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{"title":"Studying orbital period variations of XY Leo through updated eclipse times and multi-model analysis","authors":"Ilham Nasiroglu","doi":"10.1016/j.newast.2025.102374","DOIUrl":"10.1016/j.newast.2025.102374","url":null,"abstract":"<div><div>This study revisits the orbital period variation of the short-period eclipsing binary system XY Leo, a W-subtype W Ursae Majoris (W UMa) contact binary, by analyzing 30 newly collected mid-eclipse times from three telescopes between 2015 and 2021. The obtained light curves and residuals showed no deviations attributable to effects like pulsations or starspots. The updated <span><math><mrow><mi>O</mi><mo>−</mo><mi>C</mi></mrow></math></span> diagram, covering 77 years and extended by four years of new data, revealed minor deviations from previously published models. Three models were applied using MCMC sampling to analyze the orbital period variations of XY Leo. Model I includes the linear ephemeris, a quadratic term, and the Light Travel Time (LTT) effect of a 3rd body orbiting the central binary system. Models II and III add a sinusoidal function for the magnetic cycle and the LTT effect of a 4th body to Model I, respectively. Updated orbital parameters for the 3rd body are slightly larger than earlier estimates, except for <span><math><msub><mrow><mi>e</mi></mrow><mrow><mn>3</mn></mrow></msub></math></span>. Applegate mechanism analysis of the magnetic cycle indicated possible magnetic activity, though the derived period (28.09 years) exceeds the expected range. For the first time, Model III considers a 4th body, yielding the lowest RMS and systematic error, suggesting better compatibility with the <span><math><mrow><mi>O</mi><mo>−</mo><mi>C</mi></mrow></math></span> diagram. Orbital stability tests confirmed stable orbits for Models I and II over one Myr, while Model III showed no stability. Persistent oscillations in Model I residuals suggest that the orbital period variation requires additional explanations, such as magnetic cycles or the influence of further companions.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"118 ","pages":"Article 102374"},"PeriodicalIF":1.9,"publicationDate":"2025-02-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143512601","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":"An elaborate search for coherent pulsations from Intermittent–AMXPs","authors":"Mustafa Turan Sağlam ,&nbsp;Can Güngör ,&nbsp;Tuğçe Kocabıyık","doi":"10.1016/j.newast.2025.102372","DOIUrl":"10.1016/j.newast.2025.102372","url":null,"abstract":"<div><div>We present a detailed systematic pulse search for three Intermittent-Accreting Millisecond X-ray Pulsars (Intermittent-AMXPs), HETE J1900.1-2455, SAX J1748.9-2021&amp; Aql X-1, via Z<span><math><msubsup><mrow></mrow><mrow><mn>1</mn></mrow><mrow><mn>2</mn></mrow></msubsup></math></span> and maximum likelihood (ML) techniques by using 16 years data of Rossi X-ray Timing Explorer/Proportional Counter Array (RXTE/PCA) in the energy range of 3.0–13.0 keV. We first performed a pulse scan using the Z<span><math><msubsup><mrow></mrow><mrow><mn>1</mn></mrow><mrow><mn>2</mn></mrow></msubsup></math></span> technique in millisecond sensitivities for every 25 s time interval with 1 s shifts to cover all data set around the detected frequencies given in the literature. We tracked the Z<span><math><msubsup><mrow></mrow><mrow><mn>1</mn></mrow><mrow><mn>2</mn></mrow></msubsup></math></span> power over time and flagged the time intervals exceeding defined threshold levels for each source as <em>pulse candidates</em>. The detected pulse list throughout our scan has new discoveries while covering the pulsed regions presented in the literature. For a deeper search, using the pulses obtained from the Z<span><math><msubsup><mrow></mrow><mrow><mn>1</mn></mrow><mrow><mn>2</mn></mrow></msubsup></math></span> method