New Astronomy最新文献

{"title":"Spectroscopic and photometric study for five late G- to K-type short-period contact binaries","authors":"Qing Dong ,&nbsp;Raúl Michel ,&nbsp;Zhi-Hua Wang ,&nbsp;Iván Mora Zamora","doi":"10.1016/j.newast.2024.102329","DOIUrl":"10.1016/j.newast.2024.102329","url":null,"abstract":"<div><div>We reported spectroscopy and photometry for five ultra-short period W UMa-type contact binaries. Eleven sets of low resolution spectra are obtained from the Large Sky Area Multiobject Fiber Spectroscopic Telescope (LAMOST) database and analyzed. It has been determined that these systems are late G- to K-type stars: G7V for J0658, G9V for LINEAR 3562115, K0V for PS Com, and K5V for LINEAR 11570575. Additionally, it was observed that the cooler the star, the stronger the sodium absorption line. Seven sets of complete light curves, including two sets of TESS data for PS Com and V0568 Peg, were analyzed using the W-D code. All the five targets are W-subtype systems with mass ratios (<span><math><mi>q</mi></math></span>) greater than 1. The light curves of the two medium contact systems (J0658 and LINEAR 11570575) are symmetric. In contrast, the light curves of the three shallow contact binaries (LINEAR 3562115, PS Com, and V0568 Peg) show differences between their two maxima, Max.I and Max.II, suggesting the presence of cool or hot spots on their surfaces. According to the H-R diagram, the more massive components of these targets are situated between the ZAMS and TAMS, while the less massive ones are overheated due to energy transfer within the common envelope. As these binaries lose angular momentum, they will evolve into deep, low mass ratio contact binaries.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"116 ","pages":"Article 102329"},"PeriodicalIF":1.9,"publicationDate":"2024-11-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142747807","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 robust assessment of the local anisotropy of the Hubble constant in the Pantheon+ sample","authors":"Yves-Henri Sanejouand","doi":"10.1016/j.newast.2024.102331","DOIUrl":"10.1016/j.newast.2024.102331","url":null,"abstract":"<div><div>Magnitude predictions of <span><math><mi>Λ</mi></math></span>CDM, as parametrized by the Planck collaboration, are not consistent with the supernova Ia data of the whole Pantheon+ sample even when, in order to take into account the uncertainty about its value, the Hubble constant is adjusted. This is a likely consequence of the increase of the number of low-redshift supernovae in the Pantheon+ sample, with respect to previous such samples.</div><div>In order to find directions in the sky where the Hubble flow is quiet, that is, where model predictions are consistent with both low and high-redshift supernova data, predicted magnitudes of several models were compared to the corrected B band magnitudes of the supernovae of the Pantheon+ sample.</div><div>When supernovae at redshifts below 0.035 are ignored, with <span><math><mrow><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub><mo>=</mo><mn>73</mn><mo>.</mo><mn>4</mn></mrow></math></span> km<span><math><mi>⋅</mi></math></span>s<span><math><mrow><msup><mrow></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup><mi>⋅</mi></mrow></math></span>Mpc⁻¹, <span><math><mi>Λ</mi></math></span>CDM predictions become consistent with Pantheon+ data. This is also the case when subsets of low-redshift supernovae roughly centered on the direction of the CMB dipole are considered, together with high-redshift ones, at least when CMB and peculiar velocities corrections are taken into account for the redshifts. These results seem robust, since they are also obtained with a simple, single-parameter tired-light model.