New Astronomy最新文献

{"title":"A portable S-DIMM developed for preliminary measurement of seeing for Solar Site Survey: Theory and one case study","authors":"Xiao-Mei Duan ,&nbsp;Yu Liu ,&nbsp;Teng-Fei Song ,&nbsp;Feng-Rong Zhu","doi":"10.1016/j.newast.2024.102206","DOIUrl":"10.1016/j.newast.2024.102206","url":null,"abstract":"<div><p>Imaging quality is highly important for astronomical observations. The imaging quality of a telescope depends not only on the capabilities of the telescope itself but also on its location. When distant stars pass the atmosphere, due to the presence of atmospheric turbulence, the imaging quality becomes degraded. The atmospheric coherence length is the most commonly used parameter to evaluate the influence of the local atmospheric turbulence on telescopes. It is used to describe the degree of atmospheric attenuation of image quality. For the preliminary estimation of atmospheric daytime seeing from a lot of candidate sites, we have developed a portable S-DIMM (PS-DIMM),which is mainly composed of a light-duty tracking mount, a 9 cm aperture lens barrel and a Canon 60D SLR camera. With the PS-DIMM the daytime seeing of a site can be well estimated by measuring the relative displacement variance of the edge positions at both ends of the Sun’s diameter. The principle of PS-DIMM is introduced in this paper. The simultaneous seeing measurements by it and the traditional S-DIMM were carried out at the Fuxian Lake Solar Station, showing a very well correlated between them but with an offset of 2.6 cm. In contrast to the traditional S-DIMM, PS-DIMM offers the advantages of reduced weight and enhanced portability. The utilization of PS-DIMM has played an important role in the early stages of the site survey for the next-generation solar telescopes.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":null,"pages":null},"PeriodicalIF":2.0,"publicationDate":"2024-02-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139918391","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":"Unveiling compact planetary nebulae: Broad-band survey analysis and LAMOST confirmation","authors":"L.A. Gutiérrez-Soto ,&nbsp;M. Belén Mari ,&nbsp;W.A. Weidmann ,&nbsp;F.R. Faifer","doi":"10.1016/j.newast.2024.102207","DOIUrl":"10.1016/j.newast.2024.102207","url":null,"abstract":"<div><p>Planetary nebulae (PNe) are pivotal for advancing our knowledge of stellar evolution and galactic chemical enrichment. Recent progress in surveys and data analysis has revolutionized PN research, leading to the discovery of new objects and deeper insights into their properties. We have devised a novel photometric selection method, integrating GAIA and Pan-STARRS photometry, to identify compact PN candidates. This approach utilizes color–color diagrams, specifically <span><math><mrow><mo>(</mo><mi>G</mi><mo>−</mo><mi>g</mi><mo>)</mo></mrow></math></span> versus <span><math><mrow><mo>(</mo><msub><mrow><mi>G</mi></mrow><mrow><mi>B</mi><mi>P</mi></mrow></msub><mo>−</mo><msub><mrow><mi>G</mi></mrow><mrow><mi>R</mi><mi>P</mi></mrow></msub><mo>)</mo></mrow></math></span> and <span><math><mrow><mo>(</mo><mi>G</mi><mo>−</mo><mi>r</mi><mo>)</mo></mrow></math></span> versus <span><math><mrow><mo>(</mo><msub><mrow><mi>G</mi></mrow><mrow><mi>B</mi><mi>P</mi></mrow></msub><mo>−</mo><msub><mrow><mi>G</mi></mrow><mrow><mi>R</mi><mi>P</mi></mrow></msub><mo>)</mo></mrow></math></span>, as primary criteria for candidate selection. The subsequent verification step involves confirming these candidates through LAMOST spectroscopic data. By cross-referencing a comprehensive dataset of PNe, GAIA, Pan-STARRS, and LAMOST DR7 spectra, we explore the potential of our approach and the crucial role played by these surveys in the field of PN research. The LAMOST spectra provide compelling evidence supporting our selection criteria, especially