Polar cap boundary layer waves: An auroral zone phenomenon

Bruce T. Tsurutani, John K. Arballo, Carlos Galvan, Liwei Dennis Zhang, Xiao Yan Zhou, Gurbax S. Lakhina, Tohru Hada, Jolene S. Pickett, Donald A. Gurnett

    Research output: Contribution to journalArticle

    12 Citations (Scopus)

    Abstract

    Polar cap boundary layer waves are ELF/VLF electric and magnetic waves detected on field lines just adjacent to the polar cap. Intense waves are present at this location essentially all (96%) of the time. The wave latitude-local time distribution is shown to be the same as that of the Feldstein auroral oval, a distribution centered at ∼75° at local noon and ∼65° at local midnight. The most intense waves are detected coincident with the strongest magnetic field gradients (field-aligned currents). Statistically, the wave intensities are greatest near local noon (10-13 mV2 m-1 at 3 kHz) and midnight and are least near dawn and dusk (∼5 × 10-15 mV2 m-1 at 3 kHz). The noon and midnight wave intensities increase slightly when the interplanetary magnetic field is directed southward. The dawn and dusk waves appear to be controlled by the solar wind speed. Using high-resolution data, specific frequency bands of electromagnetic whistler-mode waves are identified: ∼200 Hz and 1-2 and ∼5 kHz. These may correspond to previously identified "magnetic noise bursts" and "auroral hiss", respectively. Assuming cyclotron resonant interactions, the 1- to 5-kHz auroral hiss is shown to be resonant with ∼50-eV to ∼1.0-keV electrons. Several mechanisms, both resonant (nonlocal) and nonresonant (local), are suggested for the generation of the ∼200-Hz electromagnetic waves. Three types of intense electric signals are present: solitary bipolar pulses (electron holes), waves at ∼4 × 102 to 6 × 103 Hz (lower hybrid waves), and narrowband waves at ∼10 kHz (electrostatic waves near the upper hybrid resonance frequency). Solitary bipolar pulse onset events have been detected for the first time. The bipolar pulses reached 2 mV m-1 peak-to-peak amplitudes within 3 ms. An exponential growth rate of 0.72 ms, or 0.25 fce, was determined. The previously reported "broadband nature" of the polar cap boundary layer (and low-latitude boundary layer) waves is now postulated to be caused by a fast switching between the various electromagnetic and electrostatic modes described above. The polar cap boundary layer waves are most likely a consequence of instabilities associated with auroral zone field-aligned currents carried by 50-eV to 1.0-keV electrons and protons. The currents in turn have been ascribed to be driven by the solar wind-magnetosphere global interaction. One consequence of the presence of the waves at high altitudes is diffusion of magnetosheath plasma into the magnetosphere and magnetospheric plasma out into the magnetosheath (cross-field diffusion, due to parasitic wave-particle interactions). It is speculated that field-aligned currents and similar wave modes will be detected at all planetary magnetospheres.

    Original languageEnglish
    Article number2000JA003007
    Pages (from-to)19035-19055
    Number of pages21
    JournalJournal of Geophysical Research: Space Physics
    Volume106
    Issue numberA9
    Publication statusPublished - Sep 1 2001

    Fingerprint

    auroral zones
    polar caps
    boundary layers
    Boundary layers
    boundary layer
    electrons
    magnetic fields
    wind speed
    protons
    field aligned currents
    noon
    Magnetosphere
    hiss
    magnetosheath
    magnetosphere
    Solar wind
    magnetospheres
    solar wind
    electron
    Electrons

    All Science Journal Classification (ASJC) codes

    • Geophysics
    • Forestry
    • Oceanography
    • Aquatic Science
    • Ecology
    • Water Science and Technology
    • Soil Science
    • Geochemistry and Petrology
    • Earth-Surface Processes
    • Atmospheric Science
    • Earth and Planetary Sciences (miscellaneous)
    • Space and Planetary Science
    • Palaeontology

    Cite this

    Tsurutani, B. T., Arballo, J. K., Galvan, C., Zhang, L. D., Zhou, X. Y., Lakhina, G. S., ... Gurnett, D. A. (2001). Polar cap boundary layer waves: An auroral zone phenomenon. Journal of Geophysical Research: Space Physics, 106(A9), 19035-19055. [2000JA003007].

    Polar cap boundary layer waves : An auroral zone phenomenon. / Tsurutani, Bruce T.; Arballo, John K.; Galvan, Carlos; Zhang, Liwei Dennis; Zhou, Xiao Yan; Lakhina, Gurbax S.; Hada, Tohru; Pickett, Jolene S.; Gurnett, Donald A.

