New Astronomy最新文献

{"title":"Learning from core-collapse supernova remnants on the explosion mechanism","authors":"Noam Soker","doi":"10.1016/j.newast.2025.102453","DOIUrl":"10.1016/j.newast.2025.102453","url":null,"abstract":"<div><div>I estimate some typical properties of the jittering jets explosion mechanism (JJEM) to distinguish it from competing supernova explosion models. From the imprints of jittering jets in the outskirts of some CCSN remnants, I estimate the half-opening angles of jittering jets that shape CCSN remnants to be <span><math><mrow><msub><mrow><mi>α</mi></mrow><mrow><mi>j</mi></mrow></msub><mo>≃</mo><msup><mrow><mn>1</mn></mrow><mrow><mo>∘</mo></mrow></msup><mo>−</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>∘</mo></mrow></msup></mrow></math></span>. I also estimate that intermittent accretion disks around the newly born neutron star (NS) can launch jets after they live for only several times their orbital period around the NS. To operate, the JJEM requires intermittent accretion disks that launch jets to amplify the magnetic fields in a dynamo, and the magnetic fields to reconnect and release their energy rapidly. I estimate the width of magnetic field reconnection zones to be <span><math><mrow><msub><mrow><mi>D</mi></mrow><mrow><mi>rec</mi></mrow></msub><mo>≈</mo><mn>0</mn><mo>.</mo><mn>005</mn><mi>r</mi><mo>≈</mo><mn>0</mn><mo>.</mo><mn>1</mn><mspace></mspace><mi>km</mi></mrow></math></span> near the surface of the NS. This width requires a numerical resolution several times smaller than the resolution of present CCSN simulations. I argue, therefore, that existing simulations of the CCSN explosion mechanism are still far from correctly simulating CCSN explosions.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"121 ","pages":"Article 102453"},"PeriodicalIF":1.9,"publicationDate":"2025-07-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144672215","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Optical flickering in Mira and mass accretion rate onto the companion white dwarf","authors":"R.K. Zamanov ,&nbsp;B. Spassov ,&nbsp;R. Konstantinova-Antova ,&nbsp;M. Moyseev ,&nbsp;J. Marti ,&nbsp;M.F. Bode ,&nbsp;V. Vujcic ,&nbsp;V. Sreckovic","doi":"10.1016/j.newast.2025.102452","DOIUrl":"10.1016/j.newast.2025.102452","url":null,"abstract":"<div><div>We report photometric observations in Johnson <span><math><mi>B</mi></math></span> and <span><math><mi>V</mi></math></span> bands of the short term variability (flickering) of Mira – the prototypical pulsating asymptotic giant branch (AGB) star. The observations are performed over 4 consecutive nights (24–28 November 2024), during the last minimum of the Mira pulsation. The peak-to-peak amplitude observed is 0.25-0.34 mag in <span><math><mi>B</mi></math></span> band and 0.14-0.19 mag in <span><math><mi>V</mi></math></span> band. For the flickering source we find colour <span><math><mrow><msub><mrow><mrow><mo>(</mo><mi>B</mi><mo>−</mo><mi>V</mi><mo>)</mo></mrow></mrow><mrow><mn>0</mn></mrow></msub><mo>=</mo><mn>0</mn><mo>.</mo><mn>44</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>11</mn></mrow></math></span>, temperature <span><math><mrow><mn>7000</mn><mo>±</mo><mn>700</mn></mrow></math></span> K, and average radius <span><math><mrow><msub><mrow><mi>R</mi></mrow><mrow><mi>f</mi><mi>l</mi></mrow></msub><mo>=</mo><mn>0</mn><mo>.</mo><mn>30</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>07</mn></mrow></math></span> R<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>. Assuming the mass of the white dwarf <span><math><mrow><mo>≈</mo><mn>0</mn><mo>.</mo><mn>6</mn></mrow></math></span> M<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>, we estimate a mass accretion rate <span><math><mrow><mo>≈</mo><mn>6</mn><mo>.</mo><mn>0</mn><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>−</mo><mn>10</mn></mrow></msup></mrow></math></span> M<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span> yr⁻¹ during our observations.</div><div>The data will be available on Zenodo.