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'Goescience Connections' in Braga Science Film Fest

The IUGG funded short documentary 'Geoscience Connections' that showcases the evolution of Earth with an analogy of human growth is all set to premier at the Braga Science Film Festival. The movie focusses on the science that is covered under the IUGG umbrella by its 8 different associations.

The festival is online from 18th to 26th November and free! Also, don't forget to vote for Geoscience Connections for the Audience Award! The movie can be found online at the IUGG channel as well.

Keep a look out at the IAGA and IUGG YouTube channels for an updated version of the movie where early career scientists from the 8 associations talk about the science that happens in the interior and on the surface and beyond.

Learn more about this outreach project as well as others here.

Debunking a Pillar of Ionospheric Science, and Building a New One: Episode I

Dear reader, I’m excited to try this non-traditional strategy, the thing they call a blog (honestly!), to tell you about my research into the foundations of ionospheric physics. But I suppose I should first tell you who is talking. After listening to Joan Baez sing at my elementary school, protesting the war in San Francisco with my mother, climbing over a fence because she was scared of the batons, swimming naked in a river with my entire 8th grade class, shocking the head of the math department at Palo Alto High School, working as a carpenter, out of a Volkswagen Bug, having my Fiat pulled out of a ditch by the man who made the first computer mouse (Figure 2 below) in his garage, designing my own religion, seeing people die who shouldn’t have died, working as a microwave engineer, marrying a much more conservative Chinese woman, having it work out, earning a Ph.D. in quantum gravity, and becoming the father of two hims, each amazing in their own way, I found myself trying to break into the field of ionospheric physics as a compromise approach to earning a living— at that same research lab where that wooden computer mouse arrived the next morning for testing (SRI International, where I have worked for 23 years).

Although I didn’t have time to worry about it back then, I noticed that while the magnetospheric people were all about MHD waves, there was no talk of what became of these waves when they entered the ionosphere. In the ionosphere, it was all about electrostatic theory, which made things very simple and easy. After spending a little while looking for an explanation, I quickly gave up. Quite a few years passed before I realized that I might actually be able to bridge this gap. My 2016 paper got great reviews, but was met with a deafening silence. My second paper did not get great reviews. I suspect a few of those referees had to be rushed directly to the hospital. Thank you to those few who supported me! But since I am given confidence by my rigorous education in physics and mathematics, and since the negative reviews were just sour grapes, it’s blogs away. You might now notice a slight change in tone.

The interaction of the magnetosphere with the ionosphere and atmosphere involves electromagnetic energy incident from the magnetosphere (for example as shown in Figure 1 on top left), which is output from an empirical Poynting flux model made from FAST satellite data (Cosgrove et al., 2014). The energy is dissipated by means of currents that flow through the ionospheric conductance, which arises because of the high rate of collisions with the neutral atmosphere, so that the currents cause heating and acceleration of the atmosphere. Various effects flow from this, with a particularly notable one being disruption of satellite orbits. Thus, it is important that we understand the physics that gives rise to the ionospheric conductance, which forms the inner boundary for magnetospheric modelling.

The ionospheric conductance has heretofore been calculated using a form of electrostatic theory that is very close to the textbook theory, where all time derivatives are set to zero and what remains of the equations of motion are applied to a boundary value problem. But since electrostatic theory is not valid in all cases, it is important to ask if we can show that it is valid for this ionospheric application, or, if not, to derive an electromagnetic calculation that can replace it.

The transition between electromagnetics and electrostatics is addressed in the transmission line theory of electrical engineering. Consider the simple “lumped element” circuit shown in the top panel of Figure 3, consisting of a switched harmonic source with internal resistance, driving a capacitor. In order to be properly causal, this circuit is generally analyzed by taking the Laplace transform in time, which provides a solution as a sum of steady-state and transient terms. In many cases we are only interested in the steady-state part, which leaves the usual idea of a capacitive admittance operating in a harmonic circuit (Yin iω0C, a positive imaginary number).

