New Astronomy最新文献

{"title":"An MHD simulation of the possible modulations of stellar CMEs radio observations by an exoplanetary magnetosphere","authors":"Soumitra Hazra ,&nbsp;Ofer Cohen ,&nbsp;Igor V. Sokolov","doi":"10.1016/j.newast.2025.102420","DOIUrl":"10.1016/j.newast.2025.102420","url":null,"abstract":"<div><div>Type II radio bursts are the indicator of adverse space weather in a stellar system. These radio bursts are the consequence of shock wave acceleration due to the coronal mass ejection (CME). In this study, we conduct a series of magnetohydrodynamic (MHD) simulations of CME-driven star–planet systems to investigate how close-in exoplanets modulate radio burst characteristics. We use a model for the stellar wind with a close-in exoplanet, and a CME model based on the eruption of a flux rope. We are able to generate synthetic radio burst images from our MHD simulations. We find that radio burst like phenomena is most likely to be observed for moderately active solar like stars and close-in exoplanetary systems have significant influence on the nature of radio burst spectrum. We find that when the exoplanet’s magnetic field is relatively weak, its magnetosphere compresses the CME plasma, increasing local density and shifting the radio emission to higher frequencies. Conversely, a strong planetary magnetic field results in a large magnetosphere that prevents effective CME-shock development, producing weaker radio emission concentrated at lower frequencies, particularly at the flanks of the CME. For highly active solar-like stars, strong overlying stellar magnetic fields suppress the CME shock, greatly diminishing radio burst visibility. For HD 189733 (moderate stellar field), only intensity difference is visible when the CME arrives the planet. We also do not find significant modulation in the radio emission by a close-in exoplanet system when the stellar magnetic field is complex. In summary, our findings highlight that the nature of the radio burst spectrum is strongly dependent on both the topology of the stellar magnetic field and the magnetic strength of close-in exoplanets.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"119 ","pages":"Article 102420"},"PeriodicalIF":1.9,"publicationDate":"2025-04-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143891931","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Optical spectroscopy and photoionization modeling of four selected planetary nebulae","authors":"Şengül Yalgın ,&nbsp;Nazım Aksaker ,&nbsp;Nurullah Erzincan ,&nbsp;Aysun Akyuz","doi":"10.1016/j.newast.2025.102413","DOIUrl":"10.1016/j.newast.2025.102413","url":null,"abstract":"<div><div>We present the results of chemical abundance measurements for four compact planetary nebulae (PNe) located in the Northern Hemisphere, selected from the HASH (Hong Kong/Australian Astronomical Observatory/Strasbourg H-alpha Planetary Nebula) database. Spectral data were collected using the medium-resolution TUG Faint Object Spectrograph and Camera mounted on the 1.5 m RTT telescope at the TÜBİTAK National Observatory. For each object, we determined key physical parameters, including the extinction coefficient, electron density, electron temperature, and ionization correction factors. Additionally, we constructed the spectral energy distribution across multiple wavelengths for each PN using advanced photoionization modeling with the <span>cloudy</span> code. The elemental abundance analysis, focusing on He, N, O, Ne, S, Cl, and Ar, indicates that the chemical composition of these PNe is consistent with both solar and Galactic values. The central stars exhibit effective temperatures ranging from approximately 53,000 to 180,000 K and luminosities between 2,500 and 9,000 L<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>. Based on their positions on the H-R diagram and post-AGB evolutionary tracks, their initial masses are estimated to range from 1 to 3 M<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>, with nebular masses between 0.69 and 2.34 M<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>. The ages of the nebulae, calculated to be between <span><math><mo>∼</mo></math></span>300 and 5,000 years, align with previous findings, emphasizing their evolutionary importance.