Patient-reported distress and anxiety during cone-beam CT imaging sessions with increased gantry rotation speeds.

Abstract Be stars are rapid rotators generally produced by binary interactions. The single Be stars in the observations pose challenges to the Be star formation theory. In this paper, we propose a new pathway for the formation of single Be stars, in which the Be star is taken as the ejected companion star from a Type Ia supernova (SN Ia) explosion. Recent numerical simulations suggest that explosive oxygen burning, initiated via the convective Urca process in certain helium (He) stars near the Chandrasekhar mass limit, can set off a SN Ia. Based on this proposition, we further demonstrate that about $0.4\%$ of He star + main-sequence (MS) star binaries may evolve into single Be stars, where the MS star is spun up due to the mass accretion from the He star, and then the He star explodes as a SN Ia. We employ detailed binary evolutionary simulations and find the parameter space that would produce single Be stars via the SN Ia channel. Around $22\%$ of Be stars from the SN Ia progenitor channel exhibit peculiar tangential velocities exceeding $24\ \rm km/s$, classifying them as runaway stars. This suggests that the SN Ia channel plays a meaningful role in forming single Be stars, particularly within the runaway star population.

Synchronous measures of head kinematics and in vivo brain deformation during rapid head rotation are needed to advance understanding of traumatic brain injury (TBI) mechanics and enhance computational modeling as a tool for injury risk assessment and prevention. The aims of this study were to produce repeatable rapid rotation of the in vivo sheep head, to assess the viability of the sonomicrometry method for measuring multipoint brain displacement, and to quantify the in vivo brain deformation response to rapid rotation. In three anaesthetized adult sheep, arrays of sonomicrometry transceivers were implanted into the brain and rigidly attached to the inner skull surface. Repeatable, rapid, sagittal plane head rotation (nominally about the second cervical vertebra) was induced with a non-impact head rotation apparatus. Computed tomography imaging was performed to assess relative motion between transceivers and brain tissue. Three-dimensional brain displacement, strain, and head kinematics were assessed for repeatability. The location of up to 13 (mean = 11) brain transceivers were tracked in each of 11 rapid head rotation tests. Peak head angular acceleration and velocity were up to 38.56 krad/s2 and 30.43rad/s, respectively, and average duration of head motion was 241.9 ± 23.1ms. Pre-to-post-test transceiver displacement in brain tissue was less than the spatial resolution of the measurement system, and brain displacements measured during rapid head rotation had excellent repeatability (CORA score 0.99). Brain displacements and strains up to 2.47mm and 18%, respectively, were observed. The brain exhibited decaying sinusoidal rotational deformation in the sagittal plane with oscillating tension-compression waves. Sonomicrometry was reliably applied in vivo and provided repeatable measurements of brain deformation in a non-survival large animal model of rapid head rotation.

Newborn and juveniles exhibit distinct transcriptional and pathological profiles after brain injury.

Abstract Gravitational-wave astronomy has revealed that close binaries with compact companions are widespread. Long gamma-ray bursts (LGRBs) from massive star collapse face persistent challenges in achieving the rapid core rotation required by the collapsar model. Binary interaction via tidal spin-up offers a natural solution; recent population synthesis studies suggest a substantial fraction of LGRBs may originate from close binaries with a compact companion. In this scenario, supernova ejecta from the primary can be accreted by the companion, potentially launching a second relativistic jet after a delay set by the binary separation. We develop a comprehensive model for these double-jet systems, analyzing the dynamics of the second jet and its interaction with the first. The resulting observational signatures depend critically on the Lorentz factor ratio, the alignment angle, and the time delay. For aligned jets, two regimes arise: a fast second jet producing multiple gamma-ray triggers with distinct spectral/polarization evolution, and a slow second jet where its emission appears as an X-ray flare followed by an afterglow plateau from energy injection. For misaligned jets, the observed signal ranges from normal gamma-ray bursts (GRBs) with late-time radio structures to fast X-ray transients followed by off-axis rebrightening. These features have observational parallels in existing GRB data. High-resolution radio interferometry with SKA, time-resolved polarimetry with eXTP, and multiwavelength surveys with Einstein Probe and SVOM will test these predictions, providing constraints on the evolution of close massive binaries as progenitors of GRBs and gravitational-wave sources.