The terminology “lumped element” indicates that we are considering the capacitor to be very small, so that it doesn’t matter where the electrical connections are made to the parallel plates, and we can assume that the capacitor energizes everywhere all-at-once. But in reality when the switch is flipped, there is an electromagnetic signal that enters the capacitor on the side with the electrical leads, and then propagates across to the other edges, and bounces around until a steady state is reached. And depending on the size of the capacitor, there may be a portion of a wavelength inside the capacitor. When this happens the lumped element (electrostatic) analysis is too idealized to be of use.

To understand how this effect can be accommodated, consider the case of a capacitor that is long and thin, with the leads attached at the near end. Assuming that the signal cannot leak out and radiate away, this long and thin structure is a transmission line that is open-circuited at the far end. The signal propagates from the electrical leads to the far end where it reflects back, and then continues bouncing back and forth until a steady state is reached. Assuming there is only one propagating electromagnetic mode, the steady-state amounts to a superposition of two oppositely propagating waves, which are phased so that the current is zero at the open-circuited end.

From this description can be derived the well known formula for the steady-state input admittance seen by the source, which may be found, for example, in equation 3.88 from Collin (1966), and setting the load admittance to zero,where l is the length of the transmission line, Y0 is the characteristic admittance of the wave mode, and kz is the wavevector in the direction along the line (i.e., in the “parallel” or z direction). A schematic for the circuit with the open-circuited transmission line replacing the lumped-element capacitor is shown in the middle panel of Figure 3.

Since Y0 is usually a real number, the formula (1) provides that when the transmission line is short and the waves are not too lossy (i.e., kz is strongly real), then it does in fact function as a capacitor with admittance iY0kzl. But as the line gets longer the tangent function causes an oscillation between capacitive and inductive behavior, with near singularities where real(kz)l is a multiple of 90°. The singularities arise when the electric field of the reflected wave cancels that of the incident wave, where wave dissipation makes the cancelation imperfect, and is reflected in the imaginary part of kz. The famous “Smith chart” provides a graphical representation for lossless transmission lines that was a staple of microwave laboratories in the days before computers were widely available, which, by the way, was really not very long ago (bottom panel of Figure 3).

The ionosphere is not long and thin like this hypothetical capacitor. The capacitor was made thin to ensure that we do not question the coherence of the excitation produced by the electrical connections at the end. But as long as we stipulate that the excitation is coherent the capacitor can be made very wide, with electrical connections spread along its width. For example, the electrical connections could be phased so that they excite a simple plane wave, with some chosen transverse wavelength. In fact, assuming this very-wide geometry actually removes an approximation that we had swept under the rug, which is that to properly analyze the thin capacitor we should form a wavepacket in the transverse direction. If the capacitor is very wide, like, for example, the ionosphere, then there is no such approximation, and we can analyze one transverse wavelength at a time.

Thus, consider the gedankenexperiment shown in Figure 4, where the ionosphere is simplified to be a uniform slab of collisional plasma, with empty space below. The middle panel of Figure 3 is now the electromagnetic equivalent circuit for this simplified version of magnetosphere-ionosphere coupling, with the ionosphere represented by the open-circuited transmission line. The downward looking input admittance for an incident plane wave is given by the same transmission line formula (1), where Y0 and kz depend on the frequency and transverse wavelength of the plane wave.

The real part of the input admittance is, of course, the ionospheric conductance. We can compare the input admittance to the well known electrostatic approximation, which is the field line integrated conductivity, σPl, where σP is the (zero frequency) Pedersen conductivity. Doing this we derive some preliminary criteria for electrostatic theory,where kz 2π/λz − i/ldzλz is the wavelength, and ldz is the dissipation scale length for the propagating electromagnetic mode.

To my knowledge, the last of the three criteria (2) was first derived by Cosgrove (2016), who named iY0kz the wave-Pedersen conductivity, since it replaces the usual (zero-frequency) Pedersen conductivity in an electromagnetic calculation of ionospheric conductance. Cosgrove (2016) also found that Y0 is strongly imaginary, while kz is strongly real, so that iY0kz is in fact strongly real, as expected for the ionospheric admittance. An important corollary comes from the tangent function dependence (1), which suggests the unexpected possibility that the ionospheric conductance could contain (near) singularities and change sign, if the parallel wavelength is ever comparable to the thickness of the ionosphere.

