The cosmic web contains most of the matter in the Universe, and its filamentary structure is closely related to the properties of dark matter. Compared with the cold dark matter (CDM) model, warm dark matter (WDM) suppresses the formation of low-mass halos and produces smoother cosmic filaments. In this work, we explore whether filamentary 21cm emission can be used to distinguish between these two dark matter models at z=4 and 2.5. We generate intrinsic 21cm brightness temperature maps from cosmological hydrodynamical simulations and produce mock observations by convolving them with Gaussian beams of different angular resolutions. We then compare the predicted filament signals with the expected sensitivities of SKA1-Low and SKA2-Low. We find that the intrinsic 21cm emission clearly reflects the different filament morphologies in the CDM and WDM models, particularly at z=4. However, these differences rapidly disappear as the beam size increases, especially for beam sizes larger than 6 arcsec. Although larger beams improve the observational sensitivity, they also erase the small-scale structures that encode the dark matter information. As a result, neither SKA1-Low nor the planned SKA2-Low can directly resolve individual filaments with sufficient sensitivity to distinguish between the two models. We therefore conclude that direct imaging of cosmic filaments and constraining dark matter through their morphology are unlikely to be feasible with current and planned SKA-Low facilities.
Abstract We use the Stetson, {\it Hubble Space Telescope (HST)}, and {\it Gaia} DR3 data sets for each of 22 Galactic globular clusters to select their members and fit their colour--magnitude diagrams with isochrones from the Dartmouth Stellar Evolution Database and a Bag of Stellar Tracks and Isochrones for $\alpha$--enrichment $[\alpha/$Fe$]=+0.4$ and a helium mass fraction $Y$ adopted for a combination of stellar generations. As a result, we estimate the metallicity $[$Fe$/$H$]$, age, distance from the Sun, and reddening $E(B-V)$ for these clusters. Special attention is paid to identify variable stars among the cluster members, since they affect the derived parameters and statistics. We combine these results with our earlier estimates for five other clusters into a homogeneous set of parameters for 27 clusters and investigate relationships among these parameters and their statistical properties. In particular, we count the giants on the red (RGB), horizontal (HB), and asymptotic branches using the clean data sets cross-identified to cover the entire cluster fields and count each giant only ones. This allows us to calculate the $R$-parameter, the ratio between the numbers of the HB and RGB, with unprecedented accuracy and to examine its relations with other parameters. These relations are much stronger for accreted clusters rejecting a constant $R$ value for them, possibly because of their heterogeneous origins and environments. For all in-situ clusters, a constant value of $R=1.31^{+0.06}_{-0.05}$ is consistent with the data. According to previous calculations, this value may imply anomalous energy losses in HB stars corresponding to an axion--photon coupling of $g_{a\gamma}=(0.66^{+0.11}_{-0.13})\times10^{-10}\,\mathrm{GeV}^{-1}$. However, the observed dependencies of $R$ on cluster parameters were not accounted for in previous studies. Any future study of the $R$ parameter aimed at constraining exotic particle-physics models will therefore require not only improved statistics, but also a theoretical understanding of these dependencies and their incorporation into the analysis. By comparing $R$-parameter estimates from {\it HST} and {\it Gaia} in cluster centres and peripheries, respectively, we suggest that the peripheral HB population is depleted by about half when the cluster crosses the Galactic disk, then the HB recovers over 60--80 Myr.
