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On the Identification of N-rich Metal-poor Field Stars with Future Chinese Space Station Telescope

Research in Astronomy and Astrophysics 2024年第1期24卷 151-164页

作者： Jiajun Zhang Baitian Tang Jiang Chang Xiangxiang Xue JoséGFernández-Trincado Chengyuan Li Long Wang Hao Tian Yang Huang School of Physics and Astronomy Sun Yat-sen UniversityZhuhai 519082China CSST Science Center for the Guangdong-Hong Kong-Macao Greater Bay Area Sun Yat-sen UniversityZhuhai 519082China Purple Mountain Observatory Chinese Academy of SciencesNanjing 210034China Key Lab of Optical Astronomy National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China Instituto de Astronomía Universidad Católica del NorteAv.Angamos 0610AntofagastaChile Key Lab of Space Astronomy and Technology National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China School of Astronomy and Space Science University of Chinese Academy of SciencesBeijing 100049China

During the long term evolution of globular clusters(GCs), some member stars are lost to the field. The recently found nitrogen-rich(N-rich) metal-poor field stars are promising candidates of these GC escapees, since N enhancement is the fingerprint of chemically enhanced populations in GCs. In this work, we discuss the possibility of identifying N-rich metal-poor field stars with the upcoming Chinese Space Station Telescope(CSST). We focus on the main survey camera with NUV, u, g, r, i, z, y filters and slitless spectrograph with a resolution about *** combination of UV sensitive equipment and prominent N-related molecular lines in the UV band bodes well for the identification: the color–color diagram of(u-g) versus(g-r) is capable of separating N-rich field stars from normal halo stars, if metallicity can be estimated without using the information on u-band ***, the synthetic spectra show that a signal-to-noise ratio of 10 is sufficient to identify N-rich field stars. In the near future, a large sample of N-rich field stars found by CSST, combined with state-of-the-art N-body simulations will be crucial to deciphering GC-Galaxy co-evolution.

关键词： stars:chemically peculiar stars:abundances techniques:photometric techniques:spectroscopic

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Accelerating Asteroidal Period and Pole Inversion from Multiple Lightcurves Using Parallel Differential Evolution and Cellinoid Shape Model

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Research in Astronomy and Astrophysics 2024年第4期24卷 271-286页

作者： Yong-Xiong Zhang Wen-Xiu Guo Xiao-Ping Lu Hua Zheng Hai-Bin Zhao Jun Tian Wei-Lin Wang School of Engineering Guangzhou College of Technology and BusinessGuangzhou 510850China School of Computer Science and Engineering Macao University of Science and TechnologyTaipaMacao 999078China School of Mathematics and Statistics Shaoguan UniversityShaoguan 512099China State Key Laboratory of Lunar and Planetary Sciences Macao University of Science and TechnologyMacao 999078China Key Laboratory of Planetary Sciences Purple Mountain ObservatoryCASNanjing 210023China

Determining asteroid properties provides valuable physical insights but inverting them from photometric lightcurves remains computationally *** paper presents a new approach that combines a simplified Cellinoid shape model with the Parallel Differential Evolution(PDE)algorithm to accelerate *** PDE algorithm is more efficient than the Differential Evolution algorithm,achieving an extraordinary speedup of 37.983 with 64 workers on multicore *** PDE algorithm accurately derives period and pole values from simulated *** analysis of real asteroid lightcurves validates the method’s reliability:in comparison with results published elsewhere,the PDE algorithm accurately recovers the rotational periods and,given adequate viewing geometries,closely matches the pole *** PDE approach converges to solutions within 20,000 iterations and under one hour,demonstrating its potential for large-scale data *** work provides a promising new tool for unveiling asteroid physical properties by overcoming key computational bottlenecks.

关键词： methods:numerical minor planets asteroids:general techniques:photometric astrom

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photometric Analysis for Asteroid(81)Terpsichore using Convex Inversion and Phase Function Fitting Methods

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Research in Astronomy and Astrophysics 2024年第6期24卷 201-208页

作者： Ao Wang Xiaobin Wang Xiaoyun Xu Longhua Qin Quangui Gao Huaizhen Li Yong Xiao Hairu Zhao Department of Physics Yuxi Normal UniversityYuxi 653100China Yunnan Observatories Chinese Academy of SciencesKunming 650216China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of SciencesKunming 650216China University of Chinese Academy of Sciences Beijing 100049China