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"116 ","pages":"Article 102331"},"PeriodicalIF":1.9,"publicationDate":"2024-11-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142721320","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 comprehensive study on the K2-type binary V1393 Tau in four-year observations","authors":"Ligang Yu ,&nbsp;Shaung Wang ,&nbsp;Michel Raúl ,&nbsp;Liyun Zhang","doi":"10.1016/j.newast.2024.102330","DOIUrl":"10.1016/j.newast.2024.102330","url":null,"abstract":"<div><div>We carried out a low resolution spectrum, the first ground-based multi-color light curves (LCs) analysis, and Transiting Exoplanet Survey Satellite (TESS) data analysis for the binary V1393 Tau. We determined its spectral type of K2V and updated an orbital period 0.24738715 days. By the Wilson-Devinney program, we solved ten sets of light curves. From the <em>BVRcIc</em>-band <span><math><mrow><mi>L</mi><msub><mrow><mi>C</mi></mrow><mrow><mn>2022</mn><mo>.</mo><mn>11</mn></mrow></msub></mrow></math></span>, we obtained a mass ratio <span><math><mrow><mi>q</mi><mo>=</mo><mn>2</mn><mo>.</mo><mn>500</mn><mrow><mo>(</mo><mn>3</mn><mo>)</mo></mrow></mrow></math></span> and a fill-out factor <span><math><mrow><mi>f</mi><mo>=</mo><mn>11</mn><mo>.</mo><mn>73</mn><mrow><mo>(</mo><mn>6</mn><mo>)</mo></mrow><mtext>%</mtext></mrow></math></span>, which implies that V1393 Tau is a W-type shallow-contact binary. We traced the spot migration and evolution through modeling light curves during the past four years. The spot’s size alternately becomes smaller or bigger, and its longitude intervenes between <span><math><mrow><mi>λ</mi><mo>=</mo><mn>82</mn><mo>.</mo><mn>3</mn><msup><mrow><mn>9</mn></mrow><mrow><mo>∘</mo></mrow></msup></mrow></math></span> in <span><math><mrow><mi>L</mi><msub><mrow><mi>C</mi></mrow><mrow><mi>S</mi><mn>70</mn></mrow></msub></mrow></math></span> and <span><math><mrow><mn>102</mn><mo>.</mo><mn>5</mn><msup><mrow><mn>6</mn></mrow><mrow><mo>∘</mo></mrow></msup></mrow></math></span> in <span><math><mrow><mi>L</mi><msub><mrow><mi>C</mi></mrow><mrow><mn>2022</mn><mo>.</mo><mn>10</mn></mrow></msub></mrow></math></span> except for <span><math><mrow><mi>L</mi><msub><mrow><mi>C</mi></mrow><mrow><mi>S</mi><mn>32</mn></mrow></msub></mrow></math></span>.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"115 ","pages":"Article 102330"},"PeriodicalIF":1.9,"publicationDate":"2024-11-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142654163","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 baryonic mass estimates of the Milky Way halo in the form of high-velocity clouds","authors":"Noraiz Tahir ,&nbsp;Martín López-Corredoira ,&nbsp;Francesco De Paolis","doi":"10.1016/j.newast.2024.102328","DOIUrl":"10.1016/j.newast.2024.102328","url":null,"abstract":"<div><div>The halo of our Galaxy is populated with a significant number of high-velocity clouds (HVCs) moving with a speed up to 500 km/s. It is suggested that these HVCs <em>might</em> contain a non-negligible fraction of the missing baryons. The main aim of the current paper is to estimate the baryonic mass of the Milky Way halo in the form of HVCs in order to constrain a fraction of missing baryons in the form of these clouds. Such findings would give substantial help in the studying halo dynamics of our Galaxy.</div><div>We first estimate the HVCs distance. We consider the most recent and updated HVC catalog, namely the Galactic All Sky Survey (GASS), which, however, covers the southern sky declinations, south of <span><math><mrow><mi>b</mi><mo>≤</mo><mn>6</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>∘</mo></mrow></msup></mrow></math></span>. Following a model presented in the literature, we assume that most of the HVCs (not all of the HVCs in the Milky Way) were ejected from the Magellanic Clouds (MCls) which is at a distance of about 50 kpc. We assume that the HVCs have a temperature in the range of about <span><math><mrow><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>2</mn></mrow></msup></mrow></math></span>–<span><math><mrow><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>4</mn></mrow></msup></mrow></math></span> K, and are distributed in the Galactic halo as the Navarro–Frenk–White (NFW) profile. Since the GASS survey covers a small portion of the sky, we estimate the number of missing clouds by using Monte Carlo (MC) simulations. The next step will be to estimate the total mass of the Milky Way contained in the form of these HVCs. The total mass resulted to be <span><math><mrow><mo>∼</mo><mrow><mo>(</mo><mn>7</mn><mo>±</mo><mn>2</mn><mo>)</mo></mrow><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>9</mn></mrow></msup><msub><mrow><mi>M</mi></mrow><mrow><mo>⊙</mo></mrow></msub></mrow></math></span> in the form of HVCs and compact high-velocity clouds (CHVCs).