Does this ever happen? Does iY0kz equal σP? Is there really only one propagating electromagnetic mode in the ionosphere? What happens when the ionosphere is vertically inhomogeneous? Stay tuned for the next episode. But I’ll give you a hint, the answer is not boring, just ask those referees who are recovering in the hospital— on second thought, don’t ask them (Cosgrove, 2022).



by Russell Bonner Cosgrove





Collin, R. E. (1966), Foundations for Microwave Engineering, McGraw-Hill.

Cosgrove, R. B. (2016), Does a localized plasma disturbance in the ionosphere evolve to electrostatic equilibrium? evidence to the contrary, J. Geophys. Res., 121, doi: https://doi.org/10.1002/2015JA021672.

Cosgrove, R. B. (2022), An electromagnetic calculation of ionospheric conductance that seems to override the field line integrated con- ductivity, Zenodo and ArXiv, doi: 10.48550/ARXIV.2211.10818, 10.5281/Zenodo.7416494.

Cosgrove, R. B., H. Bahcivan, S. Chen, R. J. Strangeway, J. Ortega, M. Alhassan, Y. Xu, M. V. Welie, J. Rehberger, S. Musielak, and N. Cahill (2014), Empirical model of poynting flux derived from fast data and a cusp signature, J. Geophys. Res., 119, 411–430, doi: https://doi.org/10.1002/2013JA019105.

Space magnetometry from Swarm and beyond

The Swarm satellite mission is ESA's fourth Earth Explorer in space since late 2013. As we prepare to
celebrate 10 years of successful operations (and looking forward to many years more!), the Swarm community met 10-12 October 2023 in sunny Frascati, Italy, for the thirteenth Data Quality Workshop to compare notes and plan for the future of the mission to explore Earth's magnetic field.

With the foremost minds in satellite magnetometry gathered in one room, and expertise ranging from geophysics, space instrumentation and operations to software engineering, this regular meeting is always exciting. Swarm's primary three spacecraft (https://visuals.earth.esa.int/satellites/swarm), as well as other contributing spacecraft, continue to provide invaluable measurements that probe many phenomena, from the flow of material in Earth's core to electric currents above the atmosphere driven by solar activity. We have been able to improve the data quality (i.e. improved calibration and error correction) year-on-year and continue to evolve and grow the large portfolio of data products and services which have enabled scientists to publish over 500 research papers so far, as well as providing critical input to many applications, from navigation and mineral exploration to space weather prediction.

There are two new advances in the data delivery worth mentioning here. Firstly, there is the implementation of a new "FAST" processing chain, which makes data available within a few hours (subject to down-linking constraints imposed by the satellite orbits and ground station locations). This makes it possible to use Swarm for same-day space weather monitoring. The second point is in connection with the VirES data access and exploitation platform which radically increases the accessibility of the data. We are building new capabilities in the on-demand processing of data through the SwarmPAL software, where scientists contribute algorithms and tooling that are made more flexible and coherent through the adoption of a common framework.

The growing opportunities don't stop there though. On 13th October, some of us from the Swarm workshop travelled on to the Royal Astronomical Society, London, for another meeting showing some of the first results from the newly launched Macau Science Satellite (MSS-1). This new mission offers highly complementary data to Swarm and we expect new research analysing the joint dataset over the coming years. With the growing number of operators of high-precision magnetometers in space, the need to collaborate and coordinate is more important than ever.

For more news about Swarm, click here.

Ashley Smith is a postdoctoral researcher at the University of Edinburgh, working as part of the Swarm DISC (Data, Innovation, and Science Cluster). He is passionate about computing technologies and open source software and his research interests include geomagnetic field modelling and space weather. He can be contacted by email at ashley.smith@ed.ac.uk.