New Astronomy最新文献

{"title":"ASIVA – Platform for observational and computational analysis of stellar variables","authors":"Parvej Reja Saleh ,&nbsp;Tanveer Singh ,&nbsp;Debasish Hazarika ,&nbsp;Surabhi Rajkumari ,&nbsp;Saurabh Rajkumar ,&nbsp;Pritam Das ,&nbsp;Padmakar Singh Parihar ,&nbsp;Eeshankur Saikia","doi":"10.1016/j.newast.2024.102232","DOIUrl":"https://doi.org/10.1016/j.newast.2024.102232","url":null,"abstract":"<div><p>The astronomical data analysis consists of two crucial process; data reduction of the captured images and data analysis of the derived magnitudes. We present the platform ASIVA, a data analysis platform which comes along with a data reduction pipeline. The data reduction pipeline gives flexibility to analyse the FITS images and also perform image alignment for detecting the correct image coordinates for required objects. It can be custom scheduled with cron jobs so that it picks the latest data and appends the results accordingly. The data analysis platform allows user to effectively analyse the ensemble data and perform accurate data processing and grouping with ease. It is integrated with a custom algorithm to detect the variable stars from an ensemble with its relative standard deviations. The statistical, spectral and non-linear dynamics features can be extracted from time series data which can be eventually used for in-depth analysis. To validate the capability, we have analysed 15 nights of Orion Nebula Cluster field in I filter which had 1585 images. ASIVA reduces manual effort to a great extent thus saves analysis time and excludes human errors.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"111 ","pages":"Article 102232"},"PeriodicalIF":2.0,"publicationDate":"2024-04-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140618276","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":"Charged anisotropic fluid sphere in f(Q) gravity satisfying Vaidya - Tikekar metric","authors":"Simranjeet Kaur ,&nbsp;S.K. Maurya ,&nbsp;Sacheendra Shukla ,&nbsp;B. Dayanandan","doi":"10.1016/j.newast.2024.102230","DOIUrl":"https://doi.org/10.1016/j.newast.2024.102230","url":null,"abstract":"<div><p>In this paper, we study the properties of electrically charged anisotropic and spherically symmetric compact stars in <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></mrow></math></span> gravity theory. The field equations have been solved using the MIT-Bag Equation of State (EoS) along with the Vaidya–Tikekar potential. However, the specific form of charge <span><math><mrow><msup><mrow><mi>E</mi></mrow><mrow><mn>2</mn></mrow></msup><mrow><mo>(</mo><mi>r</mi><mo>)</mo></mrow><mo>=</mo><mfrac><mrow><msub><mrow><mi>q</mi></mrow><mrow><mn>0</mn></mrow></msub><msup><mrow><mi>L</mi></mrow><mrow><mn>2</mn></mrow></msup><msup><mrow><mi>r</mi></mrow><mrow><mn>2</mn></mrow></msup></mrow><mrow><msup><mrow><mrow><mo>(</mo><mn>1</mn><mo>+</mo><mi>L</mi><msup><mrow><mi>r</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>)</mo></mrow></mrow><mrow><mn>2</mn></mrow></msup></mrow></mfrac></mrow></math></span> has been used to study the charged compact star model. The interior charge anisotropic solution has been matched with the charged Schwarzchild-(Anti)-de-Sitter metric. In particular, this study has been conducted on different compact stars viz, EXO 1785-248, PSR J1614-2230, PSR J0740+620 and SMC X-1. The mass–radius ratio of these compact stars has been predicted, and the physical viability of the model has been checked through the behaviour of causality condition, matter variables, energy constraints, modified TOV equation, and adiabatic index of the star. In conclusion, we observe a well-behaved model of a compact star in <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></mrow></math></span> gravity with charged matter distribution.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"110 ","pages":"Article 102230"},"PeriodicalIF":2.0,"publicationDate":"2024-04-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140547243","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 CCD photometric studies of the member eclipsing binary ZTFJ015003.88+534,734.1 in the newly discovered young open cluster UBC 188","authors":"Y.H.M. Hendy,&nbsp;I. Zead,&nbsp;A.E. Abdelaziz,&nbsp;A. Takey","doi":"10.1016/j.newast.2024.102231","DOIUrl":"https://doi.org/10.1016/j.newast.2024.102231","url":null,"abstract":"<div><p>We present the first CCD observations of an eclipsing binary, ZTFJ015003.88+534,734.1, which is a member in the open star cluster UBC 188. The