</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"115 ","pages":"Article 102328"},"PeriodicalIF":1.9,"publicationDate":"2024-11-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142654251","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":"Modifications of SPH towards three-dimensional simulations of an icy moon with internal ocean","authors":"Keiya Murashima ,&nbsp;Natsuki Hosono ,&nbsp;Takayuki R. Saitoh ,&nbsp;Takanori Sasaki","doi":"10.1016/j.newast.2024.102320","DOIUrl":"10.1016/j.newast.2024.102320","url":null,"abstract":"<div><div>There are some traces of the existence of internal ocean in some icy moons, such as the vapor plumes of Europa and Enceladus. This implies a region of liquid water beneath the surface ice shell. Since liquid water would be essential for the origin of life, it is important to understand the development of these internal oceans, particularly their temperature distribution and evolution. The balance between tidal heating and radiative cooling is believed to sustain liquid water beneath an icy moon’s surface. We aim to simulate the tidal heating of an internal ocean in an icy moon using 3-dimensional numerical fluid calculations with the Smoothed Particle Hydrodynamics (SPH) method. We incorporated viscosity and thermal conduction terms into the governing equations of SPH. However, we encountered two issues while calculating rigid body rotation using SPH with a viscous term: (1) conventional viscosity formulations generated unphysical forces that hindered rotation, and (2) there was artificial internal energy partitioning within the layered structure, which was due to the standard SPH formulations. To address the first issue, we modified the viscosity formulation. For the second, we adopted Density Independent SPH (DISPH) developed in previous studies to improve behavior at discontinuous surfaces. Additionally, we implemented radiative cooling using an algorithm to define fluid surfaces via the particle method. We also introduced an equation of state accounting for phase transitions. With these modifications, we have refined the SPH method to encompass all necessary physical processes for simulating the evolution of icy moons with internal oceans.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"115 ","pages":"Article 102320"},"PeriodicalIF":1.9,"publicationDate":"2024-11-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142654161","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":"Photometric study for the short period contact binary V724 And","authors":"Bin Zhang ,&nbsp;Yi-Dan Gao ,&nbsp;Zhen Zhong ,&nbsp;Bing Lv","doi":"10.1016/j.newast.2024.102318","DOIUrl":"10.1016/j.newast.2024.102318","url":null,"abstract":"<div><div>We present the new light curve synthesis and orbital period change analysis of V724 And. We found that it is a W-subtype contact binary system with a mass ratio of q = 2.31 and a fill-out factor of f = 10.8%. The weak O’Connell effect can be explained by a cool star-spot on the more massive component star. By analyzing orbital period changes, it is found that the target displays a secular period decrease superimposed on a cyclic oscillation. The orbital period decreases at a rate of dp/dt = −4.13 × 10⁻⁸ d yr⁻¹, which can be explained by the mass transfer from the more massive one to the less massive component. The new discovery suggests that the semi-amplitude and period of the cyclic variation are A = 0.0013 d and P = 10.54 yr, respectively, which implies that V724 And is a possibly triple system. The minimum mass of the tertiary companion is estimated as M<span><math><msub><mrow></mrow><mrow><mn>3</mn><mi>m</mi><mi>i</mi><mi>n</mi></mrow></msub></math></span> = 0.054 M<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>, which plays an important role during the formation and evolution of the central binary system.