as a probability density function as an input parameter, we re-scanned the time intervals centered on the detected pulse via ML. The detected pulse-on duration via ML is slightly longer than the one via Z<span><math><msubsup><mrow></mrow><mrow><mn>1</mn></mrow><mrow><mn>2</mn></mrow></msubsup></math></span> method. This phenomenon allows us to argue for the existence of the smooth transition between pulse-on and pulse-off stages. For SAX J1748.9-2021, we also obtained orbital period by using the systematic pulse arrival phase patterns throughput of ML to be 8.76 h.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"118 ","pages":"Article 102372"},"PeriodicalIF":1.9,"publicationDate":"2025-02-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143453030","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":"Composite pseudo Nambu Goldstone quintessence","authors":"Mayukh R. Gangopadhyay ,&nbsp;Nilanjana Kumar ,&nbsp;Ankan Mukherjee ,&nbsp;Mohit K. Sharma","doi":"10.1016/j.newast.2025.102373","DOIUrl":"10.1016/j.newast.2025.102373","url":null,"abstract":"<div><div>A pseudo-Nambu Goldstone Boson (pNGB) arising from the breaking of a global symmetry (<span><math><mrow><mi>G</mi><mo>→</mo><mi>H</mi></mrow></math></span>) can be one of the most promising candidate for the quintessence model, to explain the late time acceleration of our universe. Motivated from the Composite Higgs scenario, we have investigated the case where the pNGB associated with <span><math><mrow><mi>S</mi><mi>O</mi><mrow><mo>(</mo><mi>N</mi><mo>)</mo></mrow><mo>/</mo><mi>S</mi><mi>O</mi><mrow><mo>(</mo><mi>N</mi><mo>−</mo><mn>1</mn><mo>)</mo></mrow></mrow></math></span> develops a potential through its couplings with the particles that do not form the complete representations of <span><math><mi>G</mi></math></span>. The Coleman Weinberg (CW) potential is generated via the external particles in the loop which are linked with the strongly interacting dynamics and can be computed predicatively.</div><div>The model of Dark Energy (DE) is tested against several latest cosmological observations such as supernovae data of Pantheon, Baryon Acoustic Oscillation (BAO), Redshift-space distortion (RSD) data etc. We have found that the fit prefers sub-Planckian value of the pNGB field decay constant. Moreover, we have found that the model predicts cosmological parameters well within the allowed range of the observation and thus gives a well motivated model of quintessence.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"118 ","pages":"Article 102373"},"PeriodicalIF":1.9,"publicationDate":"2025-02-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143436863","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":"Studying the nature of Ultraluminous X-ray sources in NGC 1453 with XMM-Newton","authors":"Praveen Kangjam ,&nbsp;Dayananda Mayanglambam ,&nbsp;A. Senorita Devi ,&nbsp;Akram Chandrajit Singha","doi":"10.1016/j.newast.2025.102371","DOIUrl":"10.1016/j.newast.2025.102371","url":null,"abstract":"&lt;div&gt;&lt;div&gt;This paper presents a multi epoch, detailed spectral and temporal analysis of the non-nuclear X-ray point sources of the massive elliptical galaxy NGC 1453, based on two XMM-Newton observational data. In the observation with Obs ID 0901620101, seven sources having net counts &lt;span&gt;&lt;math&gt;&lt;mo&gt;≥&lt;/mo&gt;&lt;/math&gt;&lt;/span&gt; 100 were identified for PN data, which along with their corresponding MOS data were considered for the analysis. For the observation with Obs ID 0673770601, only three sources were found for PN and two sources for MOS-1 and MOS-2. The spectra of all the sources were simultaneously fitted using two empirical models: an absorbed power-law model and an absorbed disk blackbody model. Based on the estimated bolometric luminosities of the sources, six sources - X-1, X-2, X-3, X-4, X-6 and X-7 are