Spiral Disks Research Articles

Spiral excitation in protoplanetary disks through gap-edge illumination

The advent of high-resolution, near-infrared (NIR) instruments such as VLT/SPHERE and Gemini/GPI has helped uncover a wealth of substructure in planet-forming disks, including large, prominent spiral arms in MWC 75 8, SAO 206462, and V1247 Ori. In the classical theory of disk-planet interaction, these arms are consistent with Lindblad-resonance driving by companions of multiple Jupiter masses. Despite improved detection limits, evidence for massive bodies like this in connection with spiral substructure has been inconclusive. In search of an alternative explanation, we used the PLUTO code to run 3D hydrodynamical simulations with two comparatively low planet masses (Saturn mass and Jupiter mass) and two thermodynamic prescriptions (three-temperature radiation hydrodynamics, and the more traditional β-cooling) in a low-mass disk. In the radiative cases, an m = 2 mode, potentially attributable to the interaction of stellar radiation with gap-edge asymmetries, creates an azimuthal pressure gradient, which in turn gives rise to prominent spiral arms in the upper layers of the disk. Monte Carlo radiative transfer post-processing with RADMC3D revealed that in NIR scattered light, these gap-edge spirals are significantly more prominent than the traditional Lindblad spirals for planets in the mass range we tested. Our results demonstrate that even intermediate-mass protoplanets, which are less detectable, but more ubiquitous than super-Jupiters, are capable of indirectly inducing large-scale spiral disk features, and underscore the importance of including radiation physics in any efforts to reproduce observations.

Euclid preparation

The Euclid mission is expected to image millions of galaxies at high resolution, providing an extensive dataset with which to study galaxy evolution. Because galaxy morphology is both a fundamental parameter and one that is hard to determine for large samples, we investigate the application of deep learning in predicting the detailed morphologies of galaxies in Euclid using Zoobot, a convolutional neural network pretrained with 450 000 galaxies from the Galaxy Zoo project. We adapted Zoobot for use with emulated Euclid images generated based on Hubble Space Telescope COSMOS images and with labels provided by volunteers in the Galaxy Zoo: Hubble project. We experimented with different numbers of galaxies and various magnitude cuts during the training process. We demonstrate that the trained Zoobot model successfully measures detailed galaxy morphology in emulated Euclid images. It effectively predicts whether a galaxy has features and identifies and characterises various features, such as spiral arms, clumps, bars, discs, and central bulges. When compared to volunteer classifications, Zoobot achieves mean vote fraction deviations of less than 12% and an accuracy of above 91% for the confident volunteer classifications across most morphology types. However, the performance varies depending on the specific morphological class. For the global classes, such as disc or smooth galaxies, the mean deviations are less than 10%, with only 1000 training galaxies necessary to reach this performance. On the other hand, for more detailed structures and complex tasks, such as detecting and counting spiral arms or clumps, the deviations are slightly higher, of namely around 12% with 60 000 galaxies used for training. In order to enhance the performance on complex morphologies, we anticipate that a larger pool of labelled galaxies is needed, which could be obtained using crowd sourcing. We estimate that, with our model, the detailed morphology of approximately 800 million galaxies of the Euclid Wide Survey could be reliably measured and that approximately 230 million of these galaxies would display features. Finally, our findings imply that the model can be effectively adapted to new morphological labels. We demonstrate this adaptability by applying Zoobot to peculiar galaxies. In summary, our trained Zoobot CNN can readily predict morphological catalogues for Euclid images.

Radio continuum emission from a tidal dwarf galaxy

ABSTRACT Tidal dwarf galaxies (TDGs) form in the debris of galaxy mergers, making them ideal testbeds for investigating star formation in an extreme environment. We present radio continuum EVLA observations spanning 1–2 GHz of the interacting system Arp 94, which contains the TDG J1023+1952. We detect extended radio continuum emission from the disc of the TDG’s putative parent galaxy, the spiral NGC 3227. The TDG lies in front of the spiral disc, partially overlapping in projection. This challenging alignment complicates the separation of the respective contributions of radio emission from the TDG and disc. However, we show that the radio continuum appears more prominent around the TDG’s location, suggesting the detection of emission from the TDG. Quantifying this argument, we derive an upper limit of 2.2 mJy for the whole TDG’s emission. Our derived inband spectral index map of the system generally shows the expected behaviour of combined thermal and synchrotron radio emission in a galaxy disc, except for a region at the periphery of the disc and the TDG with a flat spectrum (spectral index $\sim$−0.4) unrelated to regions with high H $\alpha$ emission. We speculate that at this location – which coincides with the intersection of faint tidal tails – the collision of gas clouds produces shocks which re-accelerate cosmic ray electrons, and thereby enhance the radio emission. Overall, this study provides new insights about the Arp 94 system and expands the sample of TDGs studied at radio frequencies, with only two confirmed detections so far.