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"115 ","pages":"Article 102318"},"PeriodicalIF":1.9,"publicationDate":"2024-10-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142593906","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":"TESS and AAVSO observations of the eclipsing Z Cam-type cataclysmic variable V416 Dra","authors":"Hongfei Yang,&nbsp;Zhongtao Han,&nbsp;Weiwei Na,&nbsp;Hushan Xu,&nbsp;Tingting Yang","doi":"10.1016/j.newast.2024.102319","DOIUrl":"10.1016/j.newast.2024.102319","url":null,"abstract":"<div><div>We present a photometric analysis of the eclipsing Z Cam-type dwarf nova V416 Dra based on TESS and AAVSO data. The AAVSO light curve, spanning nearly 17 years, shows numerous outbursts recurring approximately every 20.2 and 38.6 days. We examined the amplitude vs. recurrence-time relation in V416 Dra, which appears to reflect the common characteristics of long outbursts in Z Cam stars. The TESS light curves revealed that V416 Dra is a shallow eclipse binary and shows some SU UMa-like superoutbursts, which may be related to the special structure of the accretion disk. The period-searching results show that there are the forest of peaks within the period range of 0.4–2.5 days, related to donor star’s activity. Moreover, we also find the presence of some typical quasi-periodic oscillation (QPO) signals with periods of 14–41 and 177–200 min, respectively. These results will help us locate the origin of the QPOs in V416 Dra accurately.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"115 ","pages":"Article 102319"},"PeriodicalIF":1.9,"publicationDate":"2024-10-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142586112","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":"Predicting the Physical Properties of Dark Matter Subhalos from Baryonic Parameters Using Machine Learning","authors":"Moonzarin Reza","doi":"10.1016/j.newast.2024.102316","DOIUrl":"10.1016/j.newast.2024.102316","url":null,"abstract":"<div><div>Dark matter subhalos play an important role in galaxy formation and evolution. However, accurate prediction of dark matter properties remains a challenge of modern-day astronomy. In recent times, machine learning (ML) tools have shown promising results in solving numerous astrophysical problems. In this paper, we use data from the EAGLE simulations to determine the total mass and the half-mass radius of dark matter subhalos using structural properties of gas, star, black hole, and photometric features using gradient boosted decision trees (GBDT) and dense neural network. GBDT does not require data preprocessing, and results in better performance compared to the neural network. According to GBDT, the most important feature for subhalo radius and mass estimation is gas radius and black hole mass respectively. The all-features combined approach results in the highest test accuracy — Pearson’s correlation coefficient = 0.947 and 0.981, coefficient of determination = 0.898 and 0.962, normalized median absolute deviation = 0.111 and 0.114 for radius and mass respectively. We evaluate our model for masses and redshifts beyond its training range and find that GBDT demonstrates significantly better extrapolation capabilities than the neural network. We also test our model on simulations with different resolutions, and find that the discrepancies lie within 10% if the resolution is changed. This novel study incorporates the structural parameters of gas and black hole to determine the dark matter properties using a ML-based approach. The promising results of this study prove that ML tools can improve our current understanding of dark matter, and answer some of the basic cosmological questions.