observations were taken by the 1.88 m telescope at the Kottamia Astronomical Observatory (KAO) in SDSS <em>griz</em> bands. The latest version of the Wilson-Devinney (W-D) code was employed for photometric analysis and light curve modeling of the eclipsing binary. The results indicate that the binary system is in an over-contact configuration. The mass of the primary star (M1) is determined to be 1.293 M_⊙, and the mass of the secondary star (M2) is directly derived from the system's estimated mass ratio (<em>q</em> = M2/M1) as 0.340 times the solar mass (M_⊙). We investigated the color-magnitude diagram and the membership probability of the open cluster UBC 188 using the Gaia DR3 data. We determined the membership probability of the eclipsing binary ZTFJ015003.88+534,734.1 using the pyUPMASK algorithm and found that its membership probability is one.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"110 ","pages":"Article 102231"},"PeriodicalIF":2.0,"publicationDate":"2024-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140347164","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 Investigation of six contact binary systems and a semi-detached one","authors":"Massimiliano Martignoni ,&nbsp;Velimir Popov ,&nbsp;Carlo Barani ,&nbsp;Francesco Acerbi","doi":"10.1016/j.newast.2024.102228","DOIUrl":"https://doi.org/10.1016/j.newast.2024.102228","url":null,"abstract":"<div><p>We present a photometric analysis of six W Ursae Majoris contact binaries and one semi-detached system using multifilter CCD observations. The data were obtained with the 0.25 m Schmidt Cassegrain telescope at the observatory Stazione Astronomica Betelgeuse (SAB) in Magnago, Italy, and the 30-cm Ritchey Chretien Astrograph at the IRIDA observatory (IO) of the NAO Rozhen in Bulgaria. We applied the Wilson–Devinney code to model the light curves and derive the orbital and physical parameters of the systems. Four of the contact binaries belong to the W sub-type and two to the A sub-type, and all are in thermal contact. 2MASS J23194851+3603503 has a very low mass ratio q = 0.093 and a fill-out factor of <em>f</em> = 71.4%, whereas the other contact binaries have mass ratios between 0.2 and 0.38 and fill-out factors between 8% and 39%. 2MASS J04525351+6246069 is a semi-detached system with q = 0.125 and a temperature difference of 540 K between the components. We also estimated the absolute elements of all seven eclipsing binaries.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"110 ","pages":"Article 102228"},"PeriodicalIF":2.0,"publicationDate":"2024-03-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140332846","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":"Charged anisotropic composite stellar object with strange, polytropic and gaseous matter","authors":"Lilian Olengeile,&nbsp;Jefta M. Sunzu,&nbsp;Jason M. Mkenyeleye","doi":"10.1016/j.newast.2024.102229","DOIUrl":"https://doi.org/10.1016/j.newast.2024.102229","url":null,"abstract":"<div><p>In this study, we build a charged star model with three layers with distinct equations of state. The core, intermediate layer, and envelope layer obey linear, polytropic, and Chaplygin equations of state, respectively. The model satisfies the physical requirements for the matter variables, gravitational potentials, and stability conditions. We have generated within-acceptable range masses and radii for stars. We also recover the masses and radii for the stars PSRJ1903+0327, PSRJ1614-2230, SAXJ1808.4-3658, Vela X-1, and EXO1785-248 from earlier investigations which shows astrophysical significance of our model.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"110 ","pages":"Article 102229"},"PeriodicalIF":2.0,"publicationDate":"2024-03-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140308675","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":"Estimating the absolute parameters of W UMa-type binary stars using Gaia DR3 parallax","authors":"Atila Poro ,&nbsp;Mahya Hedayatjoo ,&nbsp;Maryam Nastaran ,&nbsp;Mahshid Nourmohammad ,&nbsp;Hossein Azarara ,&nbsp;Sepideh AlipourSoudmand ,&nbsp;Fatemeh AzarinBarzandig ,&nbsp;Razieh Aliakbari ,&nbsp;Sadegh Nasirian ,&nbsp;Nazanin Kahali Poor","doi":"10.1016/j.newast.2024.102227","DOIUrl":"https://doi.org/10.1016/j.newast.2024.102227","url":null,"abstract":"<div><p>The accuracy of absolute parameters’ estimation in contact binary systems is important for investigating their evolution and solving some challenges. The Gaia DR3 parallax is one of the methods used for estimating the absolute parameters, in