categorized as HLXs with X-ray luminosity, &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;L&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;X&lt;/mi&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;mo&gt;&gt;&lt;/mo&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;msup&gt;&lt;mrow&gt;&lt;mn&gt;0&lt;/mn&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;41&lt;/mn&gt;&lt;/mrow&gt;&lt;/msup&gt;&lt;mi&gt;e&lt;/mi&gt;&lt;mi&gt;r&lt;/mi&gt;&lt;mi&gt;g&lt;/mi&gt;&lt;mspace&gt;&lt;/mspace&gt;&lt;msup&gt;&lt;mrow&gt;&lt;mi&gt;s&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mo&gt;−&lt;/mo&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;/mrow&gt;&lt;/msup&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; while one source, X-5, as an ELX with &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;L&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;X&lt;/mi&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;mo&gt;&gt;&lt;/mo&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;msup&gt;&lt;mrow&gt;&lt;mn&gt;0&lt;/mn&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;40&lt;/mn&gt;&lt;/mrow&gt;&lt;/msup&gt;&lt;mi&gt;e&lt;/mi&gt;&lt;mi&gt;r&lt;/mi&gt;&lt;mi&gt;g&lt;/mi&gt;&lt;mspace&gt;&lt;/mspace&gt;&lt;msup&gt;&lt;mrow&gt;&lt;mi&gt;s&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mo&gt;−&lt;/mo&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;/mrow&gt;&lt;/msup&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt;, within the error limit. Notably, for source X-1, the disk blackbody component is the dominant feature in both the observations. In the 2012 observation (Obs ID 0673770601), the source exhibits a soft, cool accretion disk with an inner disk temperature of &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mi&gt;k&lt;/mi&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;T&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;i&lt;/mi&gt;&lt;mi&gt;n&lt;/mi&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;mo&gt;∼&lt;/mo&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; 0.27 keV. By 2022 (Obs ID 0901620101), X-1 presents an even softer, supersoft spectrum, characterized by a significantly lower inner disk temperature of &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mi&gt;k&lt;/mi&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;T&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;i&lt;/mi&gt;&lt;mi&gt;n&lt;/mi&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;mo&gt;∼&lt;/mo&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; 0.17 keV and photon index &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mi&gt;Γ&lt;/mi&gt;&lt;mo&gt;&gt;&lt;/mo&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; 5. This shift over the span of a decade indicates a further softening of the source. In the present study, due to limited data availability, the Luminosity-Temperature (L-T) relation could not be strictly constrained. However, for the purpose of mass estimation, we have assumed that the L&lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mo&gt;∼&lt;/mo&gt;&lt;msup&gt;&lt;mrow&gt;&lt;mi&gt;T&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;4&lt;/mn&gt;&lt;/mrow&gt;&lt;/msup&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; relation holds. The observed further softening of the source (X-1), accompanied by a slight increase in luminosity in the later observation, suggests a potential inverse correlation between the inner disk temperature of the soft component and luminosity, which is consistent with the characteristics of beamed disk emission resulting from radiatively","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"118 ","pages":"Article 102371"},"PeriodicalIF":1.9,"publicationDate":"2025-02-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143422000","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":"MeerKAT-based