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"121 ","pages":"Article 102452"},"PeriodicalIF":1.9,"publicationDate":"2025-07-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144655902","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":"Impacts of variable mass disk on region and stability of motion around triangular equilibrium points of the R3BP with variable mass binaries Maxi J1659-152 and Kepler-16","authors":"Veronica Cyril-Okeme ,&nbsp;Oni Leke ,&nbsp;Jessica Gyegwe","doi":"10.1016/j.newast.2025.102457","DOIUrl":"10.1016/j.newast.2025.102457","url":null,"abstract":"&lt;div&gt;&lt;div&gt;The paper explores the impacts of variable mass disk on region and stability of motion of a dust grain around the triangular equilibrium points (TEPs) of the circular restricted three-body problem (R3BP), with variable mass binaries &lt;strong&gt;Maxi J1659-152&lt;/strong&gt; and &lt;strong&gt;Kepler-16&lt;/strong&gt;. The masses of the binaries vary with time under the Mestschersky unified law (MUL) and their motion is described by the Gylden-Mestschersky problem (GMP), with the assumption that the system is enclosed by a non-discrete disk of dust whose mass is also assumed to vary with time under the description of the MUL. Both secondary bodies in the binaries are assumed to be radiation emitters. The time varying system of equations are deduced and transformed to the autonomized equations with constant coefficients. The TEPs of the autonomized and non-autonomous systems are investigated and it is seen that there exists a pair of TEPs defined by the mass parameter&lt;span&gt;&lt;math&gt;&lt;mi&gt;υ&lt;/mi&gt;&lt;/math&gt;&lt;/span&gt;, mass of disk&lt;span&gt;&lt;math&gt;&lt;msub&gt;&lt;mi&gt;μ&lt;/mi&gt;&lt;mi&gt;d&lt;/mi&gt;&lt;/msub&gt;&lt;/math&gt;&lt;/span&gt;and the mass variation parameter&lt;span&gt;&lt;math&gt;&lt;mi&gt;κ&lt;/mi&gt;&lt;/math&gt;&lt;/span&gt;, for the autonomized system while those of the non-autonomous system additionally are defined by a function of time&lt;span&gt;&lt;math&gt;&lt;mi&gt;t&lt;/mi&gt;&lt;/math&gt;&lt;/span&gt;. It is seen that the radial and vertical scale lengths of the disk affects the locations of the TEPs but this impact depends largely on the mass of the disk. Further, the impacts of the varying disks masses on the zero velocity curves (ZVC) of the dust grain around the TEPs, is investigated, and it is seen that, as the disk mass is increasing, the energy level decreases and the region where motion of the dust grain is forbidden increases. Additionally, the regions where motion is allowed around the binaries and the TEPs are determined by the disks masses. Next, we investigate the linear stability of the TEPs of the autonomized system and found it to be stable in some interval of the masses of the disks for both binaries. The TEPs of the non-autonomous system are unstable due to time&lt;span&gt;&lt;math&gt;&lt;mi&gt;t&lt;/mi&gt;&lt;/math&gt;&lt;/span&gt;. To validate the linear stability, we explore the orbital numerical integration around the TEPs and calculated the Lyapunov exponent indicator (LEI) for different masses of the disks. It was observed that the orbits are stable in the interval of the linear stability and their corresponding LEI tend to zero. Finally, we analyze the Poincaré surface of sections (PSS) around the TEPs for the binaries and found that in the range of linearly unstable TEPs, chaos exists while periodic, quasi-periodic trajectories and islands exist in the range of the linearly stable TEPS. This model can be used to analyze the long-term motion of satellites and planets in binary systems with mass variations of disk in the environment. This model can be used to analyze the long-term motion of satellites and planets in binary systems with mass variations of disk in the environment.&lt;/div","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"121 ","pages":"Article 102457"},"PeriodicalIF":1.9,"publicationDate":"2025-07-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144680399","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":"WGAN-based molecular clumps generation","authors":"Tieliang Yu ,&nbsp;Xinqiong Liu ,&nbsp;Yao Huang ,&nbsp;Sheng Zheng ,&nbsp;Xiaoyu Luo ,&nbsp;Chen Long","doi":"10.1016/j.newast.2025.102451","DOIUrl":"10.1016/j.newast.2025.102451","url":null,"abstract":"<div><div>In this paper, a new molecular clumps generation algorithm based on the Wasserstein Generative Adversarial Network (WGAN) is investigated for the problem that the simulated molecular clumps generated by the traditional Gaussian model have a large difference from the measured clumps. The method first generates position–position intensity map of the clump using WGAN and then performs 3D expansion in the direction of the velocity axis using a Gaussian function containing weak noise, which ultimately generates 3D simulated molecular clumps in position–position–velocity (PPV) space. Semi-supervised molecular clumps validation