Equatorial Density Enhancement

• EDE is defined as a midplane concentration of material or plasma, forming disk-like or toroidal structures in both astrophysical and magnetospheric environments.
• In space physics, EDE is reconstructed from whistler wave measurements that reveal distinct equatorial electron density peaks and dynamic plasmaspheric boundaries.
• In circumstellar systems, analytical models and ALMA observations show that EDEs influence line profiles and outflow dynamics through rotation, gaps, and warps.

Searching arXiv for the cited EDE literature to ground the article in current records. Equatorial density enhancement (EDE) denotes a concentration of material or plasma toward an equatorial plane, but the term is used in more than one technical context. In near-Earth space physics, it refers to an equatorial peak in electron density in the magnetosphere, reconstructed from whistler-wave measurements near the geomagnetic equator (Shastun et al., 2017). In circumstellar and circumbinary astrophysics, it denotes a flattened overdensity—often described as a torus, disk, or equatorial belt—embedded in a circumstellar envelope or circumbinary medium, and invoked in young stellar objects, evolved stars, and symbiotic novae [(Homan et al., 2018); (Jeffers et al., 2014); (Orlando et al., 27 Jul 2025)]. Across these settings, the common element is anisotropy relative to a symmetry plane; the underlying formation mechanisms, observables, and governing equations differ substantially.

1. Terminological scope and physical meaning

In circumstellar usage, equatorial density enhancements are described as “a very common astronomical phenomenon.” Studies of the circumstellar environments of young stellar objects and of evolved stars have shown that these objects often possess such features, which are believed to originate from mechanisms “ranging from binary interactions to the gravitational collapse of interstellar material” (Homan et al., 2018). In symbiotic novae, the red giant’s slow, dense wind can be gravitationally focused in the binary orbital plane, producing a “pile-up” of wind material and thereby a torus or disk of circumbinary gas (Orlando et al., 27 Jul 2025). In the carbon-rich AGB star IRC+10216, the equatorial enhancement is interpreted as dense dust forming a narrow dark lane in scattered light rather than a bipolar outflow (Jeffers et al., 2014).

In magnetospheric usage, the relevant structure is an equatorial peak in electron density. A reconstruction from Cluster whistler-wave measurements shows that near the geomagnetic equator, the electron density has an equatorial maximum within $|\lambda|<3^\circ$, with peak widths of $\Delta\lambda \approx \pm 5^\circ$ at half-maximum density; at $|\lambda|\approx 10^\circ$, $n_e$ has decreased by $\sim 50\%$ relative to the equator (Shastun et al., 2017). In that literature, the phrase “equatorial density enhancement” refers specifically to the latitudinal concentration of plasma density rather than to a geometrically distinct dust or gas torus.

This suggests that EDE is best understood as a morphology class defined by symmetry and concentration, not by a single microphysical origin. A plausible implication is that comparisons across disciplines are most useful at the level of geometry and diagnostics rather than at the level of formation physics.

2. Magnetospheric EDE: reconstruction from whistler waves

A reconstruction method for the electron density distribution in the equatorial region of the magnetosphere uses the ratio of wave magnetic and electric field amplitudes of whistler waves (Shastun et al., 2017). Near the geomagnetic equator, whistler wave normals are mainly close to the direction of the background magnetic field, so the whistler-mode dispersion relation can be used in the parallel propagation approximation. In cold plasma with $\theta = 0$, Faraday’s law in Fourier form gives

$\vec{E}=-(\omega/k)\,\vec{B}\times \hat{e}_k,$

so that

$\frac{B}{E}=\frac{k c}{\omega}.$

With the parallel-propagation whistler dispersion relation

$$n^2 \equiv \frac{c^2k^2}{\omega^2}=\frac{\omega_{pe}^2}{\omega(\omega_{ce}-\omega)},$$

one obtains

$$(c\,B/E)^2=\frac{\omega_{pe}^2}{\omega(\omega_{ce}-\omega)},$$

and therefore the explicit inversion

$\Delta\lambda \approx \pm 5^\circ$0

This inversion expresses the local electron density directly in terms of the measured wave-field ratio $\Delta\lambda \approx \pm 5^\circ$1, the wave frequency $\Delta\lambda \approx \pm 5^\circ$2, and the local gyrofrequency $\Delta\lambda \approx \pm 5^\circ$3 (Shastun et al., 2017).

