How receptor conformation depends on lipid nanodisc size: Adenosine A2A receptor and implications for class-A GPCR proteins.

SCN1B encodes the β-subunits of the main cardiac voltage-gated sodium channel, Na V 1.5. Variants are linked to cardiac conduction disease, often with concealed phenotypes. Whether β1-subunits regulate conduction through nanoscale intercalated disc (ID) structures, e.g. perinexi, and ephaptic coupling remains unresolved. Test whether Scn1b haploinsufficiency induces latent conduction abnormalities that are unmasked by perturbations in extracellular nanodomains. Adult Scn1b+/- mice and wild-type (WT) littermates underwent multiscale phenotyping (qRT-PCR, Western blot, patch clamp, transmission electron microscopy (TEM), ex vivo optical mapping, in vivo ECG). Scn1b+/- hearts showed ∼50% reductions in Scn1b mRNA and β1 protein without changes in canonical conduction proteins. Peak sodium current, baseline conduction velocity ex vivo , and baseline QRS duration in vivo were unchanged. However, TEM revealed increased baseline perinexal width in Scn1b+/- hearts. Osmotic expansion of the perinexus with mannitol slowed conduction to a greater extent in Scn1b+/- hearts and prolonged QRS duration in vivo . In contrast, perinexal narrowing with dextran 2MDa selectively increased conduction velocity in Scn1b+/- hearts. Scn1b haploinsufficiency preserves baseline excitability and conduction but structurally remodels the ID at the nanoscale, increasing sensitivity to extracellular nanodomain perturbations. These data support a structural role for β1-subunits in ephaptic coupling, and that conduction is maintained over a range of perinexal widths with pathological conduction slowing occurring beyond a critical width. Importantly, osmotic stress unmasks a concealed conduction phenotype, identifying extracellular nanodomain stability as a potential therapeutic target to mitigate arrhythmia risk in SCN1B -associated disease.

The ubiquitous presence of nanoplastics (NPs) has drawn widespread attention for their accumulation in reproductive tissues, posing latent threats to the delicate retina. Nevertheless, the transgenerational effects of maternally transferred NPs on embryonic retinal morphogenesis and functional development remain largely uncharacterized. Here, we microinjected 60 nm polystyrene NPs (PS-NPs) into the animal pole of zebrafish zygotes to simulate maternal exposure. PS-NP exposure caused pronounced effects in zebrafish larvae at 3 days postfertilization (dpf). At this key developmental stage, exposed larvae developed microphthalmia. Confocal imaging revealed that PS-NPs were broadly distributed across retinal layers, with a preferential accumulation in the vicinity of photoreceptor region. Histological analysis revealed significant thinning of the photoreceptor outer segments (OS) accompanied by marked morphological abnormalities. Transmission electron microscopy confirmed substantial OS shortening and disorganization of disc structures, characterized by reduced disc thickness, increased spacing, and decreased flatness. In addition, mitochondrial swelling with disrupted cristae was observed, along with alterations in retinal pigment epithelium (RPE) melanosomes. Immunofluorescence analysis also indicated aberrant signal expression across multiple retinal cell types, including photoreceptors and RPE cells. Transcriptome profiling revealed that differentially expressed genes were significantly enriched in key visual cycle-related pathways, particularly those associated with retinol binding. These findings were corroborated by gene set enrichment analysis (GSEA) and reverse transcription quantitative polymerase chain reaction (RT-qPCR) validation. Additional RT-qPCR assays indicated activation of oxidative stress and inflammatory pathways. Notably, OS thickness remained significantly reduced compared with controls at 14 dpf, while some phenotypic abnormalities gradually diminished at later developmental stages (5, 10, and 14 dpf). Collectively, these results support a model in which the RPE-OS functional unit represents a primary target of 60 nm PS-NPs. Both direct physical damage and subsequent oxidative stress and inflammatory responses likely contribute to its dysfunction, ultimately impairing RPE function, disrupting OS renewal, and promoting photoreceptor degeneration. These findings highlight the potential visual risks associated with maternally derived nanoparticle exposure.