cases where photometric data is the only one that is available. The use of this method includes advantages and limitations that we have described and examined in this study. We selected 48 contact binary systems whose mass ratios were mostly obtained by spectroscopic data, in addition to a number of photometric studies. The target systems were suitable for <span><math><msub><mrow><mi>A</mi></mrow><mrow><mi>V</mi></mrow></msub></math></span> and the Re-normalized Unit Weight Error (RUWE), and their absolute parameters were calculated based on Gaia DR3 parallax, observational information, orbital period, and light cure solution from the literature and catalogs. The outcomes of OO Aql differed significantly from those reported in the literature. Upon analyzing the system’s light curve with TESS data, we concluded that the stars’ temperatures were the reason for this difference, and utilizing Gaia DR3 parallax provided reasonable results. We displayed the target systems on the Hertzsprung–Russell (HR), <span><math><mrow><mi>q</mi><mo>−</mo><msub><mrow><mi>L</mi></mrow><mrow><mi>r</mi><mi>a</mi><mi>t</mi><mi>i</mi><mi>o</mi></mrow></msub></mrow></math></span>, <span><math><mrow><mi>P</mi><mo>−</mo><msub><mrow><mi>M</mi></mrow><mrow><mi>V</mi></mrow></msub></mrow></math></span>, and <span><math><mrow><mi>l</mi><mi>o</mi><mi>g</mi><msub><mrow><mi>M</mi></mrow><mrow><mi>t</mi><mi>o</mi><mi>t</mi></mrow></msub><mo>−</mo><mi>l</mi><mi>o</mi><mi>g</mi><msub><mrow><mi>J</mi></mrow><mrow><mn>0</mn></mrow></msub></mrow></math></span> diagrams, and the systems are in good agreement with the theoretical fits. We showed that the estimation of absolute parameters with this method might be acceptable if <span><math><mrow><mi>Δ</mi><mi>a</mi><mrow><mo>(</mo><msub><mrow><mi>R</mi></mrow><mrow><mo>⊙</mo></mrow></msub><mo>)</mo></mrow></mrow></math></span> is less than <span><math><mrow><mo>∼</mo><mn>0</mn><mo>.</mo><mn>1</mn><mrow><mo>(</mo><msub><mrow><mi>R</mi></mrow><mrow><mo>⊙</mo></mrow></msub><mo>)</mo></mrow></mrow></math></span>. There are open questions regarding the existence of <span><math><msub><mrow><mi>l</mi></mrow><mrow><mn>3</mn></mrow></msub></math></span> in the light curve analysis and its effect on the estimation of absolute parameters with this method.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"110 ","pages":"Article 102227"},"PeriodicalIF":2.0,"publicationDate":"2024-03-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140296386","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":"Cosmic implications of Kaniadakis HDE model in Chern-Simons modified gravity","authors":"Sarfraz Ali,&nbsp;Muhammad Kamran,&nbsp;Umber Sheikh","doi":"10.1016/j.newast.2024.102226","DOIUrl":"10.1016/j.newast.2024.102226","url":null,"abstract":"<div><p>In this study, we investigate the FRW model in the Chern–Simons modified gravity framework, considering holographic dark energy and Kaniadakis holographic dark energy models. Employing the field equation of Chern–Simons gravity, it is analyzed some important cosmological parameters such as density, equation of state, and deceleration parameters for both models. Our findings, presented visually through graphs, reveal that holographic dark energy places the equation of state within <span><math><mrow><mi>ω</mi><mo>∈</mo><mrow><mo>(</mo><mo>−</mo><mn>1</mn><mo>,</mo><mo>−</mo><mn>0</mn><mo>.</mo><mn>4</mn><mo>)</mo></mrow></mrow></math></span>, while Kaniadakis holographic dark energy spans <span><math><mrow><mi>ω</mi><mo>∈</mo><mrow><mo>(</mo><mo>−</mo><mn>0</mn><mo>.</mo><mn>8</mn><mo>,</mo><mo>−</mo><mn>0</mn><mo>.</mo><mn>4</mn><mo>)</mo></mrow></mrow></math></span>. These results demonstrate the dynamic nature of dark energy’s influence. Our study highlights the interplay of quintessence and <span><math><mrow><mi>Λ</mi><mi>CDM</mi></mrow></math></span> across cosmic eras. We identify the ranges of <span><math><mrow><mi>q</mi><mo>∈</mo><mrow><mo>(</mo><mo>−</mo><mn>0</mn><mo>.</mo><mn>89</mn><mo>,</mo><mo>−</mo><mn>0</mn><mo>.</mo><mn>86</mn><mo>)</mo></mrow></mrow></math></span> and <span><math><mrow><mi>q</mi><mo>∈</mo><mrow><mo>(</mo><mo>−</mo><mn>0</mn><mo>.</mo><mn>9925</mn><mo>,</mo><mo>−</mo><mn>0</mn><mo>.</mo><mn>9922</mn><mo>)</mo></mrow></mrow></math></span> for Kaniadakis holographic dark energy and holographic dark energy, offering insights into their roles in cosmic inflation which implies that the universe attributes are impacted by both quintessence and the <span><math><mi>Λ</mi></math></span>CDM model in Chern–Simons modified gravity. In addition, this study implies that the universe’s expansion is decelerating in its current state.