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"119 ","pages":"Article 102413"},"PeriodicalIF":1.9,"publicationDate":"2025-04-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143887318","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Resonant absorption of kink MHD waves in twisted flux tubes with thick transitional layer","authors":"Karam Bahari","doi":"10.1016/j.newast.2025.102419","DOIUrl":"10.1016/j.newast.2025.102419","url":null,"abstract":"<div><div>The effect of magnetic twist on the resonant absorption of propagating magnetohydrodynamic (MHD) waves in coronal flux tubes with thick transitional layer has been investigated. The flux tube is assumed to be a density enhancement in a zero beta plasma with twisted magnetic field. In the thin tube approximation a perturbation method is used to solve equations of motion analytically in all the regions of the tube including the transitional layer. The dispersion relation is solved numerically to investigate both the temporal and spatial damping of the kink MHD waves. We have introduced a symmetry of the MHD waves in the presence of magnetic twist which has not been discussed earlier, this symmetry allows us to study only forward waves. The efficiency of resonant absorption depends on the sign of the twist parameter. For negative values of the twist parameter resonant absorption becomes sufficiently effective, and for positive values of the twist parameter, especially for a thick transitional layer, resonant absorption becomes almost ineffective. For a specific twist parameter, resonant absorption is efficient for the waves in which the sign of their wave number is opposite to that of the twist parameter.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"119 ","pages":"Article 102419"},"PeriodicalIF":1.9,"publicationDate":"2025-04-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143891933","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The first photometric and dynamical study of the eclipsing binary star V951 Perseus","authors":"Bin Zhang ,&nbsp;Wei Tao ,&nbsp;Zhen Zhong","doi":"10.1016/j.newast.2025.102418","DOIUrl":"10.1016/j.newast.2025.102418","url":null,"abstract":"<div><div>In this paper, we studied the short-period eclipsing binary V951 Perseus (hereafter V951 Per) using the newly observed four-color (<span><math><mi>B</mi></math></span>, <span><math><mi>V</mi></math></span>, <span><math><msub><mrow><mi>R</mi></mrow><mrow><mi>c</mi></mrow></msub></math></span>, <span><math><msub><mrow><mi>I</mi></mrow><mrow><mi>c</mi></mrow></msub></math></span>) light curves and the TESS data. Photometric solutions suggest that it is a W-subtype shallow contact binary with a mass ratio of <span><math><mi>q</mi></math></span> = 1.95 and a contact degree of <span><math><mi>f</mi></math></span> = 7.0%. In order to fit the asymmetrical light curves well, a cool star-spot on the less massive component is employed. Based on our new CCD eclipsing times and the data published until now, changes in the eclipsing times were analyzed using the <span><math><mrow><mi>O</mi><mo>−</mo><mi>C</mi></mrow></math></span> method. The <span><math><mrow><mi>O</mi><mo>−</mo><mi>C</mi></mrow></math></span> diagram indicates that the orbital period of V951 Per is decreasing at a rate of <span><math><mrow><mi>d</mi><mi>P</mi><mo>/</mo><mi>d</mi><mi>t</mi></mrow></math></span> = −8.79 × 10⁻⁸ d yr⁻¹, superposed on a cyclic oscillation with an amplitude of 0.0046 d and a period of 11.4 yr. The secular period decrease can be explained by the mass transfer from the more massive component to the less massive one or by the angular momentum loss. The cyclic oscillation may be interpreted as the light-travel-time effect because of the presence of an unseen third body. We calculated the mass of the third companion as <span><math><mrow><msub><mrow><mi>M</mi></mrow><mrow><mn>3</mn></mrow></msub><mi>s</mi><mi>i</mi><mi>n</mi><mrow><mo>(</mo><mi>i</mi><mo>)</mo></mrow></mrow></math></span> = 0.18 <span><math><msub><mrow><mi>M</mi></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"119 ","pages":"Article 102418"},"PeriodicalIF":1.9,"publicationDate":"2025-04-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143876580","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Multi-point Hermite methods for the N-body problem","authors":"Alexander J. Dittmann","doi":"10.1016/j.newast.2025.102415","DOIUrl":"10.1016/j.newast.2025.102415","url":null,"abstract":"<div><div>Numerical integration methods are central to the study of self-gravitating systems, especially those comprised of many bodies or otherwise beyond the reach of analytical methods. Predictor–corrector schemes, both multi-step methods and those based on 2-point Hermite interpolation, have found great success in the simulation of star clusters and other collisional systems. Higher-order methods, such as those based on Gaussian quadratures and Richardson extrapolation, have also proven popular for high-accuracy integrations of few-body systems, particularly those that may undergo close encounters. This work