multi-wavelength study of supernova remnant G7.7-3.7 (SN386?)","authors":"Patrick N. Mwaniki ,&nbsp;James O. Chibueze ,&nbsp;Dismas S. Wamalwa","doi":"10.1016/j.newast.2025.102370","DOIUrl":"10.1016/j.newast.2025.102370","url":null,"abstract":"<div><div>We investigated the structural characteristics of G7.7-3.7 at a higher resolution of 1284 MHz. MeerKAT observations revealed that G7.7-3.7 had an asymmetric spherical structure with filamentary features and various blowouts. The western boundary showed a strong bright blowout, while the southern perimeter showcased extended bright filaments with feather-like structures, which seemed disconnected from the western blowout. Moreover, the eastern region exhibited a blowout centered around a bright point source, with faint, elongated filaments extending north-west. These filaments connected the eastern point source to the western blowout, creating a uniform outward progression. Spectral index analysis indicated a steep spectrum (<span><math><mi>α</mi></math></span> ranged <span><math><mo>∼</mo></math></span> 0 to <span><math><mo>∼</mo></math></span> −3), suggesting a combination of synchrotron and a few traces of thermal emissions concentrated at the edges of bright blowouts. Analysis of MeerKAT and VLA data revealed that G7.7-3.7 had expanded by 9 ± 0.45 arcsec over a period of 31.907 years, corresponding to an expansion rate of 0.282 ± 0.014 arcsec yr⁻¹. This expansion indicated a shock speed of 5883 ± 294 km s⁻¹ and an age of 1636 ± 115 years. This age fits with the supernova explosion event of 386 CE and the MeerKAT observed data in 2023. The multi-wavelength investigation unveiled a distinctive structure within the southern radio blowout, encompassing a bright radio blowout, a prominent X-ray arc, and two faint optical filaments aligned with the X-ray bright arc. We attributed the bright radio blowouts to inhomogeneous mass outflow from shock-accelerated particles and the weakening of magnetic fields along its perimeter. Traces of thermal emissions, especially along the edges of blowouts, were likely due to shock-heated gas, which intensified in the southern region amid high-density Interstellar Medium (ISM). Therefore, these results supported a scenario in which the progenitor supernova of G7.7-3.7 exploded within ISM of varying density, generating the observed X-ray emissions and faint optical filaments. Our findings provided valuable insights into the dynamics and evolution of supernova remnants.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"117 ","pages":"Article 102370"},"PeriodicalIF":1.9,"publicationDate":"2025-02-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143387699","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":"Prospects for high-resolution probes of galaxy dynamics tracing background cosmology in MaNGA","authors":"Gyeong-Min Lee ,&nbsp;Maurice H.P.M. van Putten","doi":"10.1016/j.newast.2025.102360","DOIUrl":"10.1016/j.newast.2025.102360","url":null,"abstract":"<div><div>Large-<span><math><mi>N</mi></math></span> galaxy surveys offer unprecedented opportunities to probe weak gravitation in galaxy dynamics that may contain correlations tracing background cosmology. Of particular interest is the potential of finite sensitivities to the background de Sitter scale of acceleration <span><math><mrow><msub><mrow><mi>a</mi></mrow><mrow><mi>d</mi><mi>S</mi></mrow></msub><mo>=</mo><mi>c</mi><mi>H</mi></mrow></math></span>, where <span><math><mi>H</mi></math></span> is the Hubble parameter and <span><math><mi>c</mi></math></span> is the velocity of light. At sufficiently large <span><math><mi>N</mi></math></span>, this is possibly probed by ensemble-averaged (“stacked”) rotation curves (RCs) at resolutions on par with present estimates of the Hubble parameter <span><math><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub></math></span>. Here, we consider the