Abstract This paper reports a single-pulse analysis of five pulsars using the FAST. The analysis results show that pulse nulling is detected in all five pulsars. Among them, the pulse nulling of PSR J1907+4002 is reported for the first time. The nulling fractions (NFs) are calculated. The values for PSRs J0304$+$1932, J0528$+$2200, J0754$+$3231, J1115$+$5030 and J1907$+$4002 are 14.50$\pm$1.00\%, 28.50$\pm$2.00\%, 32.10$\pm$1.50\%, 60.40$\pm$1.50\% and 12.20$\pm$0.90\%, respectively. The newly measured NFs are compared with those from published literature. No obvious evidence supports a strong frequency dependence of the NFs for these pulsars. A check for correlations among NFs, spin period, and characteristic ages shows no obvious dependence. It should be noted that these correlations require further investigation using observations from a larger pulsar sample, as the current sample size is too limited to confirm any definitive correlation. Furthermore, a discrete Fourier transform (DFT) analysis of pulse nulling periodicity reveals that these pulsars likely exhibit quasi-periodic nulling behavior. An analysis of two-dimensional fluctuation spectra (2DFS) further indicates that the periodic amplitude modulation observed in these pulsars may arise from pulse nulling. Subpulse drifting is only observed in PSRs J0528+2200 and J1115+5030. This work not only enriches the observational sample of pulse nulling and subpulse drifting, but also provides important observational constraints for further understanding the radiation mechanisms in pulsar magnetospheres.
Abstract The 44-cm Visible Telescope (VT) aboard the Space-based Variable Objects Monitor (SVOM) is a dual-band (400–650 nm and 650–1000 nm) instrument designed to detect and characterize the optical counterparts of gamma-ray bursts (GRBs) and other high-energy transients. This paper presents the VT's design, scientific objectives, observation strategies, and space/ground data processing pipelines, alongside its first-year in-orbit performance. In-orbit commissioning tests confirm a sensitivity of 22.5 AB mag (300 s exposure), extendable to ~24 AB mag through stacking. This performance enables the VT to monitor over 100 GRBs in the first year with an exceptional $\sim80\%$ detection rate for SVOM/ECLAIRS-triggered bursts and promptly observed bursts from other missions (e.g., \textit{Swift, Fermi, Einstein Probe (EP)}), outperforming \textit{Swift}/UVOT’s $\sim40\%$ rate. Beyond its exceptional detection efficiency, the VT played a key role in identifying high-redshift GRBs—most notably GRB 250314A (z = 7.3). Its deep upper limits at long wavelengths (up to 1 $\mu m$) were pivotal in guiding follow-up observations with large ground-based telescopes, enabling crucial near-infrared (NIR) detections. With its rapid response, deep sensitivity, and real-time processing capabilities, the VT is a key instrument for GRB research in \textit{SVOM}-era, enabling critical studies of GRB optical afterglows, circumburst environments, relativistic jet dynamics, and the origins of optically dark bursts.
To investigate the driving mechanisms of orbital evolution across different mass ratios and evolutionary stages, we present the first multi-color photometric solutions and detailed orbital period analyses for four short-period eclipsing binaries: MX Ser, AY Pup, QW And, and TZ CrA. By analyzing the light curves using the Wilson-Devinney code, we determined the absolute parameters and geometric configurations for these systems. MX Ser (q = 4.60) and AY Pup (q = 2.02) have been identified as W-subtype contact binaries with medium fill-out factors of f similar to 30%. QW And (q = 0.51) is derived as an A-subtype contact binary (f approximate to 32%) exhibiting significant magnetic activity modeled by a cool starspot. In contrast, TZ CrA (q = 0.31) is confirmed to be a semi-detached Algol-type system with a large temperature difference (Delta T approximate to 2175 K), where the secondary component fills its Roche lobe while the primary remains detached. The orbital period analyses based on all available minimum times reveal that all four systems are undergoing continuous secular period decreases. We attribute these variations to different physical mechanisms governed by the mass ratio (q). For the high mass-ratio systems MX Ser and AY Pup (q > 1), the period decrease is dominated by conservative mass transfer from the massive secondary to the primary, consistent with the thermal relaxation oscillation (TRO) theory. For the low mass-ratio systems QW And and TZ CrA (q < 1), the period decrease is the net result of competing mechanisms, where angular momentum loss (AML) via magnetic braking completely overwhelms the mass transfer effect. The derived evolutionary status suggests that while MX Ser, AY Pup, and QW And are evolved contact binaries, TZ CrA represents a critical "pre-contact" stage (short-period Algol). Driven by efficient AML, the detached primary of TZ CrA is expected to eventually fill its Roche lobe, evolving the system into an A-subtype W UMa contact binary.