algorithm (SS-3D-Clump) is utilized to validate the 3D molecular clumps data generated by the method, and the confidence level of them are above 0.999. Experimentally, it is proved that the new method can provide simulated clumps with morphology and intensity closer to the measured clumps. The simulated molecular clumps are used on the one hand to generate PPV data in combination with measured backgrounds for testing the performance of molecular clump detection algorithms; on the other hand, they can also be used to supplement the 3D molecular clump samples. Experiments have demonstrated that, if 30%–50% of the measured positive samples are retained in the VoxNet training set, and the rest are simulated clumps generated, the classification accuracy can also be guaranteed.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"121 ","pages":"Article 102451"},"PeriodicalIF":1.9,"publicationDate":"2025-07-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144580361","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":"Mass–radius relationship of strongly magnetized deformed white dwarfs","authors":"Rajasmita Sahoo ,&nbsp;Tambe Pranjal Anant ,&nbsp;Somnath Mukhopadhyay","doi":"10.1016/j.newast.2025.102450","DOIUrl":"10.1016/j.newast.2025.102450","url":null,"abstract":"<div><div>The masses and radii of strongly magnetized anisotropic deformed white dwarf stars are investigated using the stellar structure equations in the parameterized <span><math><mi>γ</mi></math></span>-metric formalism. The Equation of State (EoS) of a completely degenerate relativistic electron gas in strong quantizing density-dependent magnetic field is developed. The fluid and field pressure anisotropy among the parallel and perpendicular components to the magnetic field is taken into consideration. This anisotropy in the EoS causes axisymmetric deformation of the star. We found stable solutions of deformed super-Chandrasekhar ultramassive white dwarfs. At a fixed central electron number density, the mass first increases from the traditional Chandrasekhar limit with increase of central magnetic field strength, reaches a maximum and then decreases with further increase of central magnetic field. For lower central magnetic field strengths, both the pressure anisotropy and the resulting deformation are very less, and hence the mass increases. In the higher central magnetic field regime, the magnetic field pressure anisotropy becomes significantly strong. This leads to greater deformation from spherical symmetry and hence reduces the stellar mass. We also see that the maximum mass and its corresponding equatorial radius both decrease as central magnetic field strength increases. We also notice that the maximum mass occurs at higher central density as the magnetic field increases. These phenomena also occur because of the deviation from spherical symmetry due to higher pressure anisotropy. High magnetic field increases stellar compactness.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"121 ","pages":"Article 102450"},"PeriodicalIF":1.9,"publicationDate":"2025-07-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144580360","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":"Libration points for ER3BP with triaxial and radiating bodies and numerical integration using Lie series","authors":"A. Chakraborty","doi":"10.1016/j.newast.2025.102448","DOIUrl":"10.1016/j.newast.2025.102448","url":null,"abstract":"<div><div>This paper examines the Elliptic Restricted Three Body Problem (ER3BP) in which the primaries are triaxial radiating bodies. Using both analytical and numerical techniques, the problem’s planar equilibrium locations were obtained. For specific triaxiality values, it was found that there are more than five classically identified equilibrium locations. Additionally, a comparison of the equilibrium points’ positions as determined analytically and numerically was conducted. In order to determine the problem’s solution, the formulation of the iterative expression for the Lie series terms was expanded in the final section. The impact of the primaries’ triaxiality on the orbit is depicted graphically in the Lie series solution of triangular equilibria.