Magnetospheric MHD Oscillations - Anatoly Leonovich, Dmitri Klimushkin, Vitalii Mazur

Magnetospheric MHD Oscillations (eBook)

A Linear Theory

Anatoly Leonovich, Dmitri Klimushkin, Vitalii Mazur (Autoren)

eBook Download: EPUB

2024 | 1. Auflage
448 Seiten
Wiley-VCH (Verlag)
978-3-527-84575-0 (ISBN)

Magnetospheric MHD Oscillations

A groundbreaking new theory of the magnetosphere

The magnetosphere is the region around Earth in which our planet's magnetic field exerts its influence to trap charged particles. Waves in this magnetosphere, known as magnetohydrodynamic (MHD) oscillations, are caused by interactions between these charged particles, Solar wind pulses, and the magnetic field. The predictable interval between these oscillations enables them to serve as tools for understanding the magnetospheric plasma which comprises the field.

Magnetospheric MHD Oscillations offers a comprehensive overview of the theory underlying these waves and their periodicity. Emphasizing the spatial structure of the oscillations, it advances a theory of MHD oscillation that promises to have significant ramifications in astronomy and beyond.

Magnetospheric MHD Oscillations readers will also find:

Theorizing of direct relevance to current satellite missions, such as THEMIS and the Van Allen Probe
In-depth discussion of topics including Alfven resonance, waveguides in plasma filaments, and many more
Detailed appendices including key calculations and statistical parameters

Magnetospheric MDH Oscillations is ideal for plasma physicists, theoretical physicists, applied mathematicians, and advanced graduate students in these and related subfields.

Anatoly Leonovich, PhD, was a Researcher at the Insitute of Solar-Terrestrial Physics, Russian Academy of Science, Irkutsk, Russia. He researched and published widely on the theory of magnetospheric magnetohydrodynamic oscillations.

Vitalii Mazur, PhD, was a renowned theoretical physicist at the Irkutsk Institute of Solar-Terrestrial Physics and held, at the same time, a professorship at the Irkutsk State University, Russia. His research was focused on the theory of magnetohydrodynamic oscillations of the Earth's magnetosphere. He supervised numerous students, among them the coauthors of this book Anatoly Leonovich and Dmitri Klimushkin.

Dmitri Klimushkin, PhD, is a Researcher at the Institute of Solar-Terrestrial Physics, Russian Academy of Science, Irkutsk, Russia. His research focuses on the wave-particle interactions in the magnetosphere.