    In: Journal of Geophysical Research: Space Physics, Vol. 106, No. A9, 2000JA003007, 01.09.2001, p. 19035-19055.

    Research output: Contribution to journalArticle

    Tsurutani, BT, Arballo, JK, Galvan, C, Zhang, LD, Zhou, XY, Lakhina, GS, Hada, T, Pickett, JS & Gurnett, DA 2001, 'Polar cap boundary layer waves: An auroral zone phenomenon', Journal of Geophysical Research: Space Physics, vol. 106, no. A9, 2000JA003007, pp. 19035-19055.
    Tsurutani BT, Arballo JK, Galvan C, Zhang LD, Zhou XY, Lakhina GS et al. Polar cap boundary layer waves: An auroral zone phenomenon. Journal of Geophysical Research: Space Physics. 2001 Sep 1;106(A9):19035-19055. 2000JA003007.
    Tsurutani, Bruce T. ; Arballo, John K. ; Galvan, Carlos ; Zhang, Liwei Dennis ; Zhou, Xiao Yan ; Lakhina, Gurbax S. ; Hada, Tohru ; Pickett, Jolene S. ; Gurnett, Donald A. / Polar cap boundary layer waves : An auroral zone phenomenon. In: Journal of Geophysical Research: Space Physics. 2001 ; Vol. 106, No. A9. pp. 19035-19055.
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    abstract = "Polar cap boundary layer waves are ELF/VLF electric and magnetic waves detected on field lines just adjacent to the polar cap. Intense waves are present at this location essentially all (96{\%}) of the time. The wave latitude-local time distribution is shown to be the same as that of the Feldstein auroral oval, a distribution centered at ∼75° at local noon and ∼65° at local midnight. The most intense waves are detected coincident with the strongest magnetic field gradients (field-aligned currents). Statistically, the wave intensities are greatest near local noon (10-13 mV2 m-1 at 3 kHz) and midnight and are least near dawn and dusk (∼5 × 10-15 mV2 m-1 at 3 kHz). The noon and midnight wave intensities increase slightly when the interplanetary magnetic field is directed southward. The dawn and dusk waves appear to be controlled by the solar wind speed. Using high-resolution data, specific frequency bands of electromagnetic whistler-mode waves are identified: ∼200 Hz and 1-2 and ∼5 kHz. These may correspond to previously identified {"}magnetic noise bursts{"} and {"}auroral hiss{"}, respectively. Assuming cyclotron resonant interactions, the 1- to 5-kHz auroral hiss is shown to be resonant with ∼50-eV to ∼1.0-keV electrons. Several mechanisms, both resonant (nonlocal) and nonresonant (local), are suggested for the generation of the ∼200-Hz electromagnetic waves. Three types of intense electric signals are present: solitary bipolar pulses (electron holes), waves at ∼4 × 102 to 6 × 103 Hz (lower hybrid waves), and narrowband waves at ∼10 kHz (electrostatic waves near the upper hybrid resonance frequency). Solitary bipolar pulse onset events have been detected for the first time. The bipolar pulses reached 2 mV m-1 peak-to-peak amplitudes within 3 ms. An exponential growth rate of 0.72 ms, or 0.25 fce, was determined. The previously reported {"}broadband nature{"} of the polar cap boundary layer (and low-latitude boundary layer) waves is now postulated to be caused by a fast switching between the various electromagnetic and electrostatic modes described above. The polar cap boundary layer waves are most likely a consequence of instabilities associated with auroral zone field-aligned currents carried by 50-eV to 1.0-keV electrons and protons. The currents in turn have been ascribed to be driven by the solar wind-magnetosphere global interaction. One consequence of the presence of the waves at high altitudes is diffusion of magnetosheath plasma into the magnetosphere and magnetospheric plasma out into the magnetosheath (cross-field diffusion, due to parasitic wave-particle interactions). It is speculated that field-aligned currents and similar wave modes will be detected at all planetary magnetospheres.",
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    N2 - Polar cap boundary layer waves are ELF/VLF electric and magnetic waves detected on field lines just adjacent to the polar cap. Intense waves are present at this location essentially all (96%) of the time. The wave latitude-local time distribution is shown to be the same as that of the Feldstein auroral oval, a distribution centered at ∼75° at local noon and ∼65° at local midnight. The most intense waves are detected coincident with the strongest magnetic field gradients (field-aligned currents). Statistically, the wave intensities are greatest near local noon (10-13 mV2 m-1 at 3 kHz) and midnight and are least near dawn and dusk (∼5 × 10-15 mV2 m-1 at 3 kHz). The noon and midnight wave intensities increase slightly when the interplanetary magnetic field is directed southward. The dawn and dusk waves appear to be controlled by the solar wind speed. Using high-resolution data, specific frequency bands of electromagnetic whistler-mode waves are identified: ∼200 Hz and 1-2 and ∼5 kHz. These may correspond to previously identified "magnetic noise bursts" and "auroral hiss", respectively. Assuming cyclotron resonant interactions, the 1- to 5-kHz auroral hiss is shown to be resonant with ∼50-eV to ∼1.0-keV electrons. Several mechanisms, both resonant (nonlocal) and nonresonant (local), are suggested for the generation of the ∼200-Hz electromagnetic waves. Three types of intense electric signals are present: solitary bipolar pulses (electron holes), waves at ∼4 × 102 to 6 × 103 Hz (lower hybrid waves), and narrowband waves at ∼10 kHz (electrostatic waves near the upper hybrid resonance frequency). Solitary bipolar pulse onset events have been detected for the first time. The bipolar pulses reached 2 mV m-1 peak-to-peak amplitudes within 3 ms. An exponential growth rate of 0.72 ms, or 0.25 fce, was determined. The previously reported "broadband nature" of the polar cap boundary layer (and low-latitude boundary layer) waves is now postulated to be caused by a fast switching between the various electromagnetic and electrostatic modes described above. The polar cap boundary layer waves are most likely a consequence of instabilities associated with auroral zone field-aligned currents carried by 50-eV to 1.0-keV electrons and protons. The currents in turn have been ascribed to be driven by the solar wind-magnetosphere global interaction. One consequence of the presence of the waves at high altitudes is diffusion of magnetosheath plasma into the magnetosphere and magnetospheric plasma out into the magnetosheath (cross-field diffusion, due to parasitic wave-particle interactions). It is speculated that field-aligned currents and similar wave modes will be detected at all planetary magnetospheres.