Bruxism-related clenching can impose excessive mechanical loads on the temporomandibular joint (TMJ), particularly in the presence of anterior disc displacement (ADD). Understanding how different therapeutic strategies influence joint stress under these conditions can support exploratory, hypothesis-generating assessment of biomechanical unloading within patient-specific models. Therefore, this study aimed to evaluate TMJ stress distributions under normal and displaced disc conditions and to assess the biomechanical effects of simulated treatment strategies using a patient-specific finite element framework. A patient-specific three-dimensional finite element model derived from clinically acquired computed tomography (CT) data was constructed to simulate TMJ biomechanics during clenching. Stress patterns were analyzed under three disc conditions: normal disc position, unilateral ADD, and bilateral ADD. Intervention scenarios included simulated reductions in masticatory muscle forces representing botulinum toxin Type-A (BoNT-A) therapy and occlusal splint therapy, applied individually and in combination. Peak von Mises stresses within the articular disc and joint structures were compared across all conditions. ADD increased peak stresses within the articular disc and adjacent joint surfaces and shifted stress concentration toward the posterior region of the disc. Simulated reductions in muscle force resulted in progressive decreases in peak joint stresses as additional muscle groups were targeted, whereas splint therapy alone provided moderate stress reduction. The greatest biomechanical unloading was observed when occlusal splint therapy was combined with BoNT-A-related muscle force reduction. Notably, a strategy targeting the masseter and temporalis muscles combined with splint therapy produced lower peak disc stresses than a three-muscle reduction strategy without splint across all disc conditions. In this exploratory single-patient finite element model, ADD increased predicted TMJ stresses during clenching, whereas simulated muscle-force reduction and splint-related changes in occlusal load transmission reduced peak stress metrics, with the largest reductions observed in combined scenarios. These results are hypothesis-generating and intended for relative, within-model comparisons under stated assumptions rather than clinical treatment recommendations.

Context . The inner regions of planet-forming disks hold invaluable insights for our understanding of planet formation. The inner disk regions that might be affected by already formed planets are of particular interest. The disk around the Herbig star HD 100453 presents one such environment, with an inner disk that is significantly misaligned with respect to the outer disk. Aims . This paper expands the existing H band (PIONIER) and K band (GRAVITY) interferometric studies of the inner disk of HD 100453 to the L band with the MATISSE VLTI instrument. Based on snapshot data spanning approximately four years, we aim to understand the inner disk structures and their potential time evolution better. Methods . Based on the MATISSE data we obtained, we used a combination of analytical models and image reconstruction to constrain the disk structure. Additionally, we fitted a temperature gradient model to the selected wavelength range of PIONIER, GRAVITY, and MATISSE to derive the physical properties of the inner regions. Results . Our parametric model determined an inclination of ≈47.5° and a position angle of ≈83.6°, which corroborates the strong misalignment of the inner to the outer disk. From the symmetric temperature gradient, we derive an inner disk radius of ≈0.27 au, with dust surface densities of Σ subl ≈ 10 −3.2 g/cm 2 and a vertical optical depth τ z,subl ≈ 0.1-0.06. Same-night MATISSE and GRAVITY observations show directional discrepancies that are inconsistent with a first-order azimuthally modulation ring. This indicates that higher-order asymmetries are required to explain the interferometric signals. This interpretation is further supported by a MATISSE snapshot image reconstruction that revealed a two-component asymmetric structure. Conclusions . The chromatic interferometric data reveal that higher-order asymmetries are probably required to explain the inner disk of HD 100453, which suggests a possible origin in dynamic interactions or disk instabilities. Coordinated multi-wavelength infrared interferometric observations with GRAVITY and MATISSE will be crucial to confirm these findings and uncover their underlying nature.

