Infernal Modes in Reversed Shear

• Infernal modes are pressure-driven MHD instabilities in tokamak plasmas with low or reversed magnetic shear, where weakened field-line bending permits rapid mode growth.
• The topic explains how non-monotonic safety-factor profiles and toroidal sideband coupling, influenced by shaping effects like elongation and triangularity, modulate mode structure and dispersion relations.
• Experimental and simulation data, such as from the CFETR 1GW SSO equilibrium, highlight strategies to optimize q-profiles and control rotation for managing infernal instabilities in advanced tokamaks.

Infernal modes in reversed shear refer to a class of pressure-driven long-wavelength MHD instabilities that manifest in toroidal fusion plasmas with extended regions of very low or reversed magnetic shear. These modes are closely associated with non-monotonic safety-factor ($q$) profiles, particularly those exhibiting flat or locally reversed shear, such that $q'(r) \approx 0$ over a finite interval. In these configurations, the stabilizing field-line bending effect is significantly weakened, allowing the destabilizing influence of pressure gradients and toroidal coupling to dominate. Infernal modes are characterized by broad radial structures spanning the low-shear region, discrete spectra of fast-growing modes for given $(m,n)$, and, under sufficient resistivity, formation of a cascade of subdominant oscillatory branches. Their relevance is amplified in advanced tokamak scenarios and reactor-scale plasmas (e.g., CFETR 1GW SSO), where the interplay between equilibrium shaping, kinetic effects, and current profiles can both promote and modulate infernal activity (Coste-Sarguet et al., 3 Sep 2025, Li et al., 2024, Han et al., 2021).

1. Overview of Governing Physics and Equilibrium Features

Infernal modes arise within the framework of linear resistive MHD, typically around static axisymmetric equilibria described by $\{\mathbf{B}_0, p_0, \rho_0\}$. The key ingredient is an extended region where the local magnetic shear $s(r) = r\,dq/dr / q$ is small or even negative. In such settings, rational surfaces (where $q(r_s) = m/n$) are densely packed or nearly degenerate, causing the coupling between neighboring poloidal harmonics ($m$, $m\pm1$) to intensify.

Shaping effects—elongation ($\kappa$), triangularity ($\delta$)—modify the effective pressure–field-line-bending competition via the generalized Mercier index $q'(r) \approx 0$0: $q'(r) \approx 0$1 where $q'(r) \approx 0$2 defines the local pressure drive (Coste-Sarguet et al., 3 Sep 2025).

Advanced scenarios, exemplified by the CFETR 1GW SSO equilibrium, feature deeply reversed $q'(r) \approx 0$3 in the core ($q'(r) \approx 0$4) and pronounced flat-$q'(r) \approx 0$5 plateaus at the edge ($q'(r) \approx 0$6), predisposing both core and edge to infernal activity (Han et al., 2021).

2. Modal Structure and Dispersion Relations

In low- or reversed-shear regions, the eigenmode structure is governed by an integro-differential equation for the radial plasma displacement $q'(r) \approx 0$7, with coupling to immediate sidebands (resistive layer physics entering via Ohm’s law and rational layer matching).

Ideal Shearless Spectrum

For $q'(r) \approx 0$8 and monotonic $q'(r) \approx 0$9, neglecting $(m,n)$0 yields the “shearless” infernal spectrum. The generalized dispersion relation reduces to: $(m,n)$1 with $(m,n)$2, $(m,n)$3, and $(m,n)$4 the Alfvén frequency. Each $(m,n)$5 root corresponds to a discrete mode, forming an unstable spectrum with the fundamental branch ($(m,n)$6) broad across the low-shear region and higher $(m,n)$7 branches more radially oscillatory (Coste-Sarguet et al., 3 Sep 2025).

Reversed Shear and Generalized $(m,n)$8 Profiles

When $(m,n)$9 exhibits a minimum ($\{\mathbf{B}_0, p_0, \rho_0\}$0), field-line bending diminishes, and analytic Bessel-type solutions break down. An energy-minimization plus singular-layer approach yields the full dispersion: $\{\mathbf{B}_0, p_0, \rho_0\}$1 which reduces continuously to the ideal case as $\{\mathbf{B}_0, p_0, \rho_0\}$2 (Coste-Sarguet et al., 3 Sep 2025).

Analytic Instability Thresholds

• Ideal interchange criterion: $\{\mathbf{B}_0, p_0, \rho_0\}$3
• Resistive infernal (reversed-shear): $\{\mathbf{B}_0, p_0, \rho_0\}$4, where $\{\mathbf{B}_0, p_0, \rho_0\}$5 depends on $\{\mathbf{B}_0, p_0, \rho_0\}$6—explicit thresholds are given in (Coste-Sarguet et al., 3 Sep 2025).

3. Physical Drivers and Discrete Mode Cascade

Several mechanisms coalesce in reversed-shear configurations to drive infernal modes:

• Field-line bending suppression: As $\{\mathbf{B}_0, p_0, \rho_0\}$7, the stabilization term drops, allowing pressure drive to dominate.
• Toroidal sideband coupling: Geometric effects couple $\{\mathbf{B}_0, p_0, \rho_0\}$8 modes to $\{\mathbf{B}_0, p_0, \rho_0\}$9 harmonics, enhancing instability even when formally higher order in aspect ratio expansion.
• Cascade spectrum: The eigenmode sequence ($s(r) = r\,dq/dr / q$0) corresponds to increasingly oscillatory radial structures. As long as the resistive growth $s(r) = r\,dq/dr / q$1, subdominant branches remain unstable (Coste-Sarguet et al., 3 Sep 2025).