prospect for these studies using the large <span><math><mi>N</mi></math></span> <em>Mapping Nearby Galaxies at Apache Point Observatory</em> MaNGA at APO survey. In a first and preliminary step, we consider unbiased control of sub-sample size by consistency in the three Position Angles, <span><math><mi>θ</mi></math></span> , from photometry and velocity fields of gas and stars by spectroscopy within 30°. In sub-samples of size <span><math><mrow><mi>N</mi><mo>=</mo><msub><mrow><mi>N</mi></mrow><mrow><mi>i</mi></mrow></msub><mrow><mo>(</mo><mi>θ</mi><mo>)</mo></mrow></mrow></math></span>, the scatter in-the-mean <span><math><mrow><mi>σ</mi><mo>/</mo><msqrt><mrow><mi>N</mi></mrow></msqrt></mrow></math></span> is found to reach one percent levels, differentiated over inclination angle <span><math><mi>i</mi></math></span> and <span><math><mi>θ</mi></math></span>. In regular propagation of uncertainties, this scatter contributes <span><math><mrow><mi>κ</mi><mi>σ</mi><mo>/</mo><msqrt><mrow><mi>N</mi></mrow></msqrt></mrow></math></span> to the standard error in-the-mean to the observable, where <span><math><mi>κ</mi></math></span> is determined by the choice of observables. As a lower bound to scatter in stacked RCs, MaNGA hereby appears promising for high-resolution analysis of sensitivity to RCs to background cosmology, notably across a sharp <span><math><msup><mrow><mi>C</mi></mrow><mrow><mn>0</mn></mrow></msup></math></span>-transition (van Putten, 2018) of Newtonian to anomalous dynamics across <span><math><msub><mrow><mi>a</mi></mrow><mrow><mi>d</mi><mi>S</mi></mrow></msub></math></span> and, further out, the baryonic Tully–Fisher relation. In turn, these markers provide a novel measurement of cosmological parameters including <span><math><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub></math></span>.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"117 ","pages":"Article 102360"},"PeriodicalIF":1.9,"publicationDate":"2025-01-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143153393","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Accretion disk around the regular black holes with a nonlinear electrodynamics source","authors":"Minou Khoshrangbaf ,&nbsp;Amin Rezaei Akbarieh ,&nbsp;K. Atazadeh ,&nbsp;Hossein Motavalli","doi":"10.1016/j.newast.2025.102354","DOIUrl":"10.1016/j.newast.2025.102354","url":null,"abstract":"<div><div>Accretion disks is crucial in studying black holes, serving as the singular source of electromagnetic radiation. The existence of singularity inherent in black holes necessitates an examination of regular cores. In this work, we study standard thin accretion disks around regular black holes (RBHs) with a nonlinear electrodynamics source. By comparing the radiant energy, luminosity derivative, and temperature of six types of RBHs with a nonlinear electrodynamics source, both among themselves and with Schwarzschild black holes, we aim to identify observable features. Our results show that the non-zero charge parameter of RBHs with a nonlinear electrodynamics source causes the radius of the innermost stable circular orbit of the accretion disk to be displaced inwards towards smaller values of <span><math><mi>r</mi></math></span>. We also obtain that the mass-to-radiant conversion efficiency for RBHs with a nonlinear electrodynamics source is higher than that of Schwarzschild black holes. Finally, we compare the free parameter of RBHs with a nonlinear electrodynamics source to the spin parameter of the Kerr black hole to extract potential observables. Our results indicate that the maximum spin that RBHs with a nonlinear electrodynamics source can mimic is approximately 0.9.