Analysis of fluid flow and heat transfer in CNT-infused spiraling disk

This study investigates the fluid flow and heat transfer characteristics influenced by the thermophysical properties of carbon nanotube suspension in engine oil over a stretching-spiraling disk. The surface comprises Homan stagnation point flow impinging normal to a rotating, radially stretching disk, which gives velocity a form of logarithmic spiral. Similarity ansatz transformed coupled nonlinear differential equation system is derived and solved numerically using MATLAB’s bvp4c collocation method. Numerical and asymptotic solutions are also obtained against the controlled parameters via graphical representations and tabular data. Findings indicate that the magnetic field enhances temperature distribution while reducing the velocity field. At the same time, stretching increases radial velocity but decreases azimuthal velocity and temperature profiles, regardless of carbon nanotube type. The asymptotic values of skin friction decline with an increase in the spiralisng angle and in the absence of a magnetic field for both SWCNTs and MWCNTs cases.

JWST/NIRCam Imaging of Young Stellar Objects. I. Constraints on Planets Exterior to the Spiral Disk Around MWC 758

MWC 758 is a young star hosting a spiral protoplanetary disk. The spirals are likely companion-driven, and two previously identified candidate companions have been identified—one at the end the Southern spiral arm at ∼0.″6, and one interior to the gap at ∼0.″1. With JWST/NIRCam, we provide new images of the disk and constraints on planets exterior to ∼1″. We detect the two-armed spiral disk, a known background star, and a spatially resolved background galaxy, but no clear companions. The candidates that have been reported are at separations that are not probed by our data with sensitivity sufficient to detect them−nevertheless, these observations place new limits on companions down to ∼2 M Jup at ∼150 au and ∼0.5 M Jup at ≳600 au. Owing to the unprecedented sensitivity of JWST and youth of the target, these are among the deepest mass-detection limits yet obtained through direct imaging observations, and provide new insights into the system’s dynamical nature.

Finishing and polishing systems influence the roughness and color stability of acrylic and bis-acryl composite resins.

To evaluate the effect of different finishing and polishing systems on the surface roughness and color changes of bis-acryl (Protemp 4 - 3M ESPE- St. Paul, USA; Structur 3 - Voco, Cuxhaven, Germany) and chemically activated acrylic materials (Duralay - Reliance, SP, Brazil). Specimens (10 x 2 mm) thick were prepared for each material. The specimens were subjected to polishing and finishing procedures with aluminum oxide discs (Diamond Master - FGM, Joinville, Santa Catarina, Brazil) and spiral rubber disks (Sof-Lex - 3M ESPE, Germany). The control did not receive any polishing and finishing procedures. Surface roughness and color measurement values were obtained after the finishing and polishing procedures and immediately after 30 days of storage in water, coffee, and red wine. Data for each material were analyzed by One-Way ANOVA (p<0.05). The polishing with aluminum oxide discs was able to affect the initial surface roughness values of chemically activated acrylic material (p<0.05). After immersion in staining solutions, lower ∆E values were only observed for the bis-acryl composite resins compared to the control group (p<0.05). The finishing and polishing systems influenced the surface roughness and color stability of the materials tested. The chemically activated acrylic resin showed lower surface roughness and higher color stability than the bis-acryl materials. Key words:Acrylic resin, bis-acryl resin, provisional restoration.