Kinetic generalizations (KIM) bridge the infernal and kinetic ballooning mode (KBM) branches, especially evident in global gyrokinetic simulations. The transition arises due to the changing proximity of rational surfaces and local shear: KIM occurs where the rational surface is nearest the minimum shear, saturating as $s(r) = r\,dq/dr / q$2 and peaking near optimal $s(r) = r\,dq/dr / q$3. FLR and FOW effects modify thresholds and radial localization (Li et al., 2024).

4. Role of Resistivity, Kinetics, and Numerical Modeling

Resistivity, compressibility, and kinetic terms influence both mode structure and instability thresholds:

• Resistive layer: Inner-layer width $s(r) = r\,dq/dr / q$4, with $s(r) = r\,dq/dr / q$5 normalized resistivity. Sufficiently large $s(r) = r\,dq/dr / q$6 admits ideal-like infernal roots; otherwise, “resistive interchange” dominates (Coste-Sarguet et al., 3 Sep 2025).
• Finite Larmor radius (FLR)/orbit width (FOW): In kinetic treatment, FLR and FOW set mode envelope width $s(r) = r\,dq/dr / q$7 and stabilize the small-scale MHD drive above threshold $s(r) = r\,dq/dr / q$8. For $s(r) = r\,dq/dr / q$9 above threshold and $q(r_s) = m/n$0 small, kinetic infernal modes can reach twice the KBM growth rate (Li et al., 2024).
• Numerical limitations: Conventional MHD codes frequently reduce the perturbed vector potential to $q(r_s) = m/n$1, suppressing parallel magnetic perturbations and altering the Mercier parameter. This omission artificially stabilizes tearing/interchange and masks the infernal branch except at vanishingly small $q(r_s) = m/n$2. Modular linear solvers that preserve full $q(r_s) = m/n$3, include sidebands up to $q(r_s) = m/n$4, and use adaptive grids reliably capture the entire infernal spectrum in shaped reversed-shear equilibria (Coste-Sarguet et al., 3 Sep 2025).

Characteristic Kinetic and Growth-Rate Data

β (%)	ω<sub>r</sub> (c<sub>s</sub>/R₀)	γ (c<sub>s</sub>/R₀)	ω<sub>r</sub> (c<sub>s</sub>/R₀, rev. shear)	γ (c<sub>s</sub>/R₀, rev. shear)
1.0	0 (ITG)	0.005	0 (ITG)	0.007
1.4	−1.3 (KBM)	0.008	−1.2 (ITG)	0.009
2.0	−1.4	0.01	−1.5 (KIM)	0.018

For $q(r_s) = m/n$5, $q(r_s) = m/n$6, $q(r_s) = m/n$7 (Li et al., 2024).

5. Experimental Manifestation and Practical Consequences

Analysis of the CFETR 1GW SSO reversed-shear equilibrium provides a clear practical demonstration:

• Profile Features: Deep $q(r_s) = m/n$8 reversal in the core, broad edge $q(r_s) = m/n$9 plateau.
• Dominant Eigenstructure: Edge-localized infernal harmonics ($m$0 at $m$1) possessing peak radial displacement 10–20$m$2 larger than core infernal components ($m$3).
• Stability Boundaries: Edge-localized infernal mode lowers both no-wall and ideal-wall $m$4 limits; the operational target $m$5 exceeds the computed no-wall limit ($m$6), necessitating additional stabilization (Han et al., 2021).

Rotational stabilization—particularly edge-localized rotation—is found to be critical. Complete suppression of the dominant edge infernal component at the design wall location requires

$m$7

where $m$8 is the Alfvén speed and $m$9 the major radius. Both uniform and edge-peaked rotation profiles suffice if this condition is met precisely at the edge plateau (Han et al., 2021).

6. Implications for Design and Control in Advanced Tokamaks

The infernal mode spectrum fundamentally constrains the operational space in reversed- and low-shear scenarios:

• Scenario Design: Avoid positioning rational surfaces in flat or reversed-shear regions coincident with strong pressure gradients unless deliberate rapid reconnection (e.g., hybrid sawtooth pacing) is desired.
• Profile Optimization: Raised minimum shear, radial displacement of $m\pm1$0, reduction of $m\pm1$1 near weak-shear regions, and controlled shaping (including negative triangularity) serve as suppression strategies (Coste-Sarguet et al., 3 Sep 2025, Li et al., 2024).
• Modeling Requirements: Neglecting parallel field perturbations and limit-sideband physics in stability codes results in overestimating achievable $m\pm1$2 or safety-factor limits, masking critical instability branches.

A plausible implication is that restrained use of advanced bootstrap-current shaping and $m\pm1$3-profile tailoring is required to balance energy confinement gains against the destabilizing persistence of infernal spectra in such advanced scenarios.

7. Connection to Kinetic and Global Non-MHD Effects

Global gyrokinetic simulations exhibit a seamless transition between kinetic ballooning and infernal branches. In the low-shear/well regimes, electromagnetic inertial instabilities driven by ion pressure gradient ($m\pm1$4) combine features of both classical infernal and kinetic ballooning modes. As $m\pm1$5 decreases, the mode envelope localizes about the shear minimum, with the growth rate maximized for moderate but finite $m\pm1$6 before declining as stabilization from residual field-line bending (and FLR) overcomes the drive (Li et al., 2024).

This continuous spectrum, dependence on rational surface separation $m\pm1$7, and the associated physics point to the necessity of adopting global (as opposed to ballooning local) analyses and kinetic-MHD models in reversed-shear stability studies for reactor-relevant plasmas.