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"121 ","pages":"Article 102448"},"PeriodicalIF":1.9,"publicationDate":"2025-06-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144518343","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":"In-depth analysis of the light curve and first orbital period of contact binary GM Dra","authors":"M.F. Yıldırım","doi":"10.1016/j.newast.2025.102445","DOIUrl":"10.1016/j.newast.2025.102445","url":null,"abstract":"<div><div>This study presents the light curve (LC) analysis of the GM Dra eclipsing binary (using data from TESS, SuperWASP, KWS(<span><math><msub><mrow><mi>I</mi></mrow><mrow><mi>c</mi></mrow></msub></math></span>), Hipparcos, and ASAS-SN), along with a detailed investigation of its orbital period (OP) for the first time. Photometric data obtained from five different databases were used to simultaneously analyze the system’s LC and radial velocity (RV). The LC modeling results for GM Dra reveal the object stars’ masses and radii as follows: <span><math><mrow><msub><mrow><mi>M</mi></mrow><mrow><mn>1</mn></mrow></msub><mo>=</mo><mn>0</mn><mo>.</mo><mn>28</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>01</mn></mrow></math></span> M<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>, <span><math><mrow><msub><mrow><mi>M</mi></mrow><mrow><mn>2</mn></mrow></msub><mo>=</mo><mn>1</mn><mo>.</mo><mn>34</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>02</mn></mrow></math></span> M<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>, <span><math><mrow><msub><mrow><mi>R</mi></mrow><mrow><mn>1</mn></mrow></msub><mo>=</mo><mn>0</mn><mo>.</mo><mn>64</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>01</mn></mrow></math></span> R<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>, and <span><math><mrow><msub><mrow><mi>R</mi></mrow><mrow><mn>2</mn></mrow></msub><mo>=</mo><mn>1</mn><mo>.</mo><mn>27</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>02</mn></mrow></math></span> R<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>. A total of 108 eclipse times (ETs) were calculated on the basis of TESS and SuperWASP observations. These ETs are of great significance in determining the OP change. The OP of the GM Dra has been analyzed based on long-term observations, revealing that the OP of GM Dra is decreasing by 0.051 s per year. A sinusoidal variation in the period change was also identified, which may be attributed to the presence of a potential third object or magnetic activity. These findings provide significant insights into the evolutionary status (the positions of the system in the Hertzsprung–Russell (HR) diagram and logM<span><math><msub><mrow></mrow><mrow><mi>t</mi><mi>o</mi><mi>t</mi><mo>.</mo></mrow></msub></math></span>–logJ diagram were discussed) of GM Dra and the dynamics of the binary system.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"121 ","pages":"Article 102445"},"PeriodicalIF":1.9,"publicationDate":"2025-06-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144480598","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Multi-point observation of a CME on August 16, 2020","authors":"Marcel Nogueira de Oliveira ,&nbsp;Carlos E. Navia ,&nbsp;Andre Asevedo Nepomuceno","doi":"10.1016/j.newast.2025.102446","DOIUrl":"10.1016/j.newast.2025.102446","url":null,"abstract":"<div><div>On August 16, 2020, at 17:12 UT, a long-duration B1.2-class flare erupted from a filament in the southeastern hemisphere, originating from an active region at <span><math><mrow><mn>32</mn><mo>°</mo></mrow></math></span>S, <span><math><mrow><mn>26</mn><mo>°</mo></mrow></math></span>E, near a large equatorial coronal hole (CH). According to LASCO coronagraph images from the L1 point, the associated CME erupted with a principal angle (PA) of approximately <span><math><mrow><mn>99</mn><mo>°</mo></mrow></math></span>, close to the ecliptic plane, and at a speed of 437 km/s. Consequently, the Lorentz force between the CH’s magnetic field and the CME deflected the CME about <span><math><mrow><mn>30</mn><mo>°</mo></mrow></math></span> northward. NOAA’s CME propagation models predicted a possible impact on Earth on August 19 around 22:00 UT. However, no signs of the CME were detected at Earth. Meanwhile, STEREO-A observed a disturbance in the solar wind around 19:00 UT, consistent with a CME impact. Considering that the magnetic field and solar wind plasma move together (i.e., under the frozen-in flux condition), and due to the Sun’s rotation, parcels of solar wind plasma spiral outward from the Sun (forming the Parker spiral). The solar wind spiral motion dragged the CME, deflecting it approximately <span><math><mrow><mn>30</mn><mo>°</mo></mrow></math></span> eastward during its propagation to 1 AU, ultimately directing it toward STEREO-A’s location. Furthermore, remote-tracking observations from the two broadband visible-light refracting camera systems (HI-1 and HI-2) aboard STEREO-A captured the CME in J-plot images, tracking it from its eruption to its impact. Additionally, the bi-directional flow of suprathermal electrons observed by STEREO-A during the first 12 h of August 19, 2020, indicates that the CME crossed a high-speed stream (HSS) sector. An isotropic flux of suprathermal electrons observed around 19:00 UT further confirms the CME’s impact in STEREO-A’s vicinity.