Abstract Quantifying the terrestrial response of solar variability across the 11-year Schwabe cycle remains an open challenge in solar-terrestrial physics, due to the dominance of anthropogenic warming signals and the limitations of conventional statistical approaches. We present a Physics-Informed Neural Network (PINN) constrained by the zero-dimensional energy balance equation C dT /dt = αS(t) + γ CO2(t) − βT (t), trained on 1488 months of detrended global surface temperature anomalies (1900--2023). By jointly minimising data misfit and the energy balance residual, the PINN learns forcing parameters directly from observations while remaining physically constrained. The model achieves R^2 = 0.844 +/- 0.002 on held-out test data, compared to R^2 = 0.178 for conventional multiple linear regression (MLR) applied to the same detrended dataset, demonstrating that physics-constrained temporal modelling provides both the predictive skill and the parameter stability that instantaneous regression and unconstrained temporal models cannot simultaneously achieve. The found learned solar sensitivity α = 0.088 +/- 0.001 is physically consistent with published estimates of solar climate sensitivity. Spectral analysis of the model-isolated solar component independently recovers the Schwabe solar cycle at ~10.2 yr without prior specification of the expected period. The solar forcing share expressed as α/(α + γ) = 15.5 +/- 0.3%, stable across five independent training realisations, quantifies the solar contribution to total modelled radiative forcing sensitivity in the detrended residual record. Applying the same framework across spatial scales reveals systematic degradation of predictive skill from global to urban station scale (R^2 = 0.844 to R^2 ~0), while the solar share remains physically consistent (14.7--18.5 +/- 0.5%) across all converging analyses. A historical Riyadh-city station independently recovers a dominant spectral peak consistent with the mean Schwabe period (11.0 +/- 0.5 yr) with R^2 = 0.577 +/- 0.060, confirming the presence of the solar signal in pre‑urban Arabian Peninsula desert temperature records. The scale‑dependent degradation in model performance demonstrates that anthropogenic urban processes may elevate the effective thermal noise floor beyond the detectable amplitude of the solar signal, with implications for solar–terrestrial studies relying on urban ground‑station datasets. An ablation study confirms that the energy balance physics constraint --- rather than the LSTM temporal memory alone --- is the primary driver of parameter stability and interpretability. Removing this constraint destabilizes the solar attribution from 15.3 +/- 0.6% to 62 +/- 32% across training seeds.
Abstract VT (Visible Telescope) is an optical telescope aboard SVOM mission, specifically designed to detect optical counterparts of gamma-ray bursts, study their afterglows, and select high-redshift candidates. It performs rapid follow-up observations simultaneously in two channels through either autonomous platform slewing or Target of Opportunity (ToO) observations. The science images acquired by VT and transmitted via the X-band downlink system are designated as VT X-band data. This paper provides an overview of GRB optical afterglow identifications with VT and describes the ground-based processing pipeline for VT X-band data, including preprocessing, astrometric calibration, and photometry. Up to December 3th, 2025, VT has followed up 111 GRBs triggered by SVOM or external missions. The overall detection rate of optical counterparts is approximately 75%. Specifically, for bursts detected by SVOM/ECLAIRs, the detection rate is 77% when observed by VT within 30 minutes after the burst. A slightly higher detection rate of 81% is achieved for GRBs triggered by external missions through rapid ToO observations with a mid-time of less than 3 hours.
The tilt of bipolar sunspot groups regulates polar-flux transport and shapes the solar cycle. Using the Debrecen Photoheliographic Data, we introduce the first classification of sunspot groups into positive, negative, and random tilt types based on their tilt evolution. These classes show distinct statistical and dynamical behaviors: positive and negative groups follow coherent tilt relaxation on timescales of several days and exhibit classical and anti-Joy trends, whereas random tilt groups-the most numerous-display multimodal frequency distributions, short coherence times, and strong variability. All three classes follow the familiar sunspot butterfly pattern of equatorward migration, with random and negative groups showing enhanced longitudinal asymmetry. Long-term trends reveal stable mean tilts for positive groups, declining tilts for negative groups, and hemisphere-dependent changes for random groups. This tripartite tilt classification highlights fundamentally different evolutionary behaviors that shape magnetic-flux redistribution and provide improved constraints for solar-cycle and flux-transport modeling.