Abstract We investigate the linear onset of convection in a rotating plane layer permeated by a uniform horizontal magnetic field perpendicular to the rotation axis, a configuration relevant to dynamics within Earth’s tangent cylinder and complementing recent investigations [Barman and Sahoo 2025. Phys. Scr. 100 125018]. The primary objective is to examine how partial thermal stratification modifies convective initiation across three thermal states—fully unstable, weakly stable, and strongly stable—over rotation rates corresponding to Ekman numbers E = 10 −3 , 10 −4 , 10 −5 , thermal-to-magnetic diffusivity contrasts characterized by Roberts numbers q = 0.01, 1, 10, and magnetic field strengths spanning Elsasser numbers 0 ≤ Λ ≤ 10. Analysis of convective onset, supported by locally derived scaling relations, shows that introducing a stable segment raises the critical threshold for convection and promotes smaller-scale structures, particularly under rapid rotation. When magnetic forcing is weak, rotational effects dominate, strengthening the vertical alignment of convective motions and enhancing the stabilizing influence of stratification, thereby delaying convective onset. In contrast, strong magnetic forcing maintains broader convective rolls even at rapid rotation, although penetration into the stable layer remains limited. Magnetic damping is most pronounced at low to moderate diffusivity contrasts and weakens when magnetic diffusion becomes dominant, while the penetration depth decreases with increasing rotation and magnetic intensity in strongly stratified regimes. This study shows that partial stable stratification significantly modifies the onset of rotating magnetoconvection under a horizontal magnetic field by increasing the instability threshold, favoring smaller-scale structures, and limiting convective penetration into the stable layer, with the combined effects of buoyancy, rotation, and magnetic forces shaping the flow morphology. These results extend classical plane-layer magnetoconvection models and provide insight into planetary core dynamics—such as within Earth’s tangent cylinder—where stable stratification and magnetic feedback coexist, while also highlighting contrasts between weak-field planetary interiors and strong-field stellar environments.

Major earthquakes often induce multi-structural rupture styles, which serve as a crucial basis for understanding stress partitioning and strain adjustment within tectonic systems, as well as for constructing regional deformation models. The 1927 M 8.0 Gulang earthquake in the northeastern Tibetan Plateau exemplifies this phenomenon. This rare event, characterized by a single mainshock triggering multiple structural ruptures, resulted in approximately 40,000 casualties and numerous missing persons. In this study, we integrate interpretations of satellite remote sensing imagery, field observations of surface ruptures, and analyses of regional tectonic–geomorphic deformations to reconstruct the coseismic processes of the Gulang earthquake. Our findings reveal that the coseismic surface ruptures exhibit distinct mechanical characteristics driven by complex stress fields. Survey and analysis results indicate that regional tectonic compression oriented from SSW–SW to NNE–NE triggered the mainshock rupture. This stress regime caused nearly E–W folding of strata north of the Huangcheng–Shuangta Fault (HSF), alongside sinistral strike-slip motion in the central-eastern section and thrusting at the eastern end of the Southern Wuwei Basin Fault (SWBF). Blocked by the rigid Alxa Block to the north, comprehensive evidence—including the Late Holocene gravelly clay folded strata formed by north-to-south compression in the Liutiao Lake area, the geomorphic deformation characterized by higher northern and lower southern terraces on both sides of the east–west-trending fault, and the clockwise rotational tectonic surfaces developed at the eastern end of the HSF zone in Shuixiakou—indicates that the coseismic tectonic movement and energy transfer within the meizoseismal area underwent a rapid clockwise rotation from NE to S. This strain rotation induced N–S tensional rupturing along the southern branch of the eastern HSF and nearly E–W thrusting along the NNW-trending Wuwei–Gulang Fault (WGF). Furthermore, this intense and rapid clockwise rotation generated a transient extensional environment characterized by rapid E–W to SE stretching, leading to the formation of a newly identified, NNE-trending, high-angle dextral strike-slip normal fault (hereafter referred to as the NNEF). This process also triggered localized activity at the junctions between the NNEF and the Lenglongling Fault (LLLF), and between the WGF and the nearly E–W-trending Gulang Fault (GLF). We conclude that the seismogenic structure of the 1927 Gulang mainshock comprises three primary components: (1) a fault–fold belt consisting of the SWBF and the nearly E–W fold system north of the HSF; (2) the southern branch of the eastern HSF; and (3) the WGF. The observed segmental activities of the GLF and LLLF are attributed to local strain adjustments. By identifying the newly formed NNEF and characterizing these segmental activations, this study provides new insights into the mechanisms of local strain adjustment within the tectonic systems of the northeastern Tibetan Plateau.