for compact PNe characterized by strong emission lines and low continuum. This characteristic spectral profile in LAMOST data underscores its effectiveness in confirming compact PNe, enabling clear differentiation based on distinctive spectral features. Applying these criteria to a catalog of emission line objects, we have selected a PN candidate. Detailed analysis of its LAMOST spectrum unveiled classical Balmer emission lines and high-ionization lines (He<span>ii</span>, [Ar<span>v</span>], [Ar<span>iii</span>], and [Ne<span>iii</span>]), characteristic of high-ionization PNe, with an absence of low-excitation lines. Utilizing the 1D-photoionization code <span>cloudy</span>, our modeling revealed crucial parameters, including an ionizing source with an effective temperature of 180<span><math><mrow><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>3</mn></mrow></msup></mrow></math></span> K, luminosity around 3,400 L<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>, and gas abundances encompassing various elements. Comparing the PN’s evolution track, the progenitor star was estimated to have a mass of 2M<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>. Our findings show the greatest promise for cleanly separating compact PNe from other objects and provide a robust framework for further exploration of these surveys in the context of planetary nebulae.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":null,"pages":null},"PeriodicalIF":2.0,"publicationDate":"2024-02-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139918392","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":"Novel hydrodynamic schemes capturing shocks and contact discontinuities and comparison study with existing methods","authors":"Takuhiro Yuasa ,&nbsp;Masao Mori","doi":"10.1016/j.newast.2024.102208","DOIUrl":"https://doi.org/10.1016/j.newast.2024.102208","url":null,"abstract":"<div><p>We present a new hydrodynamic scheme named Godunov Density-Independent Smoothed Particle Hydrodynamics (GDISPH), that can accurately handle shock waves and contact discontinuities without any manually tuned parameters. This is in contrast to the standard formulation of smoothed particle hydrodynamics (SSPH), which requires the parameters for an artificial viscosity term to handle the shocks and struggles to accurately handle the contact discontinuities due to unphysical repulsive forces, resulting in surface tension that disrupts pressure equilibrium and suppresses fluid instabilities. While Godunov SPH (GSPH) can handle the shocks without the parameters by using solutions from a Riemann solver, it still cannot fully handle the contact discontinuities. Density-Independent Smoothed Particle Hydrodynamics (DISPH), one of several schemes proposed to handle contact discontinuities more effectively than SSPH, demonstrates superior performance in our tests involving strong shocks and contact discontinuities. However, DISPH still requires the artificial viscosity term. We integrate the Riemann solver into DISPH in several ways, yielding some patterns of GDISPH. The results of standard tests such as the one-dimensional Riemann problem, pressure equilibrium, Sedov–Taylor, and Kelvin–Helmholtz tests are favourable to GDISPH Case 1 and GDISPH Case 2, as well as DISPH. We conclude that GDISPH Case 1 has an advantage over GDISPH Case 2effectively handling shocks and contact discontinuities without the need for specific parameters or introducing any additional numerical diffusion.