A new design method for the vortex hydrogen circulating pump system

Against the backdrop of “carbon peak and carbon neutrality,” the hydrogen and fuel cell vehicle industry are rapidly developing. Within the on-board hydrogen supply system, the hydrogen circulation pump serves as an essential component of the hydrogen fuel cell system. The spiral disk, as a core part of the hydrogen fuel cell system’s vortex hydrogen circulation pump (VHCP), plays a crucial role in determining the performance of the hydrogen circulation system in hydrogen fuel cell vehicles. To meet the requirements for high-performance and high-reliability development of the hydrogen circulation pump, the VHCP scheme is adopted as the choice for the hydrogen pump solution. Through the magnetic suspension and no connection shaft structural design, the feasibility of applying the high speed and high flow hydrogen turbine was initially validated. Utilizing Fluent analysis software and high precision performance test bench, a comprehensive three-dimensional numerical simulation of the turbine design under various operating conditions was conducted and performance test verification, demonstrating that the performance meets the required specifications. By conducting research in both strength optimization design and performance requirement, two major technical challenges in turbine pump application were overcome. Combined with the experimental results of the turbine medium, it is concluded that the vortex pump can meet the flow and pressure rise under the premise of low power consumption in the hydrogen circulation system so as to perfectly increase the hydrogen return amount. Based on these findings, recommendations are proposed for the future development direction of hydrogen supply systems in hydrogen fuel cell vehicles.

Stellar Bars in Isolated Gas-rich Spiral Galaxies Do Not Slow Down

Elongated bar-like features are ubiquitous in galaxies, occurring at the centers of approximately two-thirds of spiral disks in the nearby Universe. Due to gravitational interactions between the bar and the other components of galaxies, it is expected that angular momentum and matter will redistribute over long (Gyr) timescales in barred galaxies. Previous work ignoring the gas phase of galaxies has conclusively demonstrated that bars should slow their rotation over time due to their interaction with dark matter halos. We have performed a simulation of a Milky Way–like galactic disk hosting a strong bar, including a state-of-the-art model of the interstellar medium and a live dark matter halo. In this simulation, the bar pattern does not slow down over time, and instead it remains at a stable, constant rate of rotation. This behavior has been observed in previous simulations using more simplified models for the interstellar gas, but the apparent lack of secular evolution has remained unexplained. We find that the presence of the gas phase arrests the process by which the dark matter halo slows down a bar, a phenomenon we term bar locking. This locking is responsible for stabilizing the bar pattern speed. We find that, in a Milky Way–like disk, a gas fraction of only about 5% is necessary for this mechanism to operate. Our result naturally explains why nearly all observed bars rotate rapidly and is especially relevant for our understanding of how the Milky Way arrived at its present state.

Enhancing energy transport in Homann stagnation-point flow over a spiraling disk with ternary hybrid nanofluids

The incorporation of nanoparticles is highly desirable due to their capability to enhance thermal conductivity, which promotes efficient heat dissipation, enhances the performance and reliability of heat-generating/absorption systems. This study investigates the effects of three types of nanoparticles, magnetic field, stretching and rotation of disk on the Homann stagnation point flow. The gold, polystyrene, and polymethylmethacrylate nanoparticles are drenched in ethanol to make a ternary hybrid nanofluid. The governing equations are transformed via similarity transformations, and the resulting system is solved numerically by using the finite difference method. The effects of the nanoparticle's concentration, stretching-rotation of surface, and magnetic field on the velocity, temperature, skin friction, and Nusselt number are analyzed. The mechanism contributes to augment the thermal conductivity of the fluid, resulting in an elevation in temperature and a reduction in velocity. Stretching of the surface promotes the acceleration of fluid particles, leading to higher velocities. On the other hand, the decline in temperature is due to the stretching-induced expansion of the fluid, which reduces the thermal energy. The study provides valuable insights into the complex interactions between nanoparticles, stretching, rotation, and magnetic field on the flow properties and may have practical implications in the design and optimization of nanofluid-based systems for various applications.

Universal gravity-driven isothermal turbulence cascade in disk galaxies

While interstellar gas is known to be supersonically turbulent, the injection processes of this turbulence are still unclear. Many studies suggest a dominant role of gravitational instabilities. However, their effect on galaxy morphology and large-scale dynamics varies across cosmic times, in particular, due to the evolution of the gas fraction of galaxies. In this paper, we propose numerical simulations to follow the isothermal turbulent cascade of purely gravitationally driven turbulence from its injection scale down to 0.095 pc for a gas-poor spiral disk and a gas-rich clumpy disk. For this purpose, and to lift the memory-footprint technical lock of sufficiently resolving the interstellar medium of a galaxy, we developed an encapsulated zoom method that allows us to self-consistently probe the self-generated turbulence cascade over three orders of magnitude on spatial scales. We followed this cascade for 10 Myr. We find that the turbulent cascade follows the same scaling laws in both setups. Namely, in both cases, the turbulence is close to equipartition between its compressive and solenoidal modes, the velocity power spectrum follows the Burgers scaling, and the density power spectrum is rather shallow, with a power-law slope of −0.7. Last, gravitationally bound substructures follow a mass distribution with a −1.8 slope, similar to that of CO clumps. These simulations thus suggest that gravity-driven isothermal turbulent cascades are universal in disk galaxies across cosmic time.