We derive the asymptotic solution for the onset of steady, linear, Boussinesq convection in a rapidly rotating system with stress-free, fixed-flux boundary conditions. While the fixed-temperature (FT) case is attainable analytically with relative ease, the fixed-flux (FF) configuration presents greater complexity. However, in the rapidly rotating limit, the leading-order interior solution remains unaffected by the choice of thermal boundary conditions. We exploit this property by employing an asymptotic approach to characterise the differences between the FT and FF systems. Specifically, this involves constructing a composite boundary layer structure comprising an Ekman layer of thickness $ {\textit{Ta}}^{-1/4}$ , where $ \textit{Ta}$ is the Taylor number ( $ \textit{Ta} \gg 1$ for rapid rotation), and a thermal boundary layer of thickness $ {\textit{Ta}}^{-1/6}$ , to accommodate the FF boundary condition. To capture both scales systematically, we introduce the small parameter ${\varepsilon } = {\textit{Ta}}^{-1/12}$ , representing the ratio between the two boundary layer thicknesses, and use it to guide the asymptotic expansion. The asymptotic corrections capturing the differences between the two systems are combined with the FT system to construct the corresponding solution for the FF system. We find an asymptotic correction of ${\mathcal{O}} ( {\textit{Ta}}^{-1/2} )$ to the critical Rayleigh number, corresponding wavenumber, vertical velocity and temperature, along with a correction of ${\mathcal{O}} ( {\textit{Ta}}^{-1/6} )$ to the vertical vorticity.

If dark matter (DM) exists in halos around rotating neutron stars (NSs), it will be essential to understand the effects of rotation on the distribution of DM and baryonic matter (BM) in the stars to interpret observations. In this work, we construct rapidly rotating dark matter admixed neutron stars (DANS) with DM halos using the two-fluid approximation, where the BM and DM interact only through gravity. Our goal is to describe rapidly rotating millisecond-period DANS spun up by the accretion of BM from a zero angular momentum state. We extend the Rapidly Rotating Neutron Star (RNS) code to compute axisymmetric configurations in which the BM rotates rigidly while the DM remains torque-free and differentially rotates through the frame-dragging of spacetime. For the first time, we examine in detail local and global definitions of mass in general relativity for two-fluid systems, showing how their differences affect the interpretation of baryonic and dark component masses. We compute energy density and frame-dragging frequency profiles for DANS with three different characteristic DM halos. We demonstrate that rapid BM rotation reduces DM halo sizes if central energy densities are kept constant between non-rotating and rotating models. We also construct sequences of DANS to create mass and radius curves and compare rotating and non-rotating cases. Finally, we quantify deviations in the spacetime metric outside the baryonic surfaces of these sequences of stars caused by the DM halos. We hypothesize that the size of this quantity could indicate whether a DM halo will significantly impact X-ray pulse profile modeling. These results provide a framework for assessing the observational consequences of DM halos around rapidly rotating NSs.

Saturn's magnetosphere, shaped by solar wind interaction with its dipole field, differs from Earth's due to faster rotation and Enceladus's internal plasma sources. An ongoing focus of investigation is how the internal plasma sources and rapid rotation result in a different global magnetospheric configuration. The magnetospheric cusp, a crucial interaction region between solar wind and planetary magnetic field, serves as an indicator of global magnetic configuration. Here we utilize Cassini observations from 2004 to 2010 to study dawn-dusk asymmetry in Saturn's cusp distribution and extend the number of cusp events from about 11 reported in previous studies to 67. We find peak occurrence in the post-noon sector and signatures extending to post-dusk (near 20 local time), resembling recent observations of Jupiter's post-dusk cusp. We further examine magnetic topology using high-resolution magnetohydrodynamic simulations to visualize the cusp asymmetry. This is consistent with previous studies, but our simulations provide a more detailed view of Saturn's magnetic topology near the magnetopause. This asymmetry of cusp distribution demonstrates how rapid rotation and internal plasma sources fundamentally alter magnetospheric configuration, offering insights for understanding other rotating planetary systems within and beyond the solar system.