List of Figures

Figure 1.1 Friedrichs diagrams for the Alfvén (black), slow (light gray) and fast (dark gray) MHD modes for case when the Alfvén speed is greater than the speed of sound : (a) for the phase velocity and (b) for the group velocity . Here indices and mean projections on the direction parallel and perpendicular to the ambient magnetic field, respectively
Figure 1.2 Schematic of magnetic field oscillations (field lines), plasma pressure (shades of gray) and group velocity directions for Alfvén (a), fast magnetosonic (b) and slow magnetosonic (c) waves propagating in a homogeneous plasma
Figure 1.3 Relative SMS decrement vs. non‐isothermality, , of homogeneous plasma
Figure 1.4 Qualitative behaviour of the function in the complex plane as the argument varies from to
Figure 2.1 Model 1D‐inhomogeneous plasma (with density ) in a homogeneous magnetic field
Figure 2.2 Parallel structure of electric (black lines) and magnetic (gray lines) field of the MHD wave. Solid and dashed lines depict the fundamental () and second () harmonics, respectively
Figure 2.3 (a) Alfvén speed distribution along the axis in a 1D‐inhomogeneous model of the medium. (b) Dependence of the squared WKB component of the wave vector, , of MHD oscillations in a ‘cold’ plasma ( is the resonance point for Alfvén wave, is the turning point for FMS wave), (c) The structure of wave field components of MHD oscillations in a 1D‐inhomogeneous plasma
Figure 2.4 Spatial distribution of MHD oscillation ‐component (left‐hand axis) in the FMS wave which is incident to/reflected from the transition layer with an Alfvén resonance point. The gray line is the full oscillation field. WKB approximation: line 1 is FMS wave incident onto the transition layer, line 2 is FMS wave reflected from the transition layer. Oscillation hodographs for various points are shown above. The right‐hand axis line is Alfvén speed distribution
Figure 2.5 The dependence of the absorption coefficient for FMS waves incident onto the transition layer that are partially absorbed at the Alfvén resonance point. Distributions for various are shown. The black marginal curve, for , corresponds to an infinite layer with a linear profile. The dark gray dash lines show analytical distributions for two limiting cases: (1) and (2) , described by (2.21) and (2.23)
Figure 2.6 Evolution of an FMS wave packet incident onto a smooth transition layer containing an Alfvén resonance point, . The distribution of the Alfvén speed (right coordinate axis) and the component of the wave field (left coordinate axis) are shown. (a) Initial state of the unit‐wide wave packet. (b) Field structure at the moment the wave packet is reflected from the transition layer. (c) Wave packet structure upon reflection from the transition layer
Figure 2.7 Distributions of Alfvén speed , SMS wave speed (black lines, left‐hand axis) and the square of the WKB component of the wave vector, (gray lines, right‐hand axis), across the transition layer, in two limiting cases: (1) (solid gray line for ) the opaque region () is present for FMS waves, (2) (gray dashed line for ) the transparent region for SMS waves spreads from the resonance surface for SMS waves, , to infinity
Figure 2.8 Derivative distribution in the problem of FMS wave incident on/reflected from the transition layer with resonance surfaces for Alfvén () and SMS waves (). The gray line is the (numerically calculated) full oscillation field, (1) FMS wave incident on the transition layer, (2) FMS wave reflected from the transition layer (WKB approximation)
Figure 2.9 Distribution of MHD oscillation magnetic field components (Re()) in the problem of FMS wave incident on/reflected from the transition layer with resonance surfaces for Alfvén () and SMS waves ()
Figure 2.10 Hodograph behaviour for resonant MHD oscillations in the neighbourhood of resonance surfaces, and , for various decrements of Alfvén () and SMS oscillations. The curves and circles with hodograph rotation directions labelled 1,2 and 3, correspond to three values of SMS oscillation decrement: , and
Figure 2.11 Absorption coefficient dependence for FMS waves incident on the transition layer with two resonance surfaces: for Alfvén and SMS waves. The distributions are shown for the plasma layer (for waves with : curves for and curves for ) and the plasma layer (for : curves for and curves for )
Figure 2.12 Distribution of the real and imaginary parts of , a function of a real argument
Figure 2.13 Structure of MHD oscillations across magnetic shells when FMS waves are in resonance with kinetic Alfvén waves. The FMS wave amplitude decreases exponentially into the opaque region. In a ‘cold’ plasma (), a kinetic Alfvén wave is excited on the resonance magnetic shell and travels away leftwards, while in a ‘warm’ plasma (), an Alfvén wave travels away rightwards from the resonance shell
Figure 2.14 Potential in (2.79) for quasi‐parallel MHD oscillations: (a) the form of potential with Alfvén resonance points () for waveguide FMS oscillations (); (b) potential for waveguide‐travelling quasi‐parallel Alfvén waves ()
Figure 2.15 The structure of waveguide modes in the potential decaying as the related MHD waves escape. Top: waveguide FMS mode and related escaping kinetic Alfvén wave (A2) (see Figure A.1, (a) in Appendix A); bottom: waveguide mode of kinetic Alfvén waves that decays due to the FMS wave escaping from the waveguide
Figure 2.16 Graphic solution of dispersion Eqs. (2.122), (2.123). Curves I correspond to the right side of (2.122), and curves II to the right side of (2.123)
Figure 2.17 Alfvén speed distribution in the dayside magnetosphere (gray scale). distribution is shown in the meridional section inside the plasmapause and in the plasma filament (duct for MHD waves) in the outer magnetosphere. Smaller are shown by light gray. The white arrows indicate the direction of the FMS group velocity in the meridional section
Figure 2.18 Schematic representation of a magnetospheric duct model in a cylindric system of coordinates (): (a) direction of outer magnetic field and plasma density distribution in a plasma filament; (b) the form of the potential in (2.128)
Figure 2.19 Model medium and coordinate system. Roman numbers indicate the following regions: – solar wind, – magnetosphere. FMS waves are labelled as: 1 – incident on the magnetosphere, 2 – reflected from the magnetopause, 3 – penetrating into the magnetosphere
Figure 2.20 The dependence of function for fixed and . (a) – in the magnetosphere, the points labelled: 1 – , 2 – , 3 – . (b) – in the solar wind, the points labelled: 1 – , 2 – , 3 – , 4 – , 5 – , 6 –
Figure 2.21 The characteristic form of the dependencies of the relative densities of monochromatic FMS energy fluxes in the solar wind and in the magnetosphere, in the sector. Energy flux densities are labelled as: 1 – FMS wave incident to the magnetopause; 2 – wave reflected from the magnetopause; 3 – wave penetrating into the magnetosphere
Figure 2.22 Total energy transferred into the magnetosphere by the ‘geoeffective’ FMS flux over time s vs. the geotail growth rate index in the model Eq. (2.168)
Figure 2.23 Model medium and coordinate system: is the characteristic scale of the shear layer, is the location of possible boundaries in the form of rigid walls, , are the unperturbed speed and background magnetic field vectors, is the tangential wave vector of the oscillations
Figure 2.24 Growth rate () isoline distribution for MHD oscillations with generated by a shear flow in the form of a smooth transition layer in a boundless medium, for two values of : (a) , (b)
Figure 2.25 Growth rate () isoline distribution for MHD oscillations with generated by a shear flow in the form of a smooth transition layer in a boundless medium
Figure 2.26 Growth rate distribution of MHD oscillations with for a shear flow in the form of a tangential discontinuity bounded by a rigid wall on one side, for different values of parameters and : (a) , plots 1–5 refer to ; (b) , plots 1–5 refer to
Figure 2.27 Growth rate isoline distribution for MHD oscillations with for a shear flow with a smooth transition layer bounded by a rigid wall () on one side, for two different values of parameter : (a) – , (b) –
Figure 2.28 Growth rate isoline distribution for MHD oscillations with for a shear flow with a smooth transition layer bounded by a rigid wall on one side (). Thick lines correspond to the surface and radiative oscillation modes, thin lines to the oscillation...

Erscheint lt. Verlag	2.4.2024
Sprache	englisch
Themenwelt	Naturwissenschaften ► Physik / Astronomie ► Astronomie / Astrophysik
ISBN-10	3-527-84575-5 / 3527845755
ISBN-13	978-3-527-84575-0 / 9783527845750

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