Abstract Fast radio bursts (FRBs) are one of the most enigmatic phenomena in modern astronomy. In observations, these transient radio emissions can be categorized into two distinct classes: repeaters and non-repeaters. For repeaters, periodic activities play an important role in understanding their progenitors and radiation mechanisms. To date, only two FRBs, FRB 20121102 and FRB 20180916B, have been confirmed to exhibit cyclical activity, with periods of approximately 160 days and 16 days, respectively. Recently, FRB 20240209A has been identified as a potential candidate with periodicity of approximately four months. In this study, we propose to use the $k$-means clustering algorithm to derive possible periods of active repeaters from bursting time observations. Moreover, the method successfully re-detects the known period of FRB 20180916B, as well as the previously reported candidate periods of FRB 20121102A and FRB 20240209A. These findings are in excellent agreement with previous results and a strong indication for the potential of machine learning approaches in uncovering hidden patterns in FRB data, which may otherwise remain obscured by observational noise and complexity. As more observational data become available and machine learning methodologies continue to evolve, such computational tools are expected to play an increasingly crucial role in advancing our understanding of FRBs, potentially revealing new insights into their physical origins, environmental contexts, and underlying emission mechanisms.
Abstract Target allocation in multi-object spectroscopic surveys is a high-dimensional combinatorial optimization problem constrained by fiber reachability and mechanical collisions. In densely populated focal planes, local assignment decisions can induce non-local conflicts, whereby a single choice suppresses multiple neighboring opportunities, leading to reduced survey completeness and biased target selection. Existing approaches typically rely on fast heuristic or priority-driven algorithms, which, while operationally efficient, do not fully capture the global conflict structure and therefore yield suboptimal weighted target assignments in dense regimes. In this work, we reformulate the fiber assignment problem as a Maximum Weight Independent Set (MWIS) problem on a conflict graph, providing a unified representation of geometric and mechanical constraints. Building on this formulation, we develop a Graph Neural Network (GNN)–based solver that leverages iterative message passing to model long-range dependencies across the focal plane. This approach enables the propagation of constraint information over the full conflict network, effectively mitigating the ``ripple effect" induced by local collisions and allowing for globally consistent optimization. We validate the proposed method using both real observations from the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) and simulated dense focal-plane configurations. The results demonstrate that our approach achieves significantly higher weighted yields than traditional heuristic baselines, reaching up to 99.71\% of the optimal solution while maintaining computational efficiency compatible with survey operations. The method consistently produces collision-free assignment plans and exhibits robust performance across varying target densities. Importantly, the proposed graph-based framework is independent of specific hardware geometries, making it directly applicable to a broad class of fiber-fed spectroscopic surveys, including Dark Energy Spectroscopic Instrument–like systems. This work establishes a scalable and physically motivated paradigm for fiber assignment, bridging combinatorial optimization and data-driven modeling, and provides a pathway toward improving survey completeness and mitigating selection biases in next-generation spectroscopic programs.
Abstract We present the results of unfiltered and $BR$ photometry of SN Ia 2025asm. We determine the decline rate parameter $\Delta m_{15}(B)=1.85$ mag and maximum absolute magnitude $M_B=-18.85$ mag, these data allow to conclude that SN\,2025asm is among the brightest type Ia SNe with high decline rate. We reveal that SN 2025asm does not belong to 1991bg-like SNe, its light and color curve and maximum luminosity show similarity with ``transitional'' type Ia SN iPTF13ebh. The location of SN\,2025asm in a group of galaxies, far beyond the borders of nearby galaxies, indicates that its progenitor belongs to old stellar population.