Abstract We analyze the inner debris disk around $\epsilon$~Eridani using simulated observations with the Cool-Planet Imaging Coronagraph (CPI-C). Using the radiative transfer code \texttt{MCFOST}, we generate synthetic scattered-light images and spectral energy distributions for three disk models that differ in inclination and radial extent, and compare these results with the anticipated performance of CPI-C. CPI-C can resolve disk structures down to $\sim$3~au, offering substantially finer spatial resolution than existing HST/STIS and Spitzer/IRS observations. Recovered inclinations and radial extents closely match the input models, constraining the disk geometry and informing potential planet-disk interactions in the $\epsilon$~Eri system. Although the cold Jupiter-like planet $\epsilon$~Eri~b is not detected in our simulations, polarimetric methods may enable detection of its reflected light. These results highlight the capability of next-generation coronagraphs to probe cold dust in nearby planetary systems.

Abstract Scattering of stars by interstellar clouds or massive clumps increases the stellar velocity dispersion and promotes a radial disk profile that is exponential. Here we show that such scattering reaches a steady-state distribution function of stellar eccentricity, after which eccentricity increases and decreases occur at equal rates. The implication is that clump/cloud scattering recircularizes eccentric stellar orbits, keeping the stellar velocity dispersion in a limited range. This recircularization regulates disk heating and maintains kinematic coherence, contributing to the longevity of disk structures. The eccentricity distribution function and the presence of recircularizing cloud–star interactions are independent of cloud mass, but the timescale to reach equilibrium decreases with increasing mass. The calculations are made in the simplest possible disk system to highlight the effects of scattering without contamination from spiral waves, star formation, and other processes. The calculations also reveal a bifurcation in the disk evolutions whereby in a minority of cases, temporary asymmetries in the clump spatial distribution drive the disks to an end state of increased velocity dispersion and orbital eccentricity corresponding to early-type disks. Overall, the models emphasize an important physical process that can make and maintain an exponential stellar disk in all galaxies with a cloudy interstellar medium.

In this third study of the ‘Resolving supermAssive Black hole Binaries In galacTic hydrodynamical Simulations’ (Rabbits) series we develop and implement a geometrically thin relativistic accretion disc model, which self–consistently evolves the mass and spin vector of black holes via analytically modelling the structure of steady–state accretion discs. The model employs a suite of relativistic, local solutions where pressure is dominated by either gas or radiation, while opacity is primarily governed by either electron scattering or free-free absorption. These local solutions are piece–wisely combined to form the global structure of the accretion disc based on each solution’s range of validity. By explicitly modelling the structure of accretion discs, the model mitigates the stochasticity inherent in Bondi-type prescriptions, resulting in an approach where every episode of black hole mass accretion is derived from first principles. For the first time, our model enables galaxy formation simulations to place constraints on accretion disc sizes and structures. In addition, flux and temperature radial profiles can be directly extracted from the simulation, enabling the generation of spectral energy distributions (SED). Consequently, by incorporating the thermal structure and spacetime geometry around spinning black holes, our model more accurately captures the energetic output of quasars, overcoming critical limitations of classical approaches. Along with this manuscript, we make public a C version of the model appropriate to be used as a module in simulations, a Python version of the model that can be used independently to post–process any simulation and build mock accretion discs, and an updated version of the Relagn model that has the capability of producing SEDs by building an accretion disc for a given set of parameters and extracting its surface density, temperature, and opacity profiles.

Purpose To compare optic disc morphology and peripapillary structures in patients with varying degrees of myopia using swept-source optical coherence tomography, and to analyze their correlation with the peripapillary choroidal vascularity index. Methods Patients aged 18–40 years with myopia were enrolled. Patients were divided into three groups according to spherical equivalent refraction: group A (low myopia, −3.00 D < spherical equivalent ≤ −0.5 D), group B (moderate myopia, −6.00 D < spherical equivalent ≤ −3.00 D), and group C (high myopia, spherical equivalent ≤ −6.00 D). We compared the incidence and area of parapapillary atrophy in the β-zone (β-parapapillary atrophy) and the γ-zone (γ-parapapillary atrophy). The incidence and degree of optic disc tilt and optic disc rotation were also compared. We further examined differences in peripapillary choroidal thickness and peripapillary choroidal vascularity index among the groups. Linear regression analysis evaluated the relationships between peripapillary choroidal vascularity index and these parameters. Results In groups with higher myopia, the incidence and area of parapapillary atrophy, as well as optic disc tilt, increased. No significant difference in optic disc rotation was observed among the groups; however, downward optic disc rotation was more common in groups with higher myopia. Temporal peripapillary choroidal thickness was positively correlated with peripapillary choroidal vascularity index. The area of β-parapapillary atrophy showed a negative correlation with temporal, superior, and inferior peripapillary choroidal vascularity index. The area of γ-parapapillary atrophy was negatively correlated with temporal and nasal peripapillary choroidal vascularity index. Conclusion The parapapillary atrophy area increases in higher myopia groups. γ-parapapillary atrophy enlarges predominantly in low-to-moderate myopia. Downward optic disc rotation is more prevalent in highly myopic groups. Reduced temporal peripapillary choroidal thickness may indicate impaired peripapillary choroidal blood flow.