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":null,"pages":null},"PeriodicalIF":2.0,"publicationDate":"2024-02-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139901256","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":"Impact of modified gravitational theory on the viability of wormhole structures","authors":"M. Zeeshan Gul,&nbsp;M. Sharif,&nbsp;Iqra Kanwal","doi":"10.1016/j.newast.2024.102204","DOIUrl":"https://doi.org/10.1016/j.newast.2024.102204","url":null,"abstract":"<div><p>This paper explores the existence of viable traversable wormhole solutions in the framework of <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>R</mi><mo>,</mo><mi>G</mi><mo>)</mo></mrow></mrow></math></span> theory, where <span><math><mi>R</mi></math></span> represents the Ricci scalar and <span><math><mi>G</mi></math></span> denotes the Gauss–Bonnet term. We study the wormhole geometry by focusing on a static spherical spacetime with anisotropic matter configuration. The suitable shape function for the static wormhole structure is developed through the Karmarkar condition. Using this developed shape function, we construct a wormhole geometry that fulfills all the required constraints and connects asymptotically flat regions of the spacetime. Energy bounds are examined for various <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>R</mi><mo>,</mo><mi>G</mi><mo>)</mo></mrow></mrow></math></span> models to analyze the existence of traversable wormhole geometry. We investigate the stability of the wormhole solutions using the Tolman–Oppenheimer–Volkoff equation. The rigorous analysis and satisfaction of necessary conditions lead to the conclusion that the viable traversable wormhole solutions exist in this framework, offering a deep understanding of the spacetime and the possible existence of traversable shortcuts in the universe.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":null,"pages":null},"PeriodicalIF":2.0,"publicationDate":"2024-02-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139737219","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":"Berkeley 76: An intermediate age open star cluster in Gaia Era","authors":"Deepak Bisht ,&nbsp;D. Bisht ,&nbsp;A. Raj ,&nbsp;Geeta Rangwal ,&nbsp;Devesh P. Sariya ,&nbsp;Mehul Manu","doi":"10.1016/j.newast.2024.102205","DOIUrl":"https://doi.org/10.1016/j.newast.2024.102205","url":null,"abstract":"<div><p>We studied the open star cluster Berkeley 76 using Gaia DR3 and 2MASS data sets. We obtained 314 most probable cluster members with a membership probability greater than 80%. We have found the cluster center as <span><math><mi>α</mi></math></span> = 106.67 ± 0.07 deg and <span><math><mrow><mi>δ</mi><mo>=</mo><mo>−</mo><mn>11</mn><mo>.</mo><mn>75</mn><mspace></mspace><mo>±</mo><mspace></mspace></mrow></math></span>0.07 deg. The mean PMs of cluster members in right ascension and declination are <span><math><mrow><mo>−</mo><mn>0</mn><mo>.</mo><mn>60</mn><mspace></mspace><mo>±</mo><mspace></mspace></mrow></math></span>0.22 and 1.35 ± 0.19 mas yr⁻¹, respectively. The radial density profile estimates the cluster’s radius to be 4.5 arcmin. The cluster’s heliocentric distance is estimated as 4.27<span><math><msup><mrow></mrow><mrow><mo>±</mo></mrow></msup></math></span>0.91 kpc, and its age is determined as <span><math><mrow><mn>1</mn><mo>.</mo><mn>60</mn><mspace></mspace><mo>±</mo><mspace></mspace><mn>0</mn><mo>.</mo><mn>35</mn></mrow></math></span> Gyr. Using the most probable cluster members, we determined the mass function slope for Berkeley 76 as <span><math><mi>1.57 ± 0.19</mi></math></span>. This value is close to Salpeter’s slope within the uncertainty. Berkeley 76 is a dynamically relaxed cluster with a relaxation time of <strong>23.4</strong> Myr.