Terrestrial robots are used in diverse environments, including disaster sites, space exploration, and complex terrain, where rapid body rotations are essential for maintaining stability and mobility. However, conventional locomotory strategies are often limited by ground contact, actuation delays, and terrain uncertainty conditions. To address these limitations, nonlocomotory strategies achieve rotation without relying on ground contact. Instead, they utilize rotation control structures such as reaction wheels, robotic tails, reaction bars, robotic arms, robotic legs, and thrusters, which are considered and defined in this review, to generate torques for rotational control. This review categorizes these structures based on their underlying mechanisms and analyzes their applications for body rotation in terrestrial robots. In addition, their functional performances in aerial reorientation, steady‐state locomotion stabilization, perturbation recovery, and agility enhancement are compared. Representative performance metrics and the associated control strategies are also summarized to support cross‐structure evaluation. By summarizing existing research, this review provides a reference framework for selecting and developing dynamic rotation control structures that improve stability, robustness, and maneuverability in terrestrial robots.

Abstract At very low metallicities, s -process production in massive stars is expected to be negligible in non-rotating models owing to three key factors: the scarcity of the 22 Ne neutron source, the presence of primary neutron poisons, and the declining abundance of iron seeds. By making use of advanced stellar evolution models generated by the Geneva Stellar Evolution Code, we investigate the impact of rapid rotation on s -process nucleosynthesis in low-metallicity massive stars. We have presented nucleosynthesis calculations for a rotating 30 M ⊙ star at metallicity Z = 10 −4 . It is found that about 0.8% of the convective He-burning core mass comprises primary 22 Ne. Iron seeds are consumed to a significant extent in rotating stars and the production of 88 Sr, 89 Y, and 90 Zr is achieved significantly. This can also produce s -process nucleosynthesis, allowing it to reach the 208 Pb neutron-magic peak. On the other hand, the amount of 22 Ne strongly impacts the s -process efficiency and the Sr/Ba ratio. Rotation boosts the s -process in massive stars at low metallicities. There are three primary reasons for this. First, we confirm that rotation-induced mixing leads to a significant overproduction of 22 Ne. More 22 Ne means a higher neutron flux and thus higher s -process efficiency, which leads to the production of more and heavier elements. Second, at low metallicities, the primary production of 22 Ne leads to a much higher neutron-to-seed ratio than in non-rotating stars. The increased availability of neutrons allows the star to consume a much larger fraction of its iron seeds to form heavier s -process elements. Finally, as the metallicity decreases, the production of elements up to the Ba or Pb peak increases at the expense of the Sr-peak elements.

Classical Be stars are key laboratories for investigating how rapid rotation, pulsations, and mass loss couple to the formation and evolution of circumstellar decretion disks. However, few studies have combined Kepler/K2 photometry with multi-epoch Hα monitoring. Here we present four previously unclassified Be-type variable stars observed by K2 (three in Campaign 11 and one in Campaign 15) and followed up with ground-based spectroscopy. We analyzed public PDC light curves and extracted variability frequencies using Lomb–Scargle periodograms and iterative prewhitening with a conservative detection threshold of S/N ≥ 5. Optical spectra obtained at the Observatório Pico dos Dias (Brazil) over a multi-year baseline (2017–2025) include repeated Hα observations and blue-region spectra for photospheric characterization. All targets show detectable K2 variability on timescales from hours to days, with frequency spectra ranging from close multi-periodic components producing beating patterns to power dominated by low frequencies. Each star exhibits Hα emission at multiple epochs, with long-term changes in line-profile morphology and equivalent width, indicating disk variability on year-long timescales. These results demonstrate that disk evolution can occur without conspicuous photometric outbursts over the time span of space-based observations, highlighting the diagnostic value of combining high-precision space photometry with long-term spectroscopy to characterize multiscale variability in Galactic Be stars.