Abstract A giant planet embedded in a protoplanetary disk excites spiral density waves, which steepen into shocks as they propagate away from the planet. These shocks lead to secular disk heating and gap opening, both of which can have important implications for the evolution of solids near the planet. To date, these two effects have largely been modeled independently. In this study, we present a self-consistent model that unifies these processes by linking shock heating and angular momentum deposition through the entropy jumps across the spiral shocks. We show that this model accurately reproduces the temperature and surface density profiles around the planet’s orbit, as obtained from two-dimensional hydrodynamic simulations with standard $\alpha$ viscosity and $\beta$ thermal relaxation prescriptions. Furthermore, by incorporating an empirically derived scaling law for the radial distribution of the entropy jump, we construct a fully analytic model that self-consistently predicts the temperature and surface density structures of disks hosting a giant planet. This work represents a first step toward understanding how a giant planet forming in the inner disk region influences the distribution and composition of second-generation planets and planetesimals in its vicinity.

The radial drift and fragmentation of small dust grains in protoplanetary discs impedes their growth past centimetre sizes. Several mechanisms have been proposed to overcome these planet formation barriers, such as dust porosity or the streaming instability (SI), which is today regarded as the most promising mechanism to form planetesimals. Here, we examine whether the conditions for the SI to lead to strong clumping (the first step in planetesimal formation) are realised in protoplanetary discs containing porous grains. We used results from previous simulations of the evolution of porous grains subjected to growth, fragmentation, compaction, and bouncing in protoplanetary discs. In the ensuing disc structures, we determined the regions where the dust-to-gas ratio exceeds the critical value for strong clumping found in simulations of the SI including external turbulence. We find that the conditions for strong clumping are met within the first hundred thousand years in large regions of protoplanetary discs containing porous grains, provided that the CO snow line is taken into account. If the CO snow line is neglected, the conditions are only met very close to the inner disc edge early on or over large areas well after 200,000 yr.

We present measurements of key protoplanetary disk properties inferred from parametric models of ALMA 12 CO spectral line visibilities. We derived gas-disk radii, integrated fluxes, optically thick emission layers, and brightness temperature profiles for the disk population of the old (4–14 Myr) Upper Scorpius star-forming region. We measured CO emission sizes for 37 disks with bright CO J = 3–2 emission (S/N &gt; 10 on the integrated flux; out of the 83 disks with CO detections), finding that the median radius containing 90% of the flux is ∼82 au, with radii spanning from 22 up to 247 au. We report a correlation between the 12 CO brightness temperatures and stellar luminosities, with a Pearson coefficient of 0.6, which we used to prove that the 12 CO optically thick emission layer primarily emanates from a region below the superheated dust, which is optically thin to the stellar irradiation. Moreover, we derive 33 CO emission-surface height profiles, finding a median aspect ratio of ⟨ z/r ⟩ ∼ 0.16 in a range from ∼0.01 up to ∼0.45 over the sample. Finally, we comment on the multiple systems in our sample, of which only some were already known. These results confirm that it is possible to derive bulk disk properties by modeling moderate-angular-resolution ALMA visibilities.