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":null,"pages":null},"PeriodicalIF":2.0,"publicationDate":"2024-02-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139719349","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":"Role of modified Chaplygin gas in Little Rip phenomena from interaction between dark energy and dark matter","authors":"Rajani Shelote","doi":"10.1016/j.newast.2024.102203","DOIUrl":"https://doi.org/10.1016/j.newast.2024.102203","url":null,"abstract":"<div><p>In this article, an interacting dark energy (DE)- dark matter (DM) scenario has been considered in a flat Friedmann–Lemaitre–Robertson–Walker (FLRW) cosmological model, where DE has a variable equation-of-state that follows the modified Chaplygin-like equation of state (Eq. <span>(1)</span>) characterized by two time dependent parameters <span><math><mrow><mi>Λ</mi><mrow><mo>(</mo><mi>t</mi><mo>)</mo></mrow></mrow></math></span> and <span><math><mrow><mi>ω</mi><mrow><mo>(</mo><mi>t</mi><mo>)</mo></mrow></mrow></math></span> and DM has a non-zero equation of state <span><math><mrow><msub><mrow><mi>p</mi></mrow><mrow><mi>D</mi><mi>M</mi></mrow></msub><mo>=</mo><mover><mrow><mi>ω</mi></mrow><mrow><mo>̃</mo></mrow></mover><msub><mrow><mi>ρ</mi></mrow><mrow><mi>D</mi><mi>M</mi></mrow></msub></mrow></math></span>. Gravitational equations of motion for dark matter have been solved for two different cases of thermodynamic parameter <span><math><mover><mrow><mi>ω</mi></mrow><mrow><mo>̃</mo></mrow></mover></math></span> as <span><math><mrow><mover><mrow><mi>ω</mi></mrow><mrow><mo>̃</mo></mrow></mover><mo>=</mo><mi>c</mi><mi>o</mi><mi>n</mi><mi>s</mi><mi>t</mi><mi>a</mi><mi>n</mi><mi>t</mi></mrow></math></span> and <span><math><mrow><mover><mrow><mi>ω</mi></mrow><mrow><mo>̃</mo></mrow></mover><mo>≠</mo></mrow></math></span> constant. Also, it has been found that <span><math><mrow><mi>Λ</mi><mrow><mo>(</mo><mi>t</mi><mo>)</mo></mrow><mo>→</mo><mo>−</mo><mi>∞</mi></mrow></math></span> as <span><math><mrow><mi>t</mi><mo>→</mo><mi>∞</mi></mrow></math></span>, it shows that the fate of our universe depends on specific model parameters for the coupled dark energy and dark matter, and experiences Little Rip behavior. Also, it is observed that coupled dark energy and dark matter may inflate and expand the universe after the Big Bang in the far future.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":null,"pages":null},"PeriodicalIF":2.0,"publicationDate":"2024-02-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139737218","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":"Effect of perturbed potential of heterogeneous triaxial rigid bodies of N layers on the stability of libration points in the R3BP","authors":"Kumari Shalini ,&nbsp;Pankaj Sharma ,&nbsp;Kumari Ranjana","doi":"10.1016/j.newast.2024.102202","DOIUrl":"10.1016/j.newast.2024.102202","url":null,"abstract":"<div><p>In this paper, we investigate the motion of an infinitesimal mass <span><math><msub><mrow><mi>m</mi></mrow><mrow><mn>3</mn></mrow></msub></math></span> in the restricted three-body problem by taking both the primaries as heterogeneous triaxial rigid bodies with <em>N</em> layers. The potential of the proposed model and the equations of motion for the infinitesimal mass <span><math><msub><mrow><mi>m</mi></mrow><mrow><mn>3</mn></mrow></msub></math></span> are derived. Our findings reveal the existence of five libration points denoted as <span><math><msub><mrow><mi>L</mi></mrow><mrow><mi>i</mi></mrow></msub></math></span> <span><math><mrow><mo>(</mo><mi>i</mi><mo>=</mo><mn>1</mn><mo>,</mo><mn>2</mn><mo>,</mo><mn>3</mn><mo>,</mo><mn>4</mn><mo>,</mo><mn>5</mn><mo>)</mo></mrow></math></span> in the proposed model, with three being collinear and two being non-collinear. We observed that the collinear libration points <span><math><mrow><msub><mrow><mi>L</mi></mrow><mrow><mi>i</mi></mrow></msub><mrow><mo>(</mo><mi>i</mi><mo>=</mo><mn>1</mn><mo>,</mo><mn>2</mn><mo>,</mo><mn>3</mn><mo>)</mo></mrow></mrow></math></span> are unstable, whereas the non-collinear libration points <span><math><msub><mrow><mi>L</mi></mrow><mrow><mn>4</mn><mo>,</mo><mn>5</mn></mrow></msub></math></span> are conditionally stable for the mass parameter <span><math><mrow><mi>μ</mi><mo>∈</mo><mrow><mo>(</mo><mn>0</mn><mo>,</mo><msub><mrow><mi>μ</mi></mrow><mrow><mi>c</mi></mrow></msub><mo>)</mo></mrow></mrow></math></span>, where <span><math><mrow><msub><mrow><mi>μ</mi></mrow><mrow><mi>c</mi></mrow></msub><mo>=</mo><mn>0</mn><mo>.