnetosphere
2007 (English)Doctoral thesis, comprehensive summary (Other scientific)
Abstract [en]

Waves in the mHz frequency range are prominent features of the terrestrial magnetosphere. In this frequency range the waves have wavelengths comparable to the lengths of the geomagnetic field lines. The waves are then standing waves along closed field lines with endpoints in the southern and northern ionosphere. Waves play an important role in the distribution of energy in the magnetosphere and mHz waves can accelerate electrons to MeV energies and have been proposed as driving mechanism for auroral arcs. They can also be used as diagnostic tools for determining the plasma density. There are two important classes of these low frequency waves. One has large azimuthal wavelength and is usually associated with driving mechanisms outside the magnetosphere, such as the Kelvin-Helmholtz instability at the magnetopause. The other has small azimuthal wavelength and is associated with plasma instabilities inside the magnetosphere. Both types of waves are studied in this thesis with a slight emphasis on the large azimuthal wavelength waves. For the type of wave with large azimuthal wavelength there is however, a considerable debate about the driving mechanism. One recently suggested driver is coherent magnetohydrodynamic waves in the solar wind. Part of this thesis studies this experimentally and we conclude that, at least on some occasions, this driving mechanism comes into play. The Cluster satellites are used to study the morphology of the waves. We demonstrate the ability of Cluster to determine the azimuthal wave number of the waves and also how the structure along the magnetic field lines can be determined. This gives information regarding the harmonic number of the standing waves, which in turn says something about the driver of the waves. We also look at possible excitation mechanisms for the small azimuthal wavelength waves.

Place, publisher, year, edition, pages
Stockholm: KTH, 2007. xi, 52 p.
Series
Trita-EE, ISSN 1653-5146 ; 2007:014
National Category
Fusion, Plasma and Space Physics
Identifiers
urn:nbn:se:kth:diva-4404 (URN)978-91-7178-615-9 (ISBN)
Public defence
2007-06-08, Sal F3, KTH, Lindstedtsvägen 26, Stockhol, 10:00
Opponent
Supervisors
Note
QC 20100707Available from: 2007-05-29 Created: 2007-05-29 Last updated: 2010-07-07Bibliographically approved

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