We find the mature Galaxies. The massive black holes; very close to the Big Bang. The Star older than age of the Universe. The Spread Galaxies. The Galaxies without black matters at the periphery of the Universe. We have 85% Black matters in present expansion of the Universe, in 13.8 billion years. This is the remaining 15% The life of the Universe; Collapsing after maximum energy expansion, in all infinite opposite directions: revolving- Clockwise and anti-clockwise; in circular Disks, from minus infinite to plus infinite and visa - versa forming homogeneous Cloud. Clouds revolving Clockwise and Anti clockwise in circular Disks, These Disks pilling -up and down revolving Clockwise and Anti clockwise forming Various Structures in circular Disks. Disks Moving in clockwise or anti clockwise directions Their Structures having same Radial distances. Those moving in opposite directions receding coming Close or going away those coming Close showing blue Shift Those moving away Showing red shift. Some multi-billion Sun mass-black holes near the Big Bang are Showing very high red shift they are showing red Shift of 14 are being taken Towards Doomed Singularity They are looking brighter. And opaque: The Temperature not sufficient to make zero Viscosity solid light, so we have 92 billion years as the life of the Universe. It is Collapsing we have 13.8 billion years as the remaining life of the Universe, So we have 92 billion yrs as life of the Universe, Present age of the Universe is 80 billion years -Collapsing after Maximum energy Expansion of 92 billion light years. Singularity: Tachyon: Branes: expansion in all infinite opposite directions.

Abstract The majority of stars are born in clustered environments. In these environments, close encounters between young stars with planet-forming disks are expected to occur frequently. However, direct evidence of such interactions remains rare. Here, we report clear signatures of a recent dynamical interaction between the young stellar systems L1448 IRS3A and L1448 IRS3B. Millimeter wavelength observations reveal a distinct, tidally stripped bridge between the two systems. Together with previously reported spiral arm structures at the outer edge of the IRS3A disk and at the inner and outer regions of the IRS3B disk, these features imply that the systems are undergoing a dynamical flyby. Hydrodynamical simulations reproduce these features and suggest that the closest approach occurred about 15,000 yr ago. These findings offer rare insight into how stellar interactions can reshape disk structures and influence the formation of young multiple stellar systems.

Abstract We investigated the possibility of determining the mechanism of FU Orionis-type outbursts based on molecular line observations of protoplanetary disks with synthetic observations of distinct numerical burst models. The morphology of the synthetic C 18 O emission is sensitive to gas temperature and does not coincide with the actual gas disk structures, particularly in the magnetorotational instability (MRI) and clump-infall models, which exhibit peculiar temperature distributions. This highlights the need for careful interpretation of morphologies of line emission from disks under accretion outbursts. The synthetic C 18 O emission of each model exhibits distinct kinematic features that can be used to distinguish outburst scenarios. In the MRI model, kinematic features of the gravitational instability, which fuels MRI-driven accretion bursts, are small in both amplitude and spatial extent, resulting in no prominent local features in the residual velocity map at a typical distance for FU Orionis-type objects. In contrast, the clump-infall model shows a clear sign of gas expansion along a spiral, which is caused by exchange of angular momentum between an infalling clump and surrounding gas. The intruder model exhibits a highly asymmetric velocity structure with respect to the systemic velocity of the primary protostar in velocity channel maps. These distinct kinematic features may serve as promising diagnostics for distinguishing the physical mechanisms responsible for FU Orionis-type outbursts.

Abstract With its two stellar eclipses and two disk attenuations per binary orbit, V658 Carinae stands out as the first clear eclipsing Be + sdOB system. This rare alignment offers a unique opportunity to probe the structure and dynamics of a Be star disk with unprecedented detail. In this study, we present the most comprehensive observational data set and modeling effort for this system to date, including optical, near-infrared, and ultraviolet spectroscopy, space-based photometry, and optical polarization. Using a new ray-tracing code, we apply a three-component model, consisting of an oblate, rapidly rotating Be star, a symmetric circumstellar disk, and a compact stripped companion, to reproduce the system’s light curve, polarization, and spectral features. Our analysis yields precise constraints on the stellar and disk parameters, determining its status as the second-known late-type Be + stripped star, and also provides strong spectroscopic evidence for a tenuous circumsecondary envelope. Despite the model’s overall success, several key observables, such as the H α equivalent width and the secondary attenuation, remain poorly reproduced, pointing to the need for more sophisticated modeling. In particular, future improvements should incorporate the companion’s radiative feedback on the disk and account for asymmetric disk structures expected by the gravitational interaction with the companion. Owing to its unique geometry and rich diagnostics, V658 Car establishes itself as a benchmark system for Be stars (and rapid rotators in general), stripped stars, post-RLOF massive binaries, and circumstellar disk structures.