Tuning magneto-electric coherent resonance with a deep-subwavelength localized spoof surface plasmonic structure.

It has been recently shown that an ultrathin corrugated spiral metal strip can simultaneously support electric and magnetic localized spoof plasmonic modes at lower frequencies. In this Letter, we report a mirror quasi-symmetrical corrugated spiral metal disk which can support coherent resonance of an orthogonal electric dipole and a magnetic dipole to achieve azimuthally symmetric unidirectional scattering. By tuning the geometric dimensions, reconfigurable magneto-electric (ME) coherent resonance enhancement is realized. Excellent agreement between numerical simulations and experimental results verifies the tunable ME coherent resonance phenomenon. Our finding could anticipate future sensitive and versatile functional devices based on high-Q coherent resonance from the microwave to the terahertz bands.

Energy transport near Homann stagnation point flow over a spiraling disk with Cattaneo–Christov theory

In this paper, axisymmetric magnetohydrodynamic (MHD) Homann flow is studied normally over a stretching and spiraling disk in the stagnation region. Homann’s problem is modified with simultaneous effects of the radial linear stretching and uniform rotation of the disk. The magnetic field is applied perpendicular to the motion of the flow. The energy and mass distribution phenomena are analyzed by using Cattaneo–Christov (CC) double diffusion model, heat sink/source and chemical reaction effects. The main purpose of this study is to highlight the significance of CC theory on Homann problem along with asymptotic behavior. Similarly, ansatzes are utilized to transform the partial differential equations into ordinary differential equations. The solutions are computed numerically by a built-in scheme, namely, bvp4c in MATLAB. Moreover, it is concluded that the surface velocity is produced in the form of a spiral logarithm because of the continual activity of radial stretching and uniform rotation of the disk. The outcomes of magnetic field, rotation and stretching parameters are discussed graphically for coefficients of skin friction. The coefficient of skin friction along the [Formula: see text]-axis is enhanced, whereas along [Formula: see text]-axis, it is decreased by varying stretching and rotating parameters. The impact of thermal and solutal relaxation time coefficients reveals that they reduce the heat and mass transfer rates, respectively.

Numerical simulation for Tiwari–Das model for Homann flow of nanofluid due to a spiraling disk: A spectral technique

This study extracts heat transfer analysis for the axisymmetric flow of CuO-water nanofluid imposing normal to a spiraling disk uniformly rotating and radially stretching. The combined influence of uniformly rotating and linearly radial stretching surface engenders the logarithmic spirals in motion. The governing system is transformed into a system of the ordinary differential equations that represent the flow. The Tiwari–Das [Int. J. Heat Mass Trans. 50, 2002 (2007)] model is utilized to envisage the heat transfer and other physical properties of the nanofluid. A highly precise numerical technique named as Legendre wavelet-based spectral method is practiced to computing the impacts of the pertinent variables on the flow. The results of physical significance including the wall shear, skin frictions and heat transfer rate are attained for the multiple spiraling parameters and the nanoparticle volume fraction. The asymptotic results for the large spiraling parameter are also presented to analyze the flow behavior for the high spiraling parameter. The influence of the nanoparticles is also investigated and the enhancement in thermal conductivity is measured. The temperature and thermal layer thickness reduce for large spiraling parameter. Also addition of the nanoparticles enhances the heat transfer rate of the nanofluid.

Evaluation of different composite resin finishing and polishing protocols by confocal laser scan microscopy

Aim: This study aimed to analyze the influence of finishing and polishing (F/P) protocols on resin surface through roughness (Ra) values and laser scan microscopy observations. Methods: Forty-eight (n=48) resin specimens were sorted into four groups (n=12), according to the type of resin used: Filtek Z250 (Z250), Filtek Z350 (Z350), Filtek One Bulk Fill (BF), Filtek P60 (P60). The specimens were sorted into six groups according to the type of F/P system used (n=2/group): Control group, Diamond bur (KG Sorensen), Soflex Pop-On Discs (3M ESPE), Soflex Spiral (3M ESPE), Dura Gloss (American Burs), and Praxis (TDV). Results: The highest roughness values (Ra) were attributed to BF group for all F/P systems, except for the Soft-Lex PopOn discs. The Soft-Lex PopOn, Spiral, and Praxis discs presented a better performance for the surface treatment of the tested composite resins. Regardless of the restorative material, the use of diamond bur or single-step abrasive rubber (Dura Gloss) were associated with the highest Ra values. Conclusion: The effect of F/P systems on Ra is material-dependent and instrument or system-dependent.