Using multi-wavelength imaging and spectroscopic observations from the New Vacuum Solar Telescope (NVST), the Chinese H alpha Solar Explorer (CHASE), and the Solar Dynamics Observatory (SDO), we investigate a highly twisted magnetic structure associated with a filament eruption in active region NOAA 13762 during 2024 July 25-26. Initially, several jets were triggered along coronal loops by magnetic flux emergence, resulting in an exchange of loop footpoints toward the emerging negative polarity. Meanwhile, distinct brightenings were observed at the interface between two filament segments, accompanied by photospheric magnetic flux cancellation. Subsequently, the two filament segments merged into a single filament. The merged filament later erupted, exhibiting a highly right-handed twisted magnetic structure, while its threads displayed a left-handed rotational motion. This behavior suggests that the filament interacted with nearby closed magnetic fields, injecting magnetic twist into the surrounding coronal system. The total twist of the magnetic structure during the eruption is estimated to be about 2.59 turns, implying that the original filament possessed an intrinsic twist of approximately 1.59 turns. During the later phase of the eruption, several brightenings and moving bright threads exhibiting right-handed rotational motion or bidirectional propagation were observed, after which the structure evolved into a less twisted configuration. We propose that the magnetic twist was partially transported to the surrounding coronal loop through magnetic reconnection during the twist-transfer stage. The observed brightenings and moving threads are interpreted as signatures of magnetic reconnection occurring between the edge of the highly twisted structure and surrounding coronal loops. These results provide new insight into the transfer of magnetic twist during the interaction between a highly twisted filament and surrounding closed magnetic loops.
Abstract COLIBRÍ, the French–Mexican Ground Follow-up Telescope (FM-GFT) for SVOM, is a 1.3-meter rapid-response optical facility specifically developped for prompt, multi-band observations of GRB afterglows and for delivering sub-arcsecond localizations of optical counterparts for detailed follow-up studies. The telescope operates through a fully automated system that manages the entire workflow—from alert reception to counterpart identification. Commissioning results confirm that the telescope meets design specifications, and this paper presents a comprehensive performance assessment of the system’s capabilities.
Abstract Following the orbit insertion of the Einstein Probe satellite, we conducted the first five-month test monitoring campaign of 1E 2259+586, 4U 0142+61, and 1E 1048.1−5937 using the Follow-up X-ray Telescope. No significant bursting activity was detected from any of the three sources during this interval. Timing analysis reveals that the spin peri- ods of 1E 2259+586 and 4U 0142+61 remained stable, with measured frequencies of 0.143279150(2) Hz and 0.115001270(2) Hz, respectively. In contrast, 1E 1048.1−5937 ex- hibited a measurable spin-frequency derivative of −20(3) × 10−15, with a spin frequency of 0.154749612(5) Hz. Spectral analysis indicates that the soft X-ray emission is well described by either an absorbed double blackbody model or a blackbody plus power-law model. Under the blackbody plus power-law model, the best-fit parameters are: for 1E 2259+586, Γ ∼ 3.61, kT ∼ 0.42 keV, and an unabsorbed flux of 1.613 × 10−10 erg cm−2 s−1, for 4U 0142+61, Γ ∼ 3.31, kT ∼ 0.37 keV, and an unabsorbed flux of 1.937 × 10−10 erg cm−2 s−1, and for 1E 1048.1−5937, Γ ∼ 3.21, kT ∼ 0.66 keV, and an unabsorbed flux of 4.52 × 10−10 erg cm−2 s−1. The blackbody temperatures (kT ≈ 0.3 − 0.7 keV) are consistent with thermal emission from the hot neutron star surface. The power-law component exhibits a pho- ton index of Γ ≈ 3 − 4, indicating a soft spectrum that is likely produced by magnetospheric radiative processes. By leveraging the high spatial resolution and superior imaging capabil- ities of EP-FXT, this study presents a comprehensive diagnostic of the timing and spectral properties of these magnetars, demonstrating the unique value of EP-FXT for characterizing dynamic celestial sources.