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"110 ","pages":"Article 102226"},"PeriodicalIF":2.0,"publicationDate":"2024-03-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140155533","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 fast photometric image alignment algorithm with row and column means","authors":"Jie Zheng ,&nbsp;Linqiao Jiang ,&nbsp;Jianfeng Tian","doi":"10.1016/j.newast.2024.102224","DOIUrl":"https://doi.org/10.1016/j.newast.2024.102224","url":null,"abstract":"<div><p>This paper introduces an astronomical image alignment algorithm. This algorithm uses the means of the rows and columns of the original image for alignment, and finds the optimal offset corresponding to the maximum similarity by comparing different offsets between images. The similarity is evaluated by the standard deviation of the quotient divided by the means. This paper also discusses the theoretical feasibility of this algorithm. Through practical testing, it has been confirmed that the algorithm is fast and robust.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"110 ","pages":"Article 102224"},"PeriodicalIF":2.0,"publicationDate":"2024-03-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140134014","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":"Joule Thomson expansion, Maxwell equal area law and topological interpretation of Phantom RN AdS black holes","authors":"M. Umair Shahzad ,&nbsp;Aqsa Mehmood ,&nbsp;Ramish Gohar ,&nbsp;Ali Övgün","doi":"10.1016/j.newast.2024.102225","DOIUrl":"10.1016/j.newast.2024.102225","url":null,"abstract":"<div><p>This paper is devoted to study the thermodynamic topological defects, Joule–Thomson (<span><math><mrow><mi>J</mi><mo>−</mo><mi>T</mi></mrow></math></span>) and Maxwell’s equal area law of Phantom RN AdS black holes (BHs). The inversion temperatures and inversion curves are obtained and by using the isenthalpic curves in the temperature–pressure (<span><math><mrow><mi>T</mi><mo>−</mo><mi>P</mi></mrow></math></span>) plane to locate the cooling and heating regions. Using Maxwell’s equal-area law, we select different independent conjugate variables to study the phase transitions of Phantom RN AdS BHs. We find that phase transition rely on the electric potential and horizon radius of the BH when its charge is constant. Phase transition of Phantom RN AdS BH are proportional to the ratio of event horizon to its cosmological constant, where the latter is assumed to be constant. Moreover, we consider the Phantom RN AdS BH as defects with a topological nature within thermodynamic domain and examine the local and global topology by computing the winding numbers at the defects, which concludes that the overall topological charge is either equal to 0 or 1.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"110 ","pages":"Article 102225"},"PeriodicalIF":2.0,"publicationDate":"2024-03-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140097593","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":"Double-layered anisotropic stellar model of embedding class I with gaseous envelope","authors":"Amos V. Mathias,&nbsp;Jason M. Mkenyeleye,&nbsp;Jefta M. Sunzu","doi":"10.1016/j.newast.2024.102216","DOIUrl":"https://doi.org/10.1016/j.newast.2024.102216","url":null,"abstract":"<div><p>The current paper presents a double-layered neutral anisotropic stellar model in general relativistic setting. The model is developed by using Einstein field equations and class I embedding condition. We consider the core with quark matter obeying linear equation of state and envelope layer with gaseous matter admitting Chaplygin gas equation of state. The interior and exterior metric coefficients match smoothly at the interface of core and envelope layers and at the stellar surface. The profiles for matter variables, stability and energy conditions show acceptable trend for physical stellar models. In this model, stellar masses and radii consistent with compact stars HerX-1, 4U1538-52, SAXJ1808.4-3658, CenX-3 and SMCX-1 are generated. We note that studies of multi-layered stars with gaseous envelope and embedding class I condition are missing in investigations conducted in the past.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"110 ","pages":"Article 102216"},"PeriodicalIF":2.0,"publicationDate":"2024-03-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140069650","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}