    AB - Polar cap boundary layer waves are ELF/VLF electric and magnetic waves detected on field lines just adjacent to the polar cap. Intense waves are present at this location essentially all (96%) of the time. The wave latitude-local time distribution is shown to be the same as that of the Feldstein auroral oval, a distribution centered at ∼75° at local noon and ∼65° at local midnight. The most intense waves are detected coincident with the strongest magnetic field gradients (field-aligned currents). Statistically, the wave intensities are greatest near local noon (10-13 mV2 m-1 at 3 kHz) and midnight and are least near dawn and dusk (∼5 × 10-15 mV2 m-1 at 3 kHz). The noon and midnight wave intensities increase slightly when the interplanetary magnetic field is directed southward. The dawn and dusk waves appear to be controlled by the solar wind speed. Using high-resolution data, specific frequency bands of electromagnetic whistler-mode waves are identified: ∼200 Hz and 1-2 and ∼5 kHz. These may correspond to previously identified "magnetic noise bursts" and "auroral hiss", respectively. Assuming cyclotron resonant interactions, the 1- to 5-kHz auroral hiss is shown to be resonant with ∼50-eV to ∼1.0-keV electrons. Several mechanisms, both resonant (nonlocal) and nonresonant (local), are suggested for the generation of the ∼200-Hz electromagnetic waves. Three types of intense electric signals are present: solitary bipolar pulses (electron holes), waves at ∼4 × 102 to 6 × 103 Hz (lower hybrid waves), and narrowband waves at ∼10 kHz (electrostatic waves near the upper hybrid resonance frequency). Solitary bipolar pulse onset events have been detected for the first time. The bipolar pulses reached 2 mV m-1 peak-to-peak amplitudes within 3 ms. An exponential growth rate of 0.72 ms, or 0.25 fce, was determined. The previously reported "broadband nature" of the polar cap boundary layer (and low-latitude boundary layer) waves is now postulated to be caused by a fast switching between the various electromagnetic and electrostatic modes described above. The polar cap boundary layer waves are most likely a consequence of instabilities associated with auroral zone field-aligned currents carried by 50-eV to 1.0-keV electrons and protons. The currents in turn have been ascribed to be driven by the solar wind-magnetosphere global interaction. One consequence of the presence of the waves at high altitudes is diffusion of magnetosheath plasma into the magnetosphere and magnetospheric plasma out into the magnetosheath (cross-field diffusion, due to parasitic wave-particle interactions). It is speculated that field-aligned currents and similar wave modes will be detected at all planetary magnetospheres.

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