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"117 ","pages":"Article 102354"},"PeriodicalIF":1.9,"publicationDate":"2025-01-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143153392","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":"Orbital period study of two contact W UMa-type contact binaries: V551 Dra and CN Hyi","authors":"Xuan-Qi Tang ,&nbsp;Chao-Yue Li ,&nbsp;Lin-Qiao Jiang ,&nbsp;Jie Wei ,&nbsp;Jie Zheng ,&nbsp;Kai Huang ,&nbsp;Jia-Xing Wang ,&nbsp;Hao-Yi Yang ,&nbsp;Jing-Zhou Li ,&nbsp;Xiao-Man Tian ,&nbsp;Jian-Hui Yang","doi":"10.1016/j.newast.2025.102357","DOIUrl":"10.1016/j.newast.2025.102357","url":null,"abstract":"&lt;div&gt;&lt;div&gt;V551 Dra and CN Hyi are both W UMa-type contact binaries. Basing on TESS data, we conduct analyses of their orbital period variations. The results indicate that the O - C curve of V551 Dra shows a long-term upward trend, with &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mi&gt;d&lt;/mi&gt;&lt;mi&gt;P&lt;/mi&gt;&lt;mo&gt;/&lt;/mo&gt;&lt;mi&gt;d&lt;/mi&gt;&lt;mi&gt;t&lt;/mi&gt;&lt;mo&gt;=&lt;/mo&gt;&lt;mn&gt;2&lt;/mn&gt;&lt;mo&gt;.&lt;/mo&gt;&lt;mn&gt;80&lt;/mn&gt;&lt;mo&gt;×&lt;/mo&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;msup&gt;&lt;mrow&gt;&lt;mn&gt;0&lt;/mn&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mo&gt;−&lt;/mo&gt;&lt;mn&gt;7&lt;/mn&gt;&lt;/mrow&gt;&lt;/msup&gt;&lt;mi&gt;d&lt;/mi&gt;&lt;mi&gt;a&lt;/mi&gt;&lt;mi&gt;y&lt;/mi&gt;&lt;mi&gt;⋅&lt;/mi&gt;&lt;mi&gt;y&lt;/mi&gt;&lt;mi&gt;e&lt;/mi&gt;&lt;mi&gt;a&lt;/mi&gt;&lt;msup&gt;&lt;mrow&gt;&lt;mi&gt;r&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mo&gt;−&lt;/mo&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;/mrow&gt;&lt;/msup&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt;, which could be attributed to mass transfer from the less massive component to the more massive one. Additionally, a periodic variation with an amplitude of &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mi&gt;A&lt;/mi&gt;&lt;mo&gt;=&lt;/mo&gt;&lt;mn&gt;0&lt;/mn&gt;&lt;mo&gt;.&lt;/mo&gt;&lt;mn&gt;000954&lt;/mn&gt;&lt;mi&gt;d&lt;/mi&gt;&lt;mi&gt;a&lt;/mi&gt;&lt;mi&gt;y&lt;/mi&gt;&lt;mi&gt;s&lt;/mi&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; and a period of &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mi&gt;P&lt;/mi&gt;&lt;mo&gt;=&lt;/mo&gt;&lt;mn&gt;0&lt;/mn&gt;&lt;mo&gt;.&lt;/mo&gt;&lt;mn&gt;31&lt;/mn&gt;&lt;mi&gt;y&lt;/mi&gt;&lt;mi&gt;e&lt;/mi&gt;&lt;mi&gt;a&lt;/mi&gt;&lt;mi&gt;r&lt;/mi&gt;&lt;mi&gt;s&lt;/mi&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; was superimposed. The periodic variation in the orbital period may be due to the light-travel time effect caused by a third body. We estimate the minimum mass of the third body to be &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;M&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;3&lt;/mn&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;mo&gt;=&lt;/mo&gt;&lt;mn&gt;0&lt;/mn&gt;&lt;mo&gt;.&lt;/mo&gt;&lt;mn&gt;48&lt;/mn&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;M&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mo&gt;⊙&lt;/mo&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt;. The primary of V551 Dra, although less massive, is oversized and overluminous compared to standard mainsequence stars, suggesting it has evolved through substantial mass loss, while the more massive secondary remains on the main sequence, indicating a stable mass transfer phase. In contrast, The O - C curve of CN Hyi exhibits a long-term decreasing trend, with &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mi&gt;d&lt;/mi&gt;&lt;mi&gt;P&lt;/mi&gt;&lt;mo&gt;/&lt;/mo&gt;&lt;mi&gt;d&lt;/mi&gt;&lt;mi&gt;t&lt;/mi&gt;&lt;mo&gt;=&lt;/mo&gt;&lt;mo&gt;−&lt;/mo&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;mo&gt;.