The method was applied to STAFF-SA measurements on Cluster for 2001–2010. The selection retained only data with magnetic latitude $\Delta\lambda \approx \pm 5^\circ$4 and radial distances $\Delta\lambda \approx \pm 5^\circ$5. Frequency bands were defined as plasmaspheric hiss for $\Delta\lambda \approx \pm 5^\circ$6 and lower-band chorus for $\Delta\lambda \approx \pm 5^\circ$7. Quality control required signal-to-noise ratio greater than $\Delta\lambda \approx \pm 5^\circ$8 for both $\Delta\lambda \approx \pm 5^\circ$9 and $|\lambda|\approx 10^\circ$0 spectra and removed channels with instrument noise floors approaching the measured power. For each 4 s spectrum, the wave amplitude ratio was computed as $|\lambda|\approx 10^\circ$1, and equation (3) was used within the lower-band chorus interval to derive $|\lambda|\approx 10^\circ$2 per time step (Shastun et al., 2017).

The reconstructed density was then binned into $|\lambda|\approx 10^\circ$3 L-shell $|\lambda|\approx 10^\circ$4 h MLT $|\lambda|\approx 10^\circ$5 latitude cells, with median $|\lambda|\approx 10^\circ$6 and inter-quartile range computed within each cell (Shastun et al., 2017). This produced a statistical map of the equatorial density enhancement and the plasmapause across all local times covered by Cluster.

3. Statistical properties of the magnetospheric EDE

The inversion yields a distinct equatorial density enhancement in the plasmasphere (Shastun et al., 2017). Inside the plasmasphere, for $|\lambda|\approx 10^\circ$7, median equatorial $|\lambda|\approx 10^\circ$8 rises from $|\lambda|\approx 10^\circ$9 at $n_e$0 to $n_e$1 at $n_e$2, then falls beyond the plasmapause. The plasmapause itself appears as a sharp drop in $n_e$3 from $n_e$4 to $n_e$5 between $n_e$6 and $n_e$7, varying from dawn at $n_e$8 to dusk at $n_e$9 (Shastun et al., 2017).

The latitudinal structure is central to the EDE designation. The equatorial peak occupies $\sim 50\%$0, with widths of $\sim 50\%$1 at half-maximum density. By $\sim 50\%$2, the density has decreased by approximately half relative to the equator (Shastun et al., 2017). Geomagnetic activity modifies both the sharpness and location of the feature: during quiet times ($\sim 50\%$3), EDE peaks are sharper and the plasmapause L-shell is more sunward, with $\sim 50\%$4; under active conditions ($\sim 50\%$5), the equatorial peak broadens in latitude to $\sim 50\%$6 and $\sim 50\%$7 shifts inward to $\sim 50\%$8 (Shastun et al., 2017).

Validation was carried out against empirical models and in situ sounders. The derived plasmapause location and equatorial density profile agree within $\sim 50\%$9 with Ozhogin et al. (2012) and Sheeley et al. (2001), while cross-calibration with THEMIS RPI and Van Allen Probes A/B upper-hybrid sounding shows agreement to within $\theta = 0$0 in overlapping L–MLT regions (Shastun et al., 2017). The method also provides continuous, high-time-resolution density estimates at 4 s cadence and can capture transient EDE broadening and plasmapause motions at sub-hour timescales (Shastun et al., 2017).

The main limitations are explicitly quantified. Statistical wave-normal analysis gives $\theta = 0$1–$\theta = 0$2 near the equator with $\theta = 0$3, and Monte Carlo propagation of this uncertainty yields less than $\theta = 0$4 error in $\theta = 0$5 with a $\theta = 0$6 confidence interval of $\theta = 0$7 (Shastun et al., 2017). Above $\theta = 0$8, oblique hiss becomes significant and the parallel approximation underestimates $\theta = 0$9 by up to $\vec{E}=-(\omega/k)\,\vec{B}\times \hat{e}_k,$0. Additional limitations arise from the STAFF-SA electric-field noise floor when $\vec{E}=-(\omega/k)\,\vec{B}\times \hat{e}_k,$1 and from neglected warm-plasma and multi-ion effects, which may introduce systematic bias of up to $\vec{E}=-(\omega/k)\,\vec{B}\times \hat{e}_k,$2 under extreme conditions (Shastun et al., 2017).