Abstract We present the in-orbit calibration of the Visible Telescope (VT), one of the key instruments aboard the Space Variable Objects Monitor (\textit{SVOM}) mission for gamma-ray burst (GRB) studies. Using \textit{Gaia}~Data Release 3 (DR3) as a reference, the VT achieves an astrometric precision better than $0.03''$ for bright stars, degrading to $\sim 0.25''$ for faint targets. Shortly after launch, contamination was detected, reducing system transmission by $\sim40\%$. An initial bake-out successfully restored performance, but gradual recontamination caused transmission to decline by $\sim20\%$ over the following 100 days before stabilizing. Despite this effect, routine standard star observations maintain precise zero-point calibration, ensuring a photometric stability of $0.02$ mag. Using synthetic stellar spectra, we derived photometric transformations to the \textit{Gaia}, SDSS, and Johnson-Cousins systems with typical residuals of $0.03$ mag. These results demonstrate the VT system's capability and reliability in calibrating GRBs and other transients.
We present a statistical study of the global physical properties of dwarf galaxies to investigate the processes governing galaxy formation in the low-mass regime, with particular emphasis on comparing classical and Bayesian regression approaches. A unified catalog of 722 dwarf galaxies was compiled by combining structural, photometric, chemical, and dynamical data from multiple observational sources. Using Pearson, Spearman, and Kendall correlation analyses, we identify significant scaling relations among galaxy mass, luminosity, metallicity, surface brightness, size, and neutral hydrogen content, and derive both classical least-squares and Bayesian linear regressions to quantify these dependencies. We find that intrinsic relations among mass, luminosity, metallicity, surface brightness, and H I mass reflect the underlying baryonic physics within dark matter-dominated haloes. A systematic comparison shows that Bayesian regression generally yields steeper slopes for several key relations, indicating that classical methods tend to underestimate the strength of physical dependencies when measurement uncertainties and intrinsic scatter are not fully accounted for. In particular, strong mass-luminosity, mass-metallicity, and mass-surface brightness relations-further reinforced by Bayesian analysis-highlight the key role of halo mass in regulating star formation efficiency and metal retention. These trends are consistent with predictions of the Lambda cold dark matter framework, where stellar feedback and gas retention processes shape the baryonic structure of low-mass galaxies. Our results provide robust empirical constraints on galaxy formation models and demonstrate the importance of Bayesian methods for accurately characterizing scaling relations, serving as a reference for testing hydrodynamical simulations and theoretical models of dark matter-baryon interactions.
Abstract Discovering new pulsars is crucial for advancing astrophysics and fundamental physics. Conventional pulsar searches require dedispersion under various dispersion measures (DMs) before period detection, which is computationally intensive, especially for blind searches. In this paper, we introduce a novel dispersion-independent period detection (DIPD) method that eliminates the need for dedispersion prior to period analysis. By constructing a composite period searching (CPS) spectrum, DIPD method preserves harmonic spectral lines of pulsar signals without prior DM knowledge. An efficient and general fundamental detection and harmonic search algorithm then identifies candidate pulsar periods directly from this spectrum. The data can subsequently be folded at the estimated period, enabling a more efficient DM search on the folded data to extract the valid pulsar signal from the candidates. The algorithm was verified by observational data. The results show that DIPD method achieves accurate pulsar detection with fewer invalid candidates while significantly reducing computational cost compared with traditional pipelines such as PRESTO. This approach offers a promising avenue for accelerating large-scale pulsar surveys.
Abstract The SVOM (Space-based Variable Objects Monitor) mission, launched into low Earth orbit on 22 June 2024, is a French-Chinese multi-wavelength observatory dedicated to the study of the transient sky. Inspired by the Neil Gehrels Swift Observatory, it consists of an autonomous rapid-slewing satellite, linked in real time to several ground-based telescopes. The space segment comprises two X-ray/gamma-ray wide-field instruments (ECLAIRs and GRM) with real-time triggering capabilities combined with two narrow-field telescopes in X-ray (MXT) and in visible (VT). In addition, the SVOM collaboration has also developed a unique visible and NIR ground-based follow-up system to promptly respond to the gamma-ray transients detected on board. The core program of SVOM will provide new insights into the Gamma-Ray Burst physics by providing a homogeneous dataset covering both the prompt and afterglow emissions, as well as better studying the low luminosity and soft Gamma-Ray Burst populations. As a versatile satellite platform with fast slewing capabilities, SVOM also proposes a Target-of-Opportunity program and a General Program consisting in pointed observations scheduled over the year that will both significantly contribute to the multi-messenger and time-domain astronomy.