Abstract Planet formation may begin much earlier than previously expected, when the protoplanetary disk is still massive and gravitationally unstable. It has been proposed that solid grains can concentrate in the spiral arms of self-gravitating disks, leading to the formation of planetary embryos or cores that can greatly accelerate the process of planet formation. We perform hydrodynamic simulations of self-gravitating gas and even smaller dust grains than previously investigated in three-dimensional shearing box simulations to explore the conditions necessary to form these planetary seeds. Focusing on small grains of dimensionless stopping time St = 0.01 and shorter, we find that disk metallicities Z ≳ 0.02 can overcome the disruptive effects of dust diffusion among these small dust grains. In the outer reaches of a gravitationally unstable disk, these models correspond to grains of approximately 1 mm and lead to planetary embryos between 0.1 and 1 Earth mass. The formation of these planetary embryos could therefore reduce the time needed for planet assembly, particularly in the outer regions of the disk where coagulation timescales are longer and solid growth is limited.

Background: Cervicogenic headache (CGH) is a secondary headache that originates from dysfunction or pathology in the cervical spine and its associated bony, disc, or soft tissue structures, particularly the upper cervical segments (C1-C3). Investigation into PNF for cervicogenic headache management has demonstrated diverse outcomes concering pain relief, cervical mobility assessed the flexion-rotation test, and functional improvement. Objective: To study the Effectiveness of Proprioceptive Neuromuscular Facilitation (PNF) on cervicogenic headache. Method: In this experimental study ,40 participants diagnosed with cervicogenic headache received PNF treatment over a 4 week duration, with treatment sessions conducted three times weekly. The outcomes assessed were pain intensity using verbal analog scale, cervical mobility via the cervical flexion-rotation test, and functional disability using the neck disability index. Result: Analysis revealed mean difference scores of 5.45 ± 2.05 for VAS, 0.19 ± 0.09 for NDI, and 29.03 ± 38.08 for CFRT. The observed changes in all three parameters were statistically significant with p value &lt;0.0001. Conclusion: Based on the results , it can be conclude that proprioceptive neuromuscular facilitation (PNF) is an effective approach for reducing symptoms associated with cervicogenic headache. Keywords: PNF, Cervicogenic headache, NDI, Cervical flexion rotation test (CFRT)

Context . Beta Pictoris is an A-type star that hosts a complex planetary system with two massive gas giants and a prominent debris disc. Variable absorption lines in its stellar spectrum have been interpreted as signatures of exocomets – comet-like bodies transiting the star. Stellar flybys can gravitationally perturb objects in the outer comet reservoir, altering their orbits and potentially injecting them into the inner system, thereby triggering exocomet showers. Aims . We assessed the contribution of stellar flybys to the observed exocomet activity by reconstructing the stellar encounter history of β Pictoris in the past and future. Methods . We used Gaia DR3 data, supplemented with radial velocities from complementary spectroscopic surveys, to compile a catalogue of stars currently within 80 pc of β Pictoris. Their orbits were integrated backwards and forwards in time in an axisymmetric Galactic potential (via the GALA package) to identify encounters within 2 pc of the system. Results . We identified 99 416 stars currently within 80 pc of β Pictoris with resolved kinematics. Among these, 49 stars (including the eight components of five binaries) encounter β Pictoris within 2 pc between –1.5 Myr and +2 Myr. For four of the binaries, the centre-of-mass trajectories also pass within 2 pc. We estimated the sample to be more than 60% complete within 0.5 Myr of today. Conclusions . Despite β Pictoris being the eponym of its famous moving group, none of the identified encounters involved its moving group members; all are unrelated field stars. We found no encounter capable of shaping the observed disc structures, although stellar flybys may contribute to the long-term evolution of an Oort Cloud-like structure. Our catalogue constitutes the most complete reconstruction of the β Pictoris encounter history to date and provides a robust foundation for future dynamical simulations.