presents a family of high-order schemes based on multi-point Hermite interpolation. When applied as multi-step multi-derivative schemes, these can be seen as generalizing both Adams–Bashforth–Moulton methods and 2-point Hermite methods; I present results for the 6th-, 9th-, and 12th-order 3-point schemes applied in this manner using variable timesteps. In a star cluster-like test problem, the 3-point 6th-order predictor–corrector scheme matches or outperforms the standard 2-point 4th-order Hermite scheme at negligible <span><math><mrow><mi>O</mi><mrow><mo>(</mo><mi>N</mi><mo>)</mo></mrow></mrow></math></span> additional cost, potentially reducing the necessary number of force evaluations in simulations of large-<span><math><mi>N</mi></math></span> collisional systems by factors of <span><math><mrow><mo>∼</mo><mn>3</mn></mrow></math></span> or more. I also present a number of high-order time-symmetric schemes up to 18th order, which have the potential to improve the accuracy and efficiency of long-duration simulations.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"119 ","pages":"Article 102415"},"PeriodicalIF":1.9,"publicationDate":"2025-04-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143891932","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"A catalog of low frequency quasi-periodic oscillations from cygnus X-2","authors":"Kavitha Arur ,&nbsp;Divyesh Ved","doi":"10.1016/j.newast.2025.102417","DOIUrl":"10.1016/j.newast.2025.102417","url":null,"abstract":"<div><div>We present the results of timing analysis of archival Rossi X-ray Timing Explorer observations of the neutron star (NS) X-ray binary Cygnus X-2. This work focuses on the search for low-frequency (<span><math><mo>≤</mo></math></span>100 Hz) quasi-periodic oscillations (QPOs) from Cygnus X-2 performed using a semi-automatic analysis pipeline. The aim of the presented catalog is to expand the availability of timing information pertaining to neutron star low mass X-ray binaries (LMXBs) to facilitate detailed comparison with black hole LMXBs. The search identified QPOs in 88 out of 582 observations. We classify the detected QPOs into horizontal, normal, and flaring branch oscillations (HBOs, NBOs, and FBOs) respectively, analogous to the classification of black hole (BH) QPOs into type-C, type-B, and type-A. We identify 79 observations with HBOs, 8 with NBOs and no FBOs in the dataset. We further identify an observation that shows the presence of a NBO and HBO simultaneously.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"119 ","pages":"Article 102417"},"PeriodicalIF":1.9,"publicationDate":"2025-04-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143887317","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Physical parameters of stars in NGC 6397 using ANN-based interpolation and full spectrum fitting","authors":"Nitesh Kumar ,&nbsp;Philippe Prugniel ,&nbsp;Harinder P. Singh","doi":"10.1016/j.newast.2025.102416","DOIUrl":"10.1016/j.newast.2025.102416","url":null,"abstract":"<div><div>Stellar spectral interpolation is critical technique employed by fitting software to derive the physical parameters of stars. This approach is necessary because on-the-go generation of synthetic stellar spectra is not possible due to the complex and high cost of computation. The goal of this study is to develop a spectral interpolator for a synthetic spectral library using artificial neural networks (ANNs). The study aims to test the accuracy of the trained interpolator through self-inversion and, subsequently, to utilize the interpolator to derive the physical parameters of stars in the globular cluster NGC 6397 using spectra obtained from the Multi Unit Spectroscopic Explorer (MUSE) on the Very Large Telescope (VLT). In this study, ANNs were trained to function as spectral interpolators. The ULySS full-spectrum fitting package, integrated with the trained interpolators, was then used to extract the physical parameters of 1587 spectra of 1063 stars in NGC 6397. The trained ANN interpolator achieved precise determination of stellar parameters with a mean difference of 31 K for <span><math><msub><mrow><mi>T</mi></mrow><mrow><mi>eff</mi></mrow></msub></math></span> and 0.01 dex for <span><math><mi>[Fe/H]</mi></math></span> compared to previous studies. This study demonstrates the efficacy of ANN-based spectral interpolation in stellar parameter determination, offering faster and more accurate analysis.