4. Circumstellar EDEs: analytical geometry, substructure, and kinematics

A simplified analytical parametrization of a three-dimensional circumstellar EDE was developed for interpreting high-resolution data, especially ALMA data (Homan et al., 2018). In cylindrical coordinates $\vec{E}=-(\omega/k)\,\vec{B}\times \hat{e}_k,$3, a simple flared, axisymmetric EDE is written as

$\vec{E}=-(\omega/k)\,\vec{B}\times \hat{e}_k,$4

with Gaussian scale height

$\vec{E}=-(\omega/k)\,\vec{B}\times \hat{e}_k,$5

The adopted typical values are $\vec{E}=-(\omega/k)\,\vec{B}\times \hat{e}_k,$6, $\vec{E}=-(\omega/k)\,\vec{B}\times \hat{e}_k,$7, and $\vec{E}=-(\omega/k)\,\vec{B}\times \hat{e}_k,$8, where $\vec{E}=-(\omega/k)\,\vec{B}\times \hat{e}_k,$9 corresponds to a flaring disk (Homan et al., 2018).

The same framework includes several substructures. A warped disk is represented by

$\frac{B}{E}=\frac{k c}{\omega}.$0

with warp amplitude $\frac{B}{E}=\frac{k c}{\omega}.$1 and number of undulations $\frac{B}{E}=\frac{k c}{\omega}.$2. An annular gap is imposed through a multiplicative factor $\frac{B}{E}=\frac{k c}{\omega}.$3, equal to $\frac{B}{E}=\frac{k c}{\omega}.$4 between $\frac{B}{E}=\frac{k c}{\omega}.$5 and $\frac{B}{E}=\frac{k c}{\omega}.$6 and unity elsewhere. Logarithmic spiral arms are described by

$\frac{B}{E}=\frac{k c}{\omega}.$7

with $\frac{B}{E}=\frac{k c}{\omega}.$8 arms and $\frac{B}{E}=\frac{k c}{\omega}.$9 (Homan et al., 2018).

Several global velocity fields were treated explicitly: Keplerian rotation with $$n^2 \equiv \frac{c^2k^2}{\omega^2}=\frac{\omega_{pe}^2}{\omega(\omega_{ce}-\omega)},$$0; radial outflow with constant $$n^2 \equiv \frac{c^2k^2}{\omega^2}=\frac{\omega_{pe}^2}{\omega(\omega_{ce}-\omega)},$$1; super-Keplerian and sub-Keplerian spiral flows obtained by adding positive or negative radial components to the Keplerian azimuthal term; and rigid rotation $$n^2 \equiv \frac{c^2k^2}{\omega^2}=\frac{\omega_{pe}^2}{\omega(\omega_{ce}-\omega)},$$2, truncated at a maximum tangential speed at $$n^2 \equiv \frac{c^2k^2}{\omega^2}=\frac{\omega_{pe}^2}{\omega(\omega_{ce}-\omega)},$$3 (Homan et al., 2018). The effect of a bipolar outflow was modeled through a velocity law

$$n^2 \equiv \frac{c^2k^2}{\omega^2}=\frac{\omega_{pe}^2}{\omega(\omega_{ce}-\omega)},$$4

and a density

$$n^2 \equiv \frac{c^2k^2}{\omega^2}=\frac{\omega_{pe}^2}{\omega(\omega_{ce}-\omega)},$$5

with a sharp geometric boundary at polar angle $$n^2 \equiv \frac{c^2k^2}{\omega^2}=\frac{\omega_{pe}^2}{\omega(\omega_{ce}-\omega)},$$6 where EDE and outflow densities are equal (Homan et al., 2018).

These geometries and kinematics were fed into the three-dimensional radiative-transfer code LIME, which solved non-LTE CO level populations on an unstructured mesh of $$n^2 \equiv \frac{c^2k^2}{\omega^2}=\frac{\omega_{pe}^2}{\omega(\omega_{ce}-\omega)},$$7 cells weighted toward high-density regions, and produced intensity datacubes $$n^2 \equiv \frac{c^2k^2}{\omega^2}=\frac{\omega_{pe}^2}{\omega(\omega_{ce}-\omega)},$$8 with channel spacing $$n^2 \equiv \frac{c^2k^2}{\omega^2}=\frac{\omega_{pe}^2}{\omega(\omega_{ce}-\omega)},$$9 (Homan et al., 2018). The diagnostics emphasized in that work were channel maps, wide-slit position-velocity diagrams, stereograms, and spectral lines.