Numerical simulation for stagnation-point flow of nanofluid over a spiraling disk through porous media

A computational study on the diverging stagnation point of fluid flow is carried out over a convective plate. In this research, the unfaltering three-dimensional flow and heat transfer of non-Newtonian carbon nanotubes (CNTs) have been scrutinized. In order to analyze the stagnation point and rate of heat transfer, Xue’s model has been taken into consideration. Through similarity transformations, analytical unfolding of the governing coupled, non-linear, and ordinary differential equations has been performed. The most profoundly effective methods, termed the Keller Box method and the shooting method, are utilized. Using these propositions for CNTs of single-wall and multiwall carbon nano tubes, the results are co-related. For various values of material parameters, porosity, skin friction, temperature, solid volume fraction, Nusselt number, and Prandtl number, calculations have been put through. On observing, it is revealed that the porosity parameter has increased and both radial and azimuthal velocities decrease. When the stretching ratio parameter is increased while the azimuthal velocity is decreased, the radial velocity increases. It has also been discovered that sheer stress increases in direct proportion to porosity and stretching parameter. However, the rate of heat transfer shows inverse behavior against these parameters. The significant effects of these parameters are illustrated through graphs.

Galactic component mapping of galaxy UGC 2885 by machine learning classification

Automating classification of galaxy components is important for understanding the formation and evolution of galaxies. Traditionally, only the larger galaxy structures such as the spiral arms, bulge, and disc are classified. Here we use machine learning (ML) pixel-by-pixel classification to automatically classify all galaxy components within digital imagery of massive spiral galaxy UGC 2885. Galaxy components include young stellar population, old stellar population, dust lanes, galaxy center, outer disc, and celestial background. We test three ML models: maximum likelihood classifier (MLC), random forest (RF), and support vector machine (SVM). We use high-resolution Hubble Space Telescope (HST) digital imagery along with textural features derived from HST imagery, band ratios derived from HST imagery, and distance layers. Textural features are typically used in remote sensing studies and are useful for identifying patterns within digital imagery. We run ML classification models with different combinations of HST digital imagery, textural features, band ratios, and distance layers to determine the most useful information for galaxy component classification. Textural features and distance layers are most useful for galaxy component identification, with the SVM and RF models performing the best. The MLC model performs worse overall but has comparable performance to SVM and RF in some circumstances. Overall, the models are best at classifying the most spectrally unique galaxy components including the galaxy center, outer disc, and celestial background. The most confusion occurs between the young stellar population, old stellar population, and dust lanes. We suggest further experimentation with textural features for astronomical research on small-scale galactic structures.

Recent Formation of a Spiral Disk Hosting Progenitor Globular Clusters at the Center of the Perseus Brightest Cluster Galaxy. I. Spiral Disk

Abstract We address the nature and origin of a spiral disk at the center of NGC 1275, the giant elliptical galaxy at the center of the Perseus cluster, that spans a radius of ∼5 kpc. By comparing stellar absorption lines measured in long-slit optical spectra with synthetic spectra for single stellar populations, we find that fitting of these lines requires two stellar populations: (i) a very young population that peaks in radial velocity at ±250 km s−1 of the systemic velocity within a radius of ∼720 pc of the nucleus, a 1σ velocity dispersion significantly lower than 140 km s−1, and an age of 0.15 ± 0.05 Gyr; and (ii) a very old population having a constant radial velocity with a radius corresponding to the systemic velocity, a much broader velocity dispersion of ∼250 km s−1, and an age of around 10 Gyr. We attribute the former to a post-starburst population associated with the spiral disk, and the latter to the main stellar body of NGC 1275 along the same sight line. If the spiral disk is the remnant of a cannibalized galaxy, then its progenitor would have had to retain an enormous amount of gas in the face of intensive ram-pressure stripping so as to form a total initial mass in stars of ∼3 × 109 M ⊙. More likely, the central spiral originally comprised a gaseous body accreted over the distant past from a residual cooling flow, before experiencing a starburst ∼0.15 Gyr ago to form its stellar body.