Abstract We present the first X-ray polarimetry observations of a redback millisecond pulsar binary, PSR J1723−2837, with the Imaging X-ray Polarimetry Explorer (IXPE). We conduct a spectropolarimetric analysis combining IXPE data with archival Chandra, XMM-Newton, NuSTAR, and Swift observations. We explore two limiting magnetic field configurations, parallel and perpendicular to the bulk flow, and simulate their expected polarization signatures using the 3DPol radiative transport code. To account for the rapid rotation of the polarization angle (PA) predicted by these models, we implement a phase-dependent Stokes alignment procedure that preserves the polarization degree (PD) while correcting for a phase-rotating PA. We also devise a new maximum likelihood fitting strategy to determine the phase-dependence of the PA by minimizing the PD uncertainty. This technique hints that the binary may be rotating clockwise relative to the celestial north pole. We find no significant detection of polarization in the IXPE data, with PD ≲50% at the 99% confidence level. Our results exclude the high-PD scenario predicted by the perpendicular field model during the brightest orbital phase bin. Simulations show that doubling the current exposure would make the parallel configuration detectable. The new PA rotation technique is also applicable to IXPE data of many sources whose intrinsic PA variation is a priori not known but is strictly periodic.

Copper nanoclusters represent a promising yet underdeveloped frontier in materials science. Here, we propose a general and efficient strategy for enhancing photothermal conversion efficiency through the incorporation of rotor-stator ligand architectures onto copper nanocluster surfaces. As a representative example, we design carboxylate ligands functionalized with adamantane groups to stabilize a [Cu36(4-F-PhS)24(AdmCOO)6(PPh3)4H8]2- nanocluster. In this architecture, the adamantane unit functions as a molecular rotor, while the carboxylate group serves as a molecular stator. The engineered nanocluster achieves a photothermal conversion efficiency of 75%. The adamantane rotors exhibit a lowered rotational energy barrier within the cluster framework, enabling stable and rapid molecular rotation that effectively promotes non-radiative transitions. This mechanism optimizes the conversion of light into thermal energy, enabling the nanocluster to rapidly heat up to 200 °C under 445 nm laser irradiation at a power density of 1.0 W cm-2. The proposed strategy could be applicable to other rotor types, yielding a broad family of copper nanoclusters with enhanced photothermal conversion capabilities and multifunctional potential.

Based on 5298 positional observations, we determined the radial, transversal, and normal components of the nongravitational accelerations A1, A2, and A3 within the framework of the Marsden model and we also estimated the corresponding quantities for the alternative dependences of the acceleration on heliocentric distance: 1/r0, 1/r2, 1/r3, and 1/r4. We have shown that all the nongravitational acceleration models considered, when determined simultaneously with the coordinates and velocities at the chosen epoch, yield almost the same level of agreement with observations—the only exception being the constant-acceleration model (1/r0). Notably, the derived values of nongravitational accelerations exceed those characteristics of both Solar System comets and the first known interstellar comet, 2I/Borisov. In every model considered, the relationship |A1|/|A2| < 1 holds, meaning that the total nongravitational acceleration deviates markedly from the sunward direction, since the radial and transverse components are mutually perpendicular. This can be attributed either to rapid rotation of the nucleus or to pronounced inhomogeneity of its surface. For the dependencies proportional to 1/r0, 1/r3, and 1/r4, as well as in the Marsden model, the value of the parameter A1 proves to be negative. An analysis of the O–C values (differences between the observed and calculated positions) revealed no statistically significant periodic variations. Using the inject-and-recover test, we estimated the upper limit on the amplitude of hypothetical periodic O–C variations, at which their period could be reliably recovered from the available observational data.

Repeated traumatic brain injury (TBI) is a significant concern among military personnel, athletes, and abuse victims. However, little is known about the mechanisms that drive the brain's apparent increase in injury susceptibility with repeated loading. One critical factor may be the softening of cerebral blood vessels, which are significantly stiffer than brain tissue and influence its mechanical response during trauma. In this study, we employed a finite element model of a Göttingen minipig head to investigate how progressive vascular softening influences strain changes in brain tissue during both repeated blast and rapid rotation. The model incorporated pig-specific anatomical detail and material properties, including detailed cerebral vasculature. Simulations included six repeated exposures of either blast overpressure or coronal or sagittal rotations at varying severity levels. Additional "no-vasculature" (NV) cases were included for each loading condition to benchmark the mechanical contribution of blood vessels. Vessel softening was applied after each exposure based on previous experiments on Göttingen minipig cerebral arteries. While blast exposures did not generate sufficient strain to induce vessel softening, rotational events led to progressively increasing brain strain with repetition, especially in regions adjacent to softened vessels. These increases progressed toward the NV condition with repetition, consistent with diminishing structural support by softened vessels. Results also showed increasing risk of vessel rupture and axonal injury with repetition. These findings elucidate the biomechanical role of vessel softening in repeated TBI and suggest that even sub-failure vessel damage may exacerbate brain strain in repeated exposures and elevate injury risk.