The shapes and rotation states(periods and pole orientations)of main-belt asteroids are important for understanding their formation and *** order to obtain sufficient photometric data covering different apparitions for asteroid(81)Terpsichore,ground-based photometric observations in 2020 and 2021 were carried *** combining published and newly obtained photometric data,we calculated the shape and spin parameters for(81)Terpsichore using the convex inversion *** this method,we have derived a best fitted pole orientation—(22.2±_(3.1)^(3.3°),17.5±_(5.5)^(10.8°))with a spin period of 10.94±_(0.01)^(0.01)*** on the derived convex shape of(81)Terpsichore,we have fitted the H,G+1,G_(2)phase function using the calibrated TESS data and Gaia data after accounting for the lightcurve amplitude *** a result,we have derived its absolute magnitude H=8.68±_(0.19)^(0.22)mag with corresponding phase function parameters G_(1)=0.82±_(0.10)^(0.09)and G_(2)=0.02±_(0.02)^(0.03).

关键词： asteroids:general minor planets asteroids:individual(Terpsichore) techniques:photometric

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The First Ground-based White Light Lunar Polarization Imaging:A New Kind of FeO Observation on the Near Side of the Moon

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Research in Astronomy and Astrophysics 2024年第6期24卷 1-6页

作者： Wei-Nan Wang Jin-Song Ping Ming-Yuan Wang Wen-Zhao Zhang Han-Lin Ye Xing-Wei Han Song-Feng Kou Changchun Observatory National Astronomical ObservatoriesChinese Academy of SciencesChangchun 130117China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China University of Chinese Academy of Sciences Beijing 101408China Astronomy Department Beijing Normal UniversityBeijing 100875China International Center for Climate and Environment Sciences Institute of Atmospheric PhysicsChinese Academy of SciencesBeijing 100029China Nanjing Institute of Astronomical Optics and Technology Chinese Academy of SciencesNanjing 210042China

Lunar optical polarization is a fascinating phenomenon that occurs when sunlight reflects off the surface of the Moon and becomes *** study employs a novel split-focus plane polarimetric camera to conduct the initial white light polarimetric observations on the near side of the *** obtained the linear degree of polarization(DOP)parameters of white light by observation from the eastern and western hemispheres of the *** findings indicate that the white light polarization is lower in the lunar highland than in the lunar maria *** the analysis of lunar soil samples,we noticed and determined that the DOP parameters of white light demonstrate high consistency with iron oxide on the *** study may serve as a new diagnostic tool for the Moon.

关键词： techniques:photometric polarization methods:observational Moon

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Candidate Eclipsing Binary Systems with aδScuti Star in Northern TESS Field

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Research in Astronomy and Astrophysics 2022年第8期22卷 34-48页

作者： F.Kahraman Aliçavuş D.Gümüş Ö.Kırmızıtaş Ö.Ekinci S.Çavuş Y.T.Kaya F.Aliçavuş Çanakkale Onsekiz Mart University Faculty of Sciences and ArtsPhysics Department17100ÇanakkaleTurkey Çanakkale Onsekiz Mart University Astrophysics Research Center and Ulupnar ObservatoryTR-17100ÇanakkaleTurkey Istanbul University Institute of Graduate Studies in ScienceProgramme of Astronomy and Space Sciences34116BeyazıtIstanbulTurkey Çanakkale Onsekiz Mart University School of Graduate StudiesDepartment of PhysicsTR-17100ÇanakkaleTurkey Çanakkale Onsekiz Mart University School of Graduate StudiesDepartment of Space Sciences and TechnologiesTR-17100ÇanakkaleTurkey Çanakkale Onsekiz Mart University Faculty of Engineering Computer EngineeringTR-17100ÇanakkaleTurkey

The existence of pulsating stars in eclipsing binaries has been known for *** types of objects are extremely valuable systems for astronomical studies as they exhibit both eclipse and pulsation *** eclipsing binaries are the only way to directly measure the mass and radius of stars with a good accuracy(≤1%),while the pulsations are a unique way to probe the stellar interior via oscillation *** are different types of pulsating stars existing in eclipsing *** of them is theδScuti ***,the known number ofδScuti stars in eclipsing binaries is around 90 according to the latest catalog of these *** increasing number of these kinds of variables is important to understand the stellar structure,evolution and the effect of binarity on the ***,in this study,we focus on discovering new eclipsing binaries withδScuti component(s).We searched within the northern Transiting Exoplanet Survey Satellite(TESS)field with a visual inspection by following some criteria such as light curve shape,the existence of pulsation like variations in the out-of-eclipse light curve and the T_(eff) values of the *** a result of these criteria,we discovered some *** orbital variations were first removed from the TESS light curves and frequency analysis was performed on the *** luminosity,and absolute and bolometric magnitudes of the targets were calculated as *** find how much of these parameters represent the primary(more luminous)binary component,we also computed the flux density ratio of the systems by utilizing the area of the *** addition,the positions of the systems in the H-R diagram were examined considering the flux density *** a consequence of the investigation,we defined 38 candidateδScuti stars and also one Maia variable in eclipsing binary systems.