&lt;/mo&gt;&lt;mn&gt;09&lt;/mn&gt;&lt;mo&gt;×&lt;/mo&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;msup&gt;&lt;mrow&gt;&lt;mn&gt;0&lt;/mn&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mo&gt;−&lt;/mo&gt;&lt;mn&gt;6&lt;/mn&gt;&lt;/mrow&gt;&lt;/msup&gt;&lt;mi&gt;d&lt;/mi&gt;&lt;mi&gt;a&lt;/mi&gt;&lt;mi&gt;y&lt;/mi&gt;&lt;mi&gt;⋅&lt;/mi&gt;&lt;mi&gt;y&lt;/mi&gt;&lt;mi&gt;e&lt;/mi&gt;&lt;mi&gt;a&lt;/mi&gt;&lt;msup&gt;&lt;mrow&gt;&lt;mi&gt;r&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mo&gt;−&lt;/mo&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;/mrow&gt;&lt;/msup&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt;. Due to the intermediate contact nature of the binary system, this long-term period decrease is likely to be caused by mass transfer from the more massive primary star to the less massive secondary star. The primary of CN Hyi resides on the main sequence, while the oversized and overluminous secondary suggests significant material accretion. These findings suggest differing evolutionary pathways for W-subtype and A-subtype contact binaries. V551 Dra appears to exhibit stable mass transfer dynamics, whereas CN Hyi may potentially experience more dynamic structural changes as it evolves. In addition to these evolutionary considerations, we hypothesize that the period variation of CN Hyi may also be attributed by the light-travel time effect of a third body, given the common occurrence of third bodies in contact systems. Considering","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"117 ","pages":"Article 102357"},"PeriodicalIF":1.9,"publicationDate":"2025-01-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143153394","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":"Exploring the halo occupation distribution for moderate X-ray luminosity active galactic nuclei in the EAGLE cosmological simulation","authors":"Liliana Altamirano-Dévora ,&nbsp;Héctor Aceves ,&nbsp;Angel Castro ,&nbsp;Takamitsu Miyaji","doi":"10.1016/j.newast.2025.102361","DOIUrl":"10.1016/j.newast.2025.102361","url":null,"abstract":"<div><div>The hydrodynamical cosmological simulation <em>EAGLE</em> is used to model the Halo Occupation Distribution (HOD) of moderate X-ray luminosity active galactic nuclei (mXAGN), extending previous work using only dark matter simulations and empirical relations. By examining mergers as a triggering mechanism, we focus on halos typical of galaxy groups and cluster-like systems with masses <span><math><mrow><mo>≥</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>12</mn><mo>.</mo><mn>75</mn></mrow></msup><mspace></mspace><mi>M</mi><mo>⊙</mo><mspace></mspace><msup><mrow><mi>h</mi></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></mrow></math></span>. We analyze simulation data to create catalogs of central and satellite galaxies. We study their merger history we quantify the percentage of minor and major mergers in the mXAGN sample. We obtain the HOD for central and satellite mXAGN across a redshift interval from <span><math><mrow><mi>z</mi><mo>=</mo><mn>2</mn></mrow></math></span> to the present epoch. Our results indicate that, across most redshifts, minor mergers slightly predominate as the primary mechanism for triggering mXAGN.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"117 ","pages":"Article 102361"},"PeriodicalIF":1.9,"publicationDate":"2025-01-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143153395","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":"Corrigendum to “Gravitational interaction signatures in isolated galaxy triplet systems: a photometric analysis” [New Astronomy, 2021,87, 101603]","authors":"Amira A. Tawfeek ,&nbsp;Kanak Saha ,&nbsp;Kaustubh Vaghmare ,&nbsp;A.K. Kembhavi ,&nbsp;Ali Takey ,&nbsp;Bernardo Cervantes-Sodi ,&nbsp;Jacopo Fritz ,&nbsp;Zainab Awad ,&nbsp;Gamal B. Ali ,&nbsp;Z.M. Hayman","doi":"10.1016/j.newast.2025.102359","DOIUrl":"10.1016/j.newast.2025.102359","url":null,"abstract":"","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"117 ","pages":"Article 102359"},"PeriodicalIF":1.9,"publicationDate":"2025-01-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143474367","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}