</mo><mn>25681</mn><mspace></mspace><msub><mrow><mi>k</mi></mrow><mrow><mn>1</mn></mrow></msub><mo>−</mo><mn>1</mn><mo>.</mo><mn>31619</mn><mspace></mspace><msub><mrow><mi>k</mi></mrow><mrow><mn>2</mn></mrow></msub><mo>−</mo><mn>2</mn><mo>.</mo><mn>24318</mn><mspace></mspace><msub><mrow><mi>k</mi></mrow><mrow><mn>3</mn></mrow></msub><mo>−</mo><mn>6</mn><mo>.</mo><mn>10258</mn><mspace></mspace><msub><mrow><mi>k</mi></mrow><mrow><mn>4</mn></mrow></msub></mrow></math></span>.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":null,"pages":null},"PeriodicalIF":2.0,"publicationDate":"2024-02-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139679418","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":"Structure of compact stars: A pure geometric approach","authors":"M.I. Wanas ,&nbsp;Samah A. Ammar ,&nbsp;Mona M. Foda","doi":"10.1016/j.newast.2024.102201","DOIUrl":"10.1016/j.newast.2024.102201","url":null,"abstract":"<div><p>This paper uses pure geometric field theory to construct a stellar model for a static spherically symmetric anisotropic compact star. The expression pure geometry means that all physical quantities and fields are defined in terms of the geometric objects of the geometry used. This implies the possibility of defining the material-energy tensor geometrically, not phenomenologically, from the geometry under consideration, absolute parallelism (AP-) geometry. Two solutions are obtained for the field equations of the theory, an interior solution and an exterior solution. The stellar model is obtained as an analytical solution of the field equations within the material distribution. An equation of state for anisotropic material distribution is derived from the model rather than being imposed on it. The vacuum solution of the field equations coincides with the Schwarzschild exterior solution. Matching the interior and exterior solutions at the boundary of the stellar configuration enables fixing the integration constants. The physical acceptability and stability analysis of the model are discussed, and the results show that the present model is suitable for studying the envelope region of a neutron star in a core-envelope type model. The model is investigated graphically using the estimated data of the pulsar 4U1820-30 with mass <span><math><mrow><mn>1</mn><mo>.</mo><mn>58</mn><mspace></mspace><msub><mrow><mi>M</mi></mrow><mrow><mo>⊙</mo></mrow></msub></mrow></math></span> and radius 9.1 km. In conclusion, this study demonstrates the feasibility of constructing a pure geometric stellar model and highlights the benefits of using such an approach to understand stellar structure.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":null,"pages":null},"PeriodicalIF":2.0,"publicationDate":"2024-02-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139666616","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":"Particle dynamics and thermodynamical analysis of the rotating ModMax black holes","authors":"Khurshid Karshiboev ,&nbsp;Farruh Atamurotov ,&nbsp;Ali Övgün ,&nbsp;Ahmadjon Abdujabbarov ,&nbsp;Eldor Karimbaev","doi":"10.1016/j.newast.2024.102200","DOIUrl":"10.1016/j.newast.2024.102200","url":null,"abstract":"<div><p><span>In this research paper, we investigate the structure of the horizon and ergosphere of a rotating ModMax black hole. The motion of test particles is analyzed by studying the characteristics of the innermost stable circular orbit (ISCO) and the behavior of the effective potential. Different values of the screening factor </span><span><math><mi>γ</mi></math></span> and the <span><math><mi>Q</mi></math></span><span> charge of the rotating ModMax black hole are explored in this study. Moreover, we also examine several thermodynamic quantities such as Enthalpy, Hawking temperature, Gibbs free energy, and entropy of the black hole. Additionally, the center-of-mass-energy (CM) generated by the collision of two particles (both in extremal and non-extremal cases) is briefly investigated for specific parameter values associated with this black hole.