5. Observational diagnostics and constraints in circumstellar systems

The observational signatures of a circumstellar EDE depend strongly on the velocity field, inclination, and substructure (Homan et al., 2018). Keplerian rotation produces high-velocity lobes on opposite sides and a “butterfly” shape in channel maps, while radial outflow yields ring-like or “eye”-shaped structures and a broad central emission zone. Gaps and spirals can appear directly as missing or enhanced arcs at specific offsets for low inclination, whereas warp signatures are usually suppressed by projection except for special orientations (Homan et al., 2018).

Wide-slit position-velocity diagrams are particularly diagnostic. In the equatorial cut, Keplerian emission tilts from red to blue with spatial offset, while radial kinematics produce an eye shape. Rigid rotation rotates the PV morphology by $$(c\,B/E)^2=\frac{\omega_{pe}^2}{\omega(\omega_{ce}-\omega)},$$0 from face-on to edge-on, and comparing orthogonal PV diagrams can break degeneracies between some candidate velocity fields (Homan et al., 2018). Spectral lines further constrain orientation and flow: a Keplerian EDE seen edge-on yields a double-peaked line, but face-on gives a narrow central spike; a radial field evolves from flattening parabolic to double-peaked with inclination; and a disk plus outflow can generate a composite spike-plus-broad-wings profile at low inclinations (Homan et al., 2018).

The same framework provides explicit inference strategies. Inclination can be estimated from asymmetry in the polar PV cut and from the tilt of emission in the equatorial PV cut. Scale height and disk diameter can be related to the projected dimensions using the cylindrical approximation

$$(c\,B/E)^2=\frac{\omega_{pe}^2}{\omega(\omega_{ce}-\omega)},$$1

Velocity field, density contrast between EDE and outflow, and substructure parameters such as gap radius or spiral pitch can then be inferred from PV symmetries, line wings versus central spike, and the spacing of channel-map or PV features (Homan et al., 2018). Line-ratio fitting for CO $$(c\,B/E)^2=\frac{\omega_{pe}^2}{\omega(\omega_{ce}-\omega)},$$2–$$(c\,B/E)^2=\frac{\omega_{pe}^2}{\omega(\omega_{ce}-\omega)},$$3 through $$(c\,B/E)^2=\frac{\omega_{pe}^2}{\omega(\omega_{ce}-\omega)},$$4–$$(c\,B/E)^2=\frac{\omega_{pe}^2}{\omega(\omega_{ce}-\omega)},$$5 is described as an inclination-independent probe of the radial density exponent $$(c\,B/E)^2=\frac{\omega_{pe}^2}{\omega(\omega_{ce}-\omega)},$$6 (Homan et al., 2018).

Simulated ALMA observations with CASA/simobserve used the C36-1 configuration, angular resolution $$(c\,B/E)^2=\frac{\omega_{pe}^2}{\omega(\omega_{ce}-\omega)},$$7, largest angular scale $$(c\,B/E)^2=\frac{\omega_{pe}^2}{\omega(\omega_{ce}-\omega)},$$8, single pointing, $$(c\,B/E)^2=\frac{\omega_{pe}^2}{\omega(\omega_{ce}-\omega)},$$9, $\Delta\lambda \approx \pm 5^\circ$00, and $\Delta\lambda \approx \pm 5^\circ$01 (Homan et al., 2018). If the EDE or outflow exceeds the largest angular scale, low-$\Delta\lambda \approx \pm 5^\circ$02 emission is filtered out first, producing a deficit around $\Delta\lambda \approx \pm 5^\circ$03 in PV diagrams. To recover the full morphology, the recommended condition is that the largest angular scale comfortably exceed the projected EDE diameter, with spectral resolution $\Delta\lambda \approx \pm 5^\circ$04 (Homan et al., 2018).

6. EDEs in evolved stars and symbiotic novae

Specific objects illustrate the diversity of equatorial density enhancements in evolved-star environments. In IRC+10216, ExPo imaging polarimetry at $\Delta\lambda \approx \pm 5^\circ$05–$\Delta\lambda \approx \pm 5^\circ$06 and $\Delta\lambda \approx \pm 5^\circ$07 resolution revealed a narrow east–west dark lane about $\Delta\lambda \approx \pm 5^\circ$08 wide across the stellar position, with two bright lobes to the north and south and an overall scattered-light nebula spanning $\Delta\lambda \approx \pm 5^\circ$09 in the equatorial direction (Jeffers et al., 2014). The lane is interpreted as an optically thick equatorial belt of dust that forward-scatters stellar photons and thereby produces a shadow in polarized flux. Radiative-transfer modelling with MCMax reproduced the morphology using either an equatorial enhancement (“torus”) model or an episodic ring model (Jeffers et al., 2014).