Abstract The SVOM Visible Telescope (VT) is critical for the rapid identification of gamma-ray burst (GRB) optical counterparts, particularly for high-redshift candidates that require immediate infrared spectroscopic follow-up. To address the stringent bandwidth constraints of the VHF downlink while ensuring real-time data availability, we developed the VT Onboard Data Processing Pipeline (VOPP). This paper details the software architecture, algorithms, and hardware implementation of VOPP using an FPGA and a CPU. The pipeline performs essential real-time tasks, including image quality assessment, dark and flat-field correction, and optimized image stacking to mitigate cosmic ray contamination and variable background noise. Furthermore, it generates compact source catalogs and highly compressed 1-bit images to facilitate rapid downlink. In-flight performance analysis confirms the pipeline’s robustness, demonstrating availability of VT VHF data for 78% of promptly slewed SVOM GRBs, with 56% leading to the identification of optical counterparts, typically within 18 minutes post-trigger.
The phenomenon of multiple stellar populations (MPs), characterised by star-to-star variations in light-element abundances, is a ubiquitous feature of globular clusters (GCs). While spectroscopic surveys have directly revealed these abundance anomalies, photometric studies, particularly with the Hubble Space Telescope (HST), have been instrumental in characterizing MP sequences across the colour-magnitude diagrams (CMDs). However, the narrow field of view of the HST has restricted these studies to only a small portion of the star clusters, leaving the vast majority of the clusters' space unexplored. The upcoming Chinese Space Station Survey Telescope (CSST), with its wide field of view and both UV and optical capabilities, will provide new opportunities for systematic MP studies. We aim to quantify the capability of the CSST wide-field camera in detecting and characterizing MPs in GCs through virtual simulations that closely mimic real observations. We performed comprehensive simulations using synthetic stellar population models incorporating different helium abundances (Delta Y) and carbon-nitrogen-oxygen (CNO) variations. We simulated CSST observations for GCs at distances of about 9.6 kpc and 20 kpc with different exposure times. We evaluated the detection efficiency of MPs based on the CMDs constructed from the seven different bands of the CSST, as well as the pseudo color-color diagrams (chromosome diagrams) designed with the UV-optical combination. For a GC at a distance of approximately 9.6 kpc, the NUV - u color index of the CSST is highly sensitive to stellar populations with different Delta Y and CNO abundances in the CMD, providing color separations of Delta(NUV - u) approximate to 0.16 (for red giants) to 0.44 mag (for dwarfs). We find that when the total exposure time in the UV band exceeds similar to 1000 s and the exposure time in the optical band exceeds similar to 300 s, the main survey camera of CSST is sufficient to resolve these MPs. Furthermore, extending the simulations to 20 kpc, a distance encompassing similar to 80% of Galactic GCs, we demonstrate that the SCam retains significant diagnostic power, resolving stellar populations with Delta Y >= 0.06 dex and delta[N/Fe] >= 0.64 dex, and distinguishing MPs in the CMD down to i similar to 19.5 mag for clusters with substantial chemical dispersions. The combination of NUV-u-g filters provides diagnostic capabilities comparable to HST's F275W-F336W-F438W system. CSST will be a powerful facility for MP studies, capable of efficiently surveying the entire spatial extent of several hundred star clusters in the local group. Its wide field of view and multi-band capabilities will enable the first homogeneous MP census spanning the entire Milky Way and its neighbouring galaxies, significantly advancing our understanding of star clusters' formation and chemical evolution.