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"119 ","pages":"Article 102416"},"PeriodicalIF":1.9,"publicationDate":"2025-04-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143882953","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The dynamical orbital stability of the proposed 2+1+1 hierarchical eclipsing binary systems","authors":"Huseyin Er","doi":"10.1016/j.newast.2025.102414","DOIUrl":"10.1016/j.newast.2025.102414","url":null,"abstract":"<div><div>We performed a comprehensive dynamical stability analysis of the eclipsing binary systems proposed to have a <span><math><mrow><mn>2</mn><mo>+</mo><mn>1</mn><mo>+</mo><mn>1</mn></mrow></math></span> hierarchical structure. Using the REBOUND N-body integration package, which includes the WHFast, IAS15, MERCURIUS, and TRACE integrators, and the MEGNO (Mean Exponential Growth Factor of Close Orbits) chaos indicator, we analysed the orbital configurations of these systems and their stability on long time scales. For TZ Boo, dynamical simulations based on two proposed orbital models show that configurations with two additional companions (models I and III) exhibit significant dynamical instability, with chaotic orbital behaviour occurring on short time scales (<span><math><mrow><mo>∼</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>3</mn></mrow></msup></mrow></math></span> years). This instability is confirmed by MEGNO chaos parameters greater than 2 and the rapid divergence of the semi-major axes and eccentricities of the proposed companions. Similarly, the BB Peg and V539 Arae systems, despite being proposed to host two additional companions, also show pronounced chaotic behaviour on short timescales, as evidenced by high MEGNO values and instability times of about 708 and 458 years, respectively. In contrast, NSVS 7453183 exhibits significant dynamical stability over <span><math><mrow><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>8</mn></mrow></msup></mrow></math></span> year simulations, supported by bounded oscillations in the orbital parameters and MEGNO values consistently below 2. The stability of the system was further validated by an analysis of the orbital parameter uncertainties, indicating the critical role of the high eccentricity dynamics in the outer companion. These results indicate the need to integrate dynamical analyses with observational constraints to assess the plausibility of additional companions in binary systems. While NSVS 7453183 provides a plausible quadruple system configuration, the results for TZ Boo, BB Peg, and V539 Arae suggest against over-reliance on <span><math><mrow><mi>O</mi><mo>−</mo><mi>C</mi></mrow></math></span> diagram modelling without detailed stability evaluations.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"119 ","pages":"Article 102414"},"PeriodicalIF":1.9,"publicationDate":"2025-04-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143859412","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"V455 Car: An oscillating eclipsing Algol-type binary in triple star system","authors":"Zhao-Long Deng ,&nbsp;Wen-Ping Liao ,&nbsp;Li-Ying Zhu ,&nbsp;Xiang-Dong Shi ,&nbsp;Nian-Ping Liu ,&nbsp;Ping Li","doi":"10.1016/j.newast.2025.102412","DOIUrl":"10.1016/j.newast.2025.102412","url":null,"abstract":"<div><div>V455 Car is a southern oscillating eclipsing Algol-type system with an orbital period of 5.132888 days. Our first photometric solutions based on the Transiting Exoplanet Survey Satellite indicate that it is a semi-detached binary with the secondary star is almost filling its Roche lobe. The noticeable O’Connell effect in light curve could be explained by hot spot on the primary component, which may be attributed to the mass transfer from the secondary component to the primary one. The absolute parameters are determined as: <span><math><mrow><msub><mrow><mi>M</mi></mrow><mrow><mn>1</mn></mrow></msub><mo>=</mo><mn>5</mn><mo>.</mo><mn>30</mn><mo>±</mo><mn>1</mn><mo>.</mo><mn>10</mn><mspace></mspace></mrow></math></span> M<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>, <span><math><mrow><msub><mrow><mi>R</mi></mrow><mrow><mn>1</mn></mrow></msub><mo>=</mo><mn>3</mn><mo>.</mo><mn>17</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>22</mn><mspace></mspace></mrow></math></span> R<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span> for the primary, and <span><math><mrow><msub><mrow><mi>M</mi></mrow><mrow><mn>2</mn></mrow></msub><mo>=</mo><mn>1</mn><mo>.</mo><mn>58</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>32</mn><mspace></mspace></mrow></math></span> M<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>, <span><math><mrow><msub><mrow><mi>R</mi></mrow><mrow><mn>2</mn></mrow></msub><mo>=</mo><mn>6</mn><mo>.