In the torus interpretation for IRC+10216, the density has the form

$\Delta\lambda \approx \pm 5^\circ$10

with representative best-fit parameters $\Delta\lambda \approx \pm 5^\circ$11, $\Delta\lambda \approx \pm 5^\circ$12, $\Delta\lambda \approx \pm 5^\circ$13, $\Delta\lambda \approx \pm 5^\circ$14, $\Delta\lambda \approx \pm 5^\circ$15, and inclination $\Delta\lambda \approx \pm 5^\circ$16 (Jeffers et al., 2014). The optical depths are $\Delta\lambda \approx \pm 5^\circ$17 and $\Delta\lambda \approx \pm 5^\circ$18, and the current dust-mass-loss rate is approximately $\Delta\lambda \approx \pm 5^\circ$19 compared with approximately $\Delta\lambda \approx \pm 5^\circ$20 in the old spherical wind (Jeffers et al., 2014). An alternative episodic ring model also reproduces the dark lane, and current data do not constrain whether a binary companion is responsible (Jeffers et al., 2014).

In EP Aquarii, ALMA analyses place the birth of the EDE very close to the star. The EDE first appears in CO(2–1) as a narrow spectral component with $\Delta\lambda \approx \pm 5^\circ$21 emerging already at $\Delta\lambda \approx \pm 5^\circ$22–$\Delta\lambda \approx \pm 5^\circ$23, with kinematics there dominated by rotation rather than expansion (Nhung et al., 2023). Sinusoidal fits in $\Delta\lambda \approx \pm 5^\circ$24 rings give rotational amplitudes $\Delta\lambda \approx \pm 5^\circ$25 at $\Delta\lambda \approx \pm 5^\circ$26–$\Delta\lambda \approx \pm 5^\circ$27, about an axis inclined $\Delta\lambda \approx \pm 5^\circ$28 to the line of sight, consistent with a power-law decline $\Delta\lambda \approx \pm 5^\circ$29 with $\Delta\lambda \approx \pm 5^\circ$30 (Nhung et al., 2023). Beyond $\Delta\lambda \approx \pm 5^\circ$31, the narrow component is dominated by radial expansion, with $\Delta\lambda \approx \pm 5^\circ$32 and intrinsic line broadening $\Delta\lambda \approx \pm 5^\circ$33 (Nhung et al., 2023).

The EP Aquarii EDE is nearly face-on, with inclination $\Delta\lambda \approx \pm 5^\circ$34, and flared by rms $\Delta\lambda \approx \pm 5^\circ$35 about the midplane, corresponding to $\Delta\lambda \approx \pm 5^\circ$36–$\Delta\lambda \approx \pm 5^\circ$37 (Nhung et al., 2023). A plausible vertical profile is

$\Delta\lambda \approx \pm 5^\circ$38

with $\Delta\lambda \approx \pm 5^\circ$39, giving $\Delta\lambda \approx \pm 5^\circ$40 (Nhung et al., 2023). The CO(2–1) brightness indicates a CO emissivity $\Delta\lambda \approx \pm 5^\circ$41–$\Delta\lambda \approx \pm 5^\circ$42 higher than in the polar wind at the same radius, with fluctuations of $\Delta\lambda \approx \pm 5^\circ$43 around the mean disc; if the polar density scales as $\Delta\lambda \approx \pm 5^\circ$44, the disc midplane density must exceed the polar density by a factor $\Delta\lambda \approx \pm 5^\circ$45–$\Delta\lambda \approx \pm 5^\circ$46 (Nhung et al., 2023). The same observations show episodic, lumpy mass ejections in the polar outflows, with shell-like arcs spanning $\Delta\lambda \approx \pm 5^\circ$47–$\Delta\lambda \approx \pm 5^\circ$48 in position angle and characteristic timescales $\Delta\lambda \approx \pm 5^\circ$49 (Nhung et al., 2023).