Recent Formation of a Spiral Disk Hosting Progenitor Globular Clusters at the Center of the Perseus Brightest Cluster Galaxy. II. Progenitor Globular Clusters

Abstract We address the nature and origin of super star clusters (SSCs) discovered by Holtzman et al. within a radius of ∼5 kpc from the center of NGC 1275, the giant elliptical galaxy at the center of the Perseus Cluster. We show that, in contrast with the much more numerous population of SSCs subsequently discovered up to ∼30 kpc from the center of this galaxy, the central SSC population have maximal masses an order of magnitude higher and a mass function with a shallower power-law slope. Furthermore, whereas the outer SSC population have ages spanning a few Myr to at least ∼1 Gyr, the central SSC population have ages strongly concentrated around ∼500 Myr with a 1σ dispersion of ∼100 Myr. These SSCs share a close spatial and temporal relationship with the “central spiral,” which also has a radius ∼5 kpc centered on NGC 1275 and a characteristic stellar age of ∼150 Myr. We argue that both the central SSC population and the central spiral formed from gas deposited by a residual cooling flow, with the SSCs forming first followed by the formation of the stellar body of the central spiral ∼300–400 Myr later. The ages of the central SSC population imply that they are able to withstand very strong tidal fields near the center of NGC 1275, making them genuine progenitor globular clusters. Evidently, a spiral disk hosting progenitor globular clusters has recently formed at the center of a giant elliptical galaxy.

Electrical conductivity characterized at varying strains in spiral cut high-pressure torsion discs

High-pressure torsion (HPT) imparts inhomogeneous strain to process discs with low strain in the center and higher strain at the outer edge. Microscopy and microhardness indentation have been used to characterize and correlate this inhomogeneity with strain, but similar exploration with other properties has been uncommon. In this work, the electrical conductivity of pure copper discs processed by HPT was characterized with respect to equivalent strain by cutting them into spirals with an incremental, monotonic increase in strain. Electrical conductivity varied with straining in agreement with the literature and expectations based on grain boundary evolution. The spiral conductivity testing method outlined in this work can improve characterization of HPT materials in future studies.

Evaluation of Bulk Fill Composite Roughness Polished with Spiral Rubber Discs: An In-vitro Study

Introduction: Restorations with high surface roughness directly influences restorative procedure longevity. When used correctly, polishing systems optimizes the quality, aesthetics and longevity of composite resins. Aim: To evaluate the influence of three two-step polishing systems of spiral rubber discs on surface roughness of three different bulks fill composite resins. Materials and Methods: This in-vitro study was conducted from May, 2021 to January 2022, at the Universidade Estadual de Pernambuco, School of Dentistry, Recife, Pernambuco, Brazil. Total 20 specimens of each resin {three Bulk Fill resins: Filtek One Bulk Fill (3M-ESPE), Aura Ultra Universal Restorative Bulk Fill (SDI) and Opus Bulk Fill (FGM)} were randomly divided into four groups (n=5 each). The three groups include test polishing systems {Sof-Lex Diamond Polishing System (3M/ ESPE, Saint Paul, Minnesota, USA), Decamp Plus Twist Spiral EVE (Odon omega, Ribera Prato, SP, Brazil), Spiral Swivel (Jota, Ruth, Kanton St. Gallen, Switzerland)} and one control group include no polishing system. To assess surface roughness, before and after polishing, specimens were evaluated on a digital rugosimeter. Data was subjected to the Shapiro-Wilk test to assess normality, followed by Analysis of Variance (ANOVA) to compare the mean between the different types of resins and types of polishers. Results: For the composite resins studied, significant differences were observed only when polished with Soflex Spiral (p-value=0.013). All polishing system caused a significant improvement in the roughness of composite resins compared to the control group. The mean roughness reduction comparison test between the types of polisher was significant (p-value &lt;0.001), there was a significantly greater reduction in the roughness of EVE Decamp Plus Twist Spiral and Swivel Spiral polish system, compared to polish system from Sof-Lex Diamond Polishing System and control group. No statistically significant differences were found between EVE Diacomp Plus Spiral and Spiral Swivel polishing system. Conclusion: The spiral rubber polishers evaluated were effective in reducing the roughness of bulk fill composites. However, EVE Decamp Plus Spiral and Spiral Swivel polishers showed better results than Sof-Lex Spiral.