</mo><mn>66</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>46</mn><mspace></mspace></mrow></math></span> R<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span> for the secondary. <strong>Based on <em>O − C</em> analysis, we find a periodic variation of</strong> <span><math><mrow><msub><mrow><mi>P</mi></mrow><mrow><mn>3</mn></mrow></msub><mo>=</mo><mn>26</mn><mo>.</mo><mn>62</mn></mrow></math></span> (<span><math><mrow><mo>±</mo><mn>1</mn><mo>.</mo><mn>66</mn></mrow></math></span>), <span><math><mrow><mi>y</mi><mi>r</mi></mrow></math></span>. <strong>The periodic oscillation suggests a possible third body with a minimal mass of</strong> <span><math><mrow><mn>0</mn><mo>.</mo><mn>59</mn><mrow><mo>(</mo><mo>±</mo><mn>0</mn><mo>.</mo><mn>13</mn><mo>)</mo></mrow><mspace></mspace></mrow></math></span> <strong>M</strong><span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>. It is speculated that the secondary star has undergone a longer evolution, leading to a mass ratio reversal being experienced in the binary system. Our frequency analysis finds that the primary of V455 Car may be an SPB/SLF star. This study reports a novel example of an oscillating eclipsing Algol-type system featuring an SPB/SLF primary star and a red giant star, which suggest that strong observational results for a high incidence of third bodies in massive binaries.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"119 ","pages":"Article 102412"},"PeriodicalIF":1.9,"publicationDate":"2025-04-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143859409","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Few EURONEAR NEA mini-surveys observed with the INT, KASI and T80S telescopes during the ParaSOL synthetic tracking project","authors":"O. Vaduvescu ,&nbsp;M. Stanescu ,&nbsp;M. Popescu ,&nbsp;M. Predatu ,&nbsp;L. Curelaru ,&nbsp;D. Bertesteanu ,&nbsp;C. Boldea ,&nbsp;F. Ursache ,&nbsp;C. Fotin ,&nbsp;C. de la Fuente Marcos ,&nbsp;R. de la Fuente Marcos ,&nbsp;E. Unda-Sanzana ,&nbsp;F. Barwell ,&nbsp;K. Jhass ,&nbsp;S. Shenoy ,&nbsp;A. Santos-Garcia ,&nbsp;J. Bishop ,&nbsp;J. Munday ,&nbsp;J. de Leon ,&nbsp;C.-U. Lee ,&nbsp;C. Mendes de Oliveira","doi":"10.1016/j.newast.2025.102410","DOIUrl":"10.1016/j.newast.2025.102410","url":null,"abstract":"<div><div>The modern synthetic tracking technique (ST) can make use of small and medium-sized telescopes to detect asteroids fainter than the classic blinking methods, by arbitrary shifting and co-adding more images of the same survey field, if GPU computing resources are available. In the framework of the Romanian ParaSOL project, we developed and tested an innovative ST algorithm capable of detecting in near-real-time very faint near-Earth asteroids (NEAs), which likely became the first ST pipeline developed in Europe. To test our pipeline, we conducted several mini-surveys using three large-field telescopes, namely the ING’s INT, the Korean KASI and the Brazilian T80S telescopes. Most images were processed using our <em>Umbrella Image Processing Pipeline</em> (IPP) module. The ST search was conducted using our <em>Synthetic Tracking via Umbrella</em> (STU) module and the commercial <em>Tycho Tracker</em> software, which allowed to compare and complement the findings. The source validation was supported by reducers using our new <em>Webrella</em> platform. Most of the nights were reduced in near-real-time, demonstrating the ability to process, sort, and report large volumes of data. We discovered 5 credited and 4 one-night NEAs, co-discovered other 3 NEAs and recovered 3 poorly known NEAs. We flagged 59 NEA candidates for recovery and orbital classification, discovering, co-discovering and recovering other 18 orbitally related NEAs, additionally improving the orbits of 23,428 known asteroids and reporting 1,374 unknown objects. A comparison between ST and traditional blinking detection using the new EURONEAR tool <em>MagLim</em> shows improvements of two magnitudes and a two-fold increase in the number of detections. A preliminary comparison between STU and Tycho shows that STU detects about 70% of Tycho findings, however STU detects rapid objects much faster than Tycho, 7 NEAs with speeds between 2-10<span><math><msup><mrow></mrow><mrow><mo>′</mo><mo>′</mo></mrow></msup></math></span>/min being found exclusively by STU. Based on our surveys, we assessed the current NEA discovery rate using 1-2-m class telescopes and ST methods, finding that one NEA candidate can be discovered in every 9-12 square degrees up to magnitude <span><math><mrow><mo>∼</mo><mn>23</mn></mrow></math></span>.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"119 ","pages":"Article 102410"},"PeriodicalIF":1.9,"publicationDate":"2025-04-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143843971","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}