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"121 ","pages":"Article 102446"},"PeriodicalIF":1.9,"publicationDate":"2025-06-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144480597","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 detectability of gravitational waves from PSR J0737–3039 with the laser interferometer space antenna: A quadrupole approximation approach","authors":"Zheng Zhou","doi":"10.1016/j.newast.2025.102449","DOIUrl":"10.1016/j.newast.2025.102449","url":null,"abstract":"<div><div>Gravitational waves (GWs) are an important component of gravitational physics. In a binary system, it is emitted through orbital energy loss. In this paper, we explore the Laser Interferometer Space Antenna (LISA)’s detectability of gravitational waves from PSR J0737–3039, the first known binary pulsar system. The system is located around 1150 parsecs from Earth, with an orbital period of ∼2.45 h and an inclination angle of 87°, making it an ideal candidate for testing gravitational physics. We approximated the GW frequency of the system to be ∼2.26 × 10⁻⁴ Hz using rules of orbital frequency. We used the quadrupole formula, a part of the multipole expansion, to estimate that the calculated GW strains (<em>h</em>_<em>✕</em> ∼ 4.8702×10⁻²³ and <em>h</em>₊ ∼ 4.6656×10⁻²²). The strain magnitudes fall below the detector noise curve of LISA. We offer possible explanations for this, including arm length and acceleration noise, while proposing methods to enhance LISA’s sensitivity. These methods include the Noise2Noise algorithm and possibility of the installation of resonant detectors.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"121 ","pages":"Article 102449"},"PeriodicalIF":1.9,"publicationDate":"2025-06-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144491492","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":"uvby−Hβ Photoelectric photometry of 65 A/F-type candidate stars in the Kepler field: Observations, stellar parameters and variability analysis","authors":"L. Fox-Machado ,&nbsp;J.H. Peña ,&nbsp;B. Smalley","doi":"10.1016/j.newast.2025.102436","DOIUrl":"10.1016/j.newast.2025.102436","url":null,"abstract":"<div><div>We present the results of <span><math><mrow><mi>u</mi><mi>v</mi><mi>b</mi><mi>y</mi><mo>−</mo><msub><mrow><mi>H</mi></mrow><mrow><mi>β</mi></mrow></msub><mspace></mspace></mrow></math></span> photoelectric photometry for 65 stars in the Kepler field, focusing on the study of <span><math><mi>δ</mi></math></span> Scuti, <span><math><mi>γ</mi></math></span> Doradus, and hybrid-type stars. The observing procedures and methodology used to derive the Strömgren indices and colors <span><math><mi>V</mi></math></span>, <span><math><mrow><mo>(</mo><mi>b</mi><mo>−</mo><mi>y</mi><mo>)</mo></mrow></math></span>, <span><math><msub><mrow><mi>m</mi></mrow><mrow><mn>1</mn></mrow></msub></math></span>, <span><math><msub><mrow><mi>c</mi></mrow><mrow><mn>1</mn></mrow></msub></math></span>, and <span><math><msub><mrow><mi>H</mi></mrow><mrow><mi>β</mi></mrow></msub></math></span> are described in detail. We identify dwarfs and giants within the sample and report their physical parameters. For 47 stars, <span><math><msub><mrow><mi>T</mi></mrow><mrow><mi>eff</mi></mrow></msub></math></span> and <span><math><mrow><mo>log</mo><mspace></mspace><mi>g</mi><mspace></mspace></mrow></math></span> determined from our indices were previously reported by Uytterhoeven et al. (2011), while for the remaining stars, these parameters are provided in this work. Additionally, we revisit the variability classifications of these stars by analyzing all available Kepler and TESS light curves and confirm most of the pulsation classifications assigned in previous studies.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"121 ","pages":"Article 102436"},"PeriodicalIF":1.9,"publicationDate":"2025-06-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144364962","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}