</span></p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":null,"pages":null},"PeriodicalIF":2.0,"publicationDate":"2024-02-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139666836","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":"Gaia (DR3)-based astronomical analysis of the seven unstudied open star clusters","authors":"W.A. Badawy ,&nbsp;A.L. Tadross ,&nbsp;Y.H.M. Hendy ,&nbsp;M.N. Ismail ,&nbsp;A. Mouner","doi":"10.1016/j.newast.2024.102196","DOIUrl":"10.1016/j.newast.2024.102196","url":null,"abstract":"<div><p>The seven open star clusters FSR 0717, FSR 1698, Loden 2313, Ruprecht 49, Majaess 61, Mayer 2, and Teutsch 48, which are located near the Milky Way’s Galactic plane are studied in this article using the Gaia DR3 dataset. The estimated numbers of potential cluster members are 102, 362, 285, 197, 95, 116, 160, and 397, correspondingly. The calculated radius values are 3.10<!--> <span><math><mo>±</mo></math></span> <!--> <!-->0.20, 3.20<!--> <span><math><mo>±</mo></math></span> <!--> <!-->0.30, 5.10<!--> <span><math><mo>±</mo></math></span> <!--> <!--> <!-->0.10, 5.30<!--> <span><math><mo>±</mo></math></span> <!--> <!-->0.20, 4.50<!--> <span><math><mo>±</mo></math></span> <!--> <!-->0.40, 3.50<!--> <span><math><mo>±</mo></math></span> <!--> <!-->0.20, and 5.20<!--> <span><math><mo>±</mo></math></span> <!--> <!-->0.20 arcmin, respectively. The clusters’ log ages of 8.80<!--> <span><math><mo>±</mo></math></span> <!--> <!-->0.15, 7.80<!--> <span><math><mo>±</mo></math></span> <!--> <!-->0.05, 6.95<!--> <span><math><mo>±</mo></math></span> <!--> <!-->0.05, 8.00<!--> <span><math><mo>±</mo></math></span> <!--> <!-->0.10, 8.70<!--> <span><math><mo>±</mo></math></span> <!--> <!-->0.05, 7.95<!--> <span><math><mo>±</mo></math></span> <!--> <!-->0.10, and 8.95<!--> <span><math><mo>±</mo></math></span> <!--> <!-->0.05 yr are determined using solar metallicity isochrones. The distances of 3176.76<!--> <span><math><mo>±</mo></math></span> <!--> <!-->17.30, 2122.76<!--> <span><math><mo>±</mo></math></span> <!--> <!-->14.35, 1157.07<!--> <span><math><mo>±</mo></math></span> <!--> <!-->15.20, 3924.10<!--> <span><math><mo>±</mo></math></span> <!--> <!-->20.10, 2513.21<!--> <span><math><mo>±</mo></math></span> <!--> <!-->9.04, 3364.34<!--> <span><math><mo>±</mo></math></span> <!--> <!-->8.01, and 3505.36<!--> <span><math><mo>±</mo></math></span> <!--> <!-->7.93 pc that were obtained by the isochrone’s best fitting are comparable to the distances determined by inverting median parallaxes. The slopes of the mass function are matched the Salpeter mean value. Total masses are determined to be 128.55<!--> <span><math><mo>±</mo></math></span> <!--> <!-->11, 548.30<!--> <span><math><mo>±</mo></math></span> <!--> <!-->8, 254.57<!--> <span><math><mo>±</mo></math></span> <!--> <!-->7, 194.09<!--> <span><math><mo>±</mo></math></span> <!--> <!-->6, 92.32<!--> <span><math><mo>±</mo></math></span> <!--> <!-->15, 191.50<!--> <span><math><mo>±</mo></math></span> <!--> <!-->12, and 455.62<!--> <span><math><mo>±</mo></math></span> <!--> <!-->10 <span><math><msub><mrow><mi>M</mi></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>, respectively.</p></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":null,"pages":null},"PeriodicalIF":2.0,"publicationDate":"2024-02-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139666463","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}