In the symbiotic recurrent nova T Coronae Borealis, the circumbinary medium is modeled as a spherical red-giant wind plus a torus-like EDE (Orlando et al., 27 Jul 2025). The EDE is represented as a Gaussian torus centered on the binary center of mass, aligned with the orbital plane, with density

$\Delta\lambda \approx \pm 5^\circ$50

Characteristic scale lengths are $\Delta\lambda \approx \pm 5^\circ$51 up to $\Delta\lambda \approx \pm 5^\circ$52, and $\Delta\lambda \approx \pm 5^\circ$53 in representative runs, with variants at $\Delta\lambda \approx \pm 5^\circ$54 and $\Delta\lambda \approx \pm 5^\circ$55 (Orlando et al., 27 Jul 2025). These correspond to an opening angle of order $\Delta\lambda \approx \pm 5^\circ$56–$\Delta\lambda \approx \pm 5^\circ$57, and the EDE is inclined by $\Delta\lambda \approx \pm 5^\circ$58 to the observer’s line of sight (Orlando et al., 27 Jul 2025).

For T CrB, the spherical wind corresponds to $\Delta\lambda \approx \pm 5^\circ$59 for a $\Delta\lambda \approx \pm 5^\circ$60 wind, while the EDE has peak hydrogen number density $\Delta\lambda \approx \pm 5^\circ$61 in representative runs and integrated mass $\Delta\lambda \approx \pm 5^\circ$62 (Orlando et al., 27 Jul 2025). In the hydrodynamic models, the disk and EDE collimate the nova blast: the disk dominates during the first hours, the EDE after approximately one day, and the result is a bipolar shock and a prolate, twin-lobed remnant (Orlando et al., 27 Jul 2025). Synthetic X-ray light curves show three phases—an early phase dominated by shocked disk material, an intermediate phase driven by reverse-shocked ejecta, and a late phase dominated by the forward shock into the EDE and red-giant wind. The EDE produces a soft X-ray bump or plateau around $\Delta\lambda \approx \pm 5^\circ$63–$\Delta\lambda \approx \pm 5^\circ$64 days, and its column density modulates early attenuation below approximately $\Delta\lambda \approx \pm 5^\circ$65 (Orlando et al., 27 Jul 2025).

7. Interpretation, degeneracies, and open problems

The cited literature makes clear that EDEs are diagnostically powerful but not uniquely constraining. In IRC+10216, both a torus model and a dust-rings model reproduce the observed dark lane, and the available data do not constrain the formation of the equatorial enhancement by a binary system (Jeffers et al., 2014). In EP Aquarii, neither conservation of angular momentum in a slow, dense wind nor gravitational focusing of an equatorial outflow by a companion has been uniquely identified as the origin of the close-in disc; what is observationally clear is that the disc must form inside $\Delta\lambda \approx \pm 5^\circ$66, before radial radiation-pressure acceleration erases rotation (Nhung et al., 2023). In T CrB, the EDE is operationally defined through a hydrodynamic circumbinary model, where its principal observable significance is blast collimation and its imprint on synthetic X-ray spectra and light curves (Orlando et al., 27 Jul 2025).

A recurring issue is the distinction between equatorial overdensity and bipolar outflow. The IRC+10216 scattered-light morphology was previously interpreted as bipolar, but the modelling discussed in the cited work attributes the dark lane to dense equatorial dust rather than a bipolar outflow (Jeffers et al., 2014). In circumstellar line observations, the analytical models show that degeneracies between Keplerian, radial, and rigid-body fields can persist unless orthogonal PV diagrams, channel maps, stereograms, and line profiles are considered together (Homan et al., 2018). In the magnetospheric case, an analogous caution concerns propagation assumptions: near the equator the parallel approximation is justified statistically, but at higher latitudes oblique hiss can bias density retrievals (Shastun et al., 2017).

Taken together, these studies show that the physical content of “equatorial density enhancement” depends on context, but several structural themes recur: concentration toward a midplane, strong sensitivity to inclination, and an observational signature mediated by transport or radiative processes. In astrophysical systems, this leads to torus- or disk-like morphologies, altered line profiles, and anisotropic outflow dynamics [(Homan et al., 2018); (Jeffers et al., 2014); (Nhung et al., 2023); (Orlando et al., 27 Jul 2025)]. In magnetospheric plasma physics, it appears as a latitudinal maximum in electron density near the geomagnetic equator that can be reconstructed from wave-field ratios and used to track plasmapause structure and activity dependence (Shastun et al., 2017).