Aims . This study aims to characterize debris disk targets observed with SPHERE across multiple programs, with the goal of identifying systematic trends in disk morphology, dust mass, and grain properties as a function of stellar parameters. By combining scattered-light imaging with photometric and parametric modeling, we seek to improve our understanding of the composition and evolution of circumstellar material in young debris systems and to place debris disks in the broader context of planetary system architectures. Methods . We analyzed a sample of 161 young main-sequence stars using archival SPHERE observations at optical and near-infrared (IR) wavelengths. Disk geometries were derived from ellipse fitting and model grids, while dust mass and properties were constrained by modified blackbody (MBB) and size distribution (SD) modeling of spectral energy distributions (SEDs). We also carried out dynamical modeling to assess whether the observed disk structures can be explained by the presence of unseen planets. Results . We resolve 51 debris disks, including four new detections where disks are resolved for the first time: HD 36968, BD-20 951, and the inner belts of HR 8799 and HD 36546. In addition, we find a second transiting giant planet in the HD 114082 system, with a radius of 1.29 ± 0.05 R Jup and an orbital distance of ~1 au, providing an important new benchmark for planet–disk interaction studies. Beyond these new detections, we identify nine multi-belt systems, with outer-to-inner belt radius ratios of 1.5–2, and find close agreement between scattered-light and millimeter continuum belt radii with a mean ratio R belt (near-IR)/ R belt (mm) of 1.05 ± 0.04. Belt radii scale weakly with stellar luminosity ( R belt ∝ L ⋆ 0.11±0.05 ), but show steeper dependencies when separated by CO and CO 2 freeze-out regimes, and also increase with age as R belt ∝ t age 0.37±0.11 . Uniform image modeling yields vertical disk aspect ratios of 0.02–0.06, consistent with collisionally stirred belts, while gas-rich systems show unusually small values. Inner density slopes steepen with stellar luminosity, indicating more efficient dust removal around luminous stars. Disk fractional luminosities follow collisional decay trends, declining as t age −1.18±0.14 for A-type and t age −0.81±0.12 for F-type stars. SD modeling yields minimum grain sizes consistently above the blowout limit, typically &gt;0.8 μm, with a mean SD index of q = 3.6, assuming astrosilicate composition. The inferred dust masses span 10 −5 −1 M ⊕ from MBB modeling (and 0.01–1 M ⊕ from SD modeling for detected disks). These masses scale as R belt n with n &gt; 2 in belt radius and super-linearly with stellar mass, consistent with trends seen in protoplanetary disks (PPDs). Our detailed analysis of disk scattered-light non-detections indicates that they are mainly caused by low dust masses, unfavorable viewing geometries, or suboptimal observing conditions. SD modeling combined with Mie theory further shows that bulk albedos are consistently above 0.5 with little variation, making albedo differences an unlikely explanation. To explore this further, we introduced a new parametric approach based on scattered-light and polarized-light images, which provides independent estimates of dust albedo and maximum polarization fraction. We find a correlation between measured disk polarized flux and IR excess, with a slope shallower than that of optical total-intensity fluxes measured with HST/STIS. The offset of ~1 dex between total-intensity and polarized fluxes arises because polarized flux represents only a fraction of the total scattered light which depends on both grain properties and disk inclination. Finally, a comparison of planetary architectures shows that most benchmark systems resemble the Solar System, with multiple planets located inside wide Kuiper-belt analogues. Dynamical modeling further indicates that many observed gaps and inner edges can be explained by unseen planets below current detection thresholds, typically with Neptune- to sub-Jovian masses, underscoring the likely ubiquity of such planets in shaping debris disk morphologies.