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"115 ","pages":"Article 102316"},"PeriodicalIF":1.9,"publicationDate":"2024-10-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142527652","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":"Slowly rotating charged Bardeen stellar structure","authors":"Adnan Malik ,&nbsp;Zoya Asghar ,&nbsp;M. Farasat Shamir ,&nbsp;Fatemah Mofarreh","doi":"10.1016/j.newast.2024.102314","DOIUrl":"10.1016/j.newast.2024.102314","url":null,"abstract":"<div><div>This paper is devoted to investigating the dynamics of charged stellar structures with Bardeen exterior geometry. For this purpose, firstly a proposed metric coefficient is utilized, which is defined as <span><math><mrow><mi>a</mi><mo>=</mo><mi>N</mi><msup><mrow><mfenced><mrow><mn>1</mn><mo>+</mo><mn>2</mn><mi>h</mi><msup><mrow><mi>r</mi></mrow><mrow><mn>2</mn></mrow></msup></mrow></mfenced></mrow><mrow><mi>m</mi><mo>/</mo><mn>2</mn></mrow></msup></mrow></math></span>. Here, <span><math><mi>h</mi></math></span> and <span><math><mi>N</mi></math></span> are arbitrary constants determined from matching conditions and <span><math><mi>m</mi></math></span> is a positive integer. The pressure and density profiles are found to be positive and monotonically decreasing, with maximum values occurring at the center. Furthermore, the energy conditions and causality conditions are satisfied, and the adiabatic index falls within an acceptable range. The second part of the paper focuses on the dynamics of rotating stars. Numerical values for relevant parameters are assumed to obtain the masses and radii of stars within the desired range. Five different compact stars, namely, <span><math><mrow><mi>V</mi><mi>e</mi><mi>l</mi><mi>a</mi><mi>X</mi><mo>−</mo><mn>1</mn></mrow></math></span>, <span><math><mrow><mi>C</mi><mi>e</mi><mi>n</mi><mi>X</mi><mo>−</mo><mn>3</mn></mrow></math></span>, <span><math><mrow><mn>4</mn><mi>U</mi><mn>1820</mn><mo>−</mo><mn>30</mn></mrow></math></span>, <span><math><mrow><mn>4</mn><mi>U</mi><mn>1608</mn><mo>−</mo><mn>52</mn></mrow></math></span>, and <span><math><mrow><mi>P</mi><mi>S</mi><mi>R</mi><mn>1903</mn><mo>+</mo><mn>327</mn></mrow></math></span>, are considered. The behavior of the moment of inertia of the sphere against the solar mass is investigated, revealing an increase in the moment of inertia with an increase in solar mass. Furthermore, the relationships of mass and energy density against the radius of the compact structure exhibit natural behavior, supporting the acceptability of the analysis. Overall, the study supports the existence of realistic charged compact structures with Bardeen exterior geometry.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"114 ","pages":"Article 102314"},"PeriodicalIF":1.9,"publicationDate":"2024-10-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142418764","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":"Composition tracking for collisions between differentiated bodies in REBOUND","authors":"Noah Ferich ,&nbsp;Anna C. Childs ,&nbsp;Jason H. Steffen","doi":"10.1016/j.newast.2024.102315","DOIUrl":"10.1016/j.newast.2024.102315","url":null,"abstract":"<div><div>Previous research suggests that impacts between planetary embryos and planetesimals during the late stages of planet formation can often determine the percentages of core and mantle material that compose the newly formed planets in a system. Previous studies have attempted to include the composition-changing effects of these collisions in N-body simulations of planet formation, often as post-processing codes. In this paper, we present the Differentiated Body Composition Tracker, a new post-processing tool that uses collisional data collected from the N-body integrator REBOUND to determine the amount of core and mantle material that is transferred between colliding objects and the resulting fragments during an impact. We demonstrate how this code works using the data from 50 REBOUND simulations of planet formation and explore how the parameters in the code affect the core mass fractions of the remaining objects from these simulations. We then investigate how non-uniform distributions of core material across an initial disc affect the final core mass fractions of planets. Under ideal conditions, we find that a combination of giant impacts and planetary embryos enriched in core material could create some of the iron-rich planets that have been discovered.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"114 ","pages":"Article 102315"},"PeriodicalIF":1.9,"publicationDate":"2024-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142418252","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}