Mild traumatic brain injury (mTBI) is underdiagnosed and can lead to long-term symptoms in children. Currently, we lack diagnostic markers and effective therapies for pediatric mTBI. MicroRNAs (miRNAs) show promise for diagnosing and treating pediatric mTBIs due to their role in regulating key biological processes. Cyclosporine A (CsA) has also shown therapeutic effectiveness in modulating neuronal recovery and protection. We aimed at studying miRNA changes in the frontal lobe (FL) and hippocampus + amygdala (H&A) after a sagittal rapid non-impact head rotation (RNR) in 4 week old piglets (N = 50) at 1 day post-injury, 1 week post-injury, and following 1 day of 20 mg/kg/day Cyclosporine A (CsA) treatment compared to anesthesia-only shams. Interestingly, many miRNAs involved in disrupted neuronal and upregulated glial, epithelial, and endothelial functions were differentially expressed (DE-miRNAs) at 1 day post-injury and most returned to baseline by 1 week post-injury. However, miR-20a-3p, miR-10386, and miR-4331-3p were among the Top 10 DE-miRNAs at 1 day post-injury, and remained altered at 1 week. Upregulated neuroprotective miR-17-3p and miR-212 were also part of the Top 10 DE-miRNAs at 1 day post-injury, and their increases were correlated with decreases in axonal injury. Furthermore, to identify miRNAs that could serve as candidate diagnostic biomarkers of injury, we employed LASSO analysis and identified miRNAs miR-363, miR-15b, and miR-450c-3p as the best predictors of mTBI at 1 day post-injury. Lastly, WGCNA revealed the possible neuroprotective effects of CsA treatment in ameliorating neuronal, immune, stress, and vascular functions disrupted at 1 day post-injury. Overall, our data revealed key miRNAs that were differentially expressed at 1 day and 1 week post-injury, modulated by CsA treatment, and suggest that they may serve as diagnostic biomarkers of pediatric mTBI.

In recent years, there has been no shortage of research achievements in light-responsive materials based on azobenzene photoswitches. Of growing interest is the ability to reversibly tune the competing "dark" thermal cis-trans back-isomerization through protonation effects. The hydroxy-substituted azobenzenes are well-known for their complex pH-dependent behavior, including azo-hydrazone tautomerism. Presently, experimental studies rationalize only qualitatively the marked acceleration in thermal switching upon acquiring the hydrazone tautomer, while the results of theoretical treatments have experienced a persistent cusp problem in calculated potential energy surfaces. Here, using density functional theory, spin-flip, and multireference wavefunction quantum chemical methods, we provide for the first time a comprehensive explanation of thermal switching in the hydrazone tautomer. We show that, through concerted torsion of two dihedral angles, the hydrazone tautomer unexpectedly acquires a maximally puckered transition state, enabling rapid rotation of the entire system. This study demonstrates the exploitative advantages of protonation for tuning thermal isomerization in azobenzene photoswitches.

Buried pipelines in mountainous regions are highly vulnerable to lateral landslides, which generate complex soil–pipe interactions and multi-axial deformation. This study develops a principal strain–azimuth coupling method and applies it to 1:75 centrifuge model tests to quantify pipeline responses under controlled landslide loading. High-resolution strain rosettes were used to monitor both principal strain magnitudes and their orientations. Before sliding, only minor settlement-induced deformation and stable azimuth patterns were observed. Once landsliding initiated, the pipeline exhibited rapid azimuth rotations of 20–40° and clear asymmetry between tensile and compressive strains. Soil density and moisture strongly affected the response: higher dry density increased maximum tensile strain by approximately 2.7%, whereas high-moisture soil produced larger shear–torsional effects and frequent azimuth fluctuations. At 75 g, maximum tensile strain reached 0.53–0.64% and maximum compressive strain reached 0.71–0.84%, exceeding ASCE allowable limits. In the high-moisture test, deformation resulted from a combination of settlement-induced bending and landslide-driven lateral displacement. Importantly, azimuth rotation consistently preceded strain accumulation, demonstrating its potential as a leading indicator of soil–pipe interaction changes. These findings provide quantitative evidence supporting early-warning monitoring strategies and offer design guidance for improving the resilience of pipelines in landslide-prone regions.