关键词： (stars:)binaries:eclipsing stars:variables:delta Scuti techniques:photometric

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Analysis of TESS Field Eclipsing Binary Star V948 Her: A Pulsating or Non-pulsating Star?

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Research in Astronomy and Astrophysics 2022年第1期22卷 137-147页

作者： F Kahraman Alicavus O Ekinci Canakkde Onsekiz Mart University Faculty of Sciences and ArtsPhysics Department17100QanakkaleTurkey Canakkale Onsekiz Mart University Astrophysics Research Center and Ulupinar ObservatoryTR-17100CanakkaleTurkey Canakkale Onsekiz Mart University School of Graduate StudiesDepartment of Space Sciences and TechnologiesTR-17100CanakkaleTurkey

Pulsating stars occupy a significant place in the H-R diagram and it was thought that all stars inside the classical instability strip should pulsate. However, recent studies showed that there are many non-pulsating stars located inside the classical instability strip. The existence of these non-pulsating stars is still a mystery. To deeply understand the properties of these non-pulsating and pulsating stars, one needs precise fundamental stellar parameters(e.g. mass).For this purpose, the eclipsing binaries are unique systems. Hence, in this study, we present the TESS data analysis of one candidate pulsating eclipsing binary system, V948 Her. TESS data were used for the binary modeling with the literature radial velocity measurements, and the precise fundamental parameters of the system were obtained. The system’s age was derived as 1 ± 0.24 Gyr. The positions of the binary components in the H-R diagram were examined and the primary component was found inside the δ Scuti instability strip. However, in the frequency analysis of TESS data, we found no significant pulsation frequencies. Only the harmonics of the orbital periods were obtained in the analysis. Therefore, the system was classified as a non-pulsator. V948 Her is an important object to understand the nature of non-pulsating stars inside the δ Scuti instability strip.

关键词： (stars:)binaries:eclipsing stars:fundamental parameters techniques:photometric

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photometric and Spectroscopic Analysis of LBV Candidate J004341.84+411112.0 in M31

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Research in Astronomy and Astrophysics 2022年第1期22卷 237-244页

作者： A.Sarkisyan Sholukhova Fabrika A.Valeev A.Valcheva P.Nedialkov A.Tatamikov Special Astrophysical Observatory of Russian Academy of Sciences Niznij Arkhyz 369167Karachai-CherkessiaRussia Crimean Astrophysical Observatory Russian Academy of SciencesNauchnyi 298409Russia Department of Astronomy Sofia University5 J.Bourchier BlvdSofia 1164Bulgaria Sternberg Astronomical Institute Moscow M.V.Lomonosov State UniversityUniversitetskiy Prospekt 13Moscow 119234Russia

We study Luminous Blue Variable(LBV)candidate J004341.84+411112.0 in the Andromeda *** present optical spectra of the object obtained with the 6 m telescope of BTA SAO *** candidate shows typical LBV features in its spectra:broad and strong hydrogen lines and the He I lines with P Cygni *** remarkable spectral resemblance to the well known LBV P Cygni suggests a common nature of the objects and supports LBV classification of J004341.84+*** estimate the temperature,reddening,radius and luminosity of the star using its spectral energy *** bolometric luminosity of the candidate(M_(bol)=-10.41±0.12 mag)is quite similar to those of known LBV stars in the Andromeda *** analyzed a ten year light curve of the object in R *** candidate demonstrates photometric variations of the order of 0.4 mag,with an overall brightness increasing trendΔR>0.1 ***,the corresponding color variations of the object are fully consistent with LBV behavior when a star become cooler and brighter in the optical spectral range with a nearly constant bolometric ***-type variability of the object,similarity of its spectrum and estimated luminosity to those of known LBVs allow us to classify J004341.84+411112.0 as an LBV.

关键词： stars:early-type stars:massive stars:variables:S Doradus stars:Wolf Rayet techniques:photometric techniques:spectroscopic galaxies:individual(KIC 8098300)

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New Apsidal Motion in Four Eccentric Eclipsing Binaries:V610 Car,V944 Cep,V2815 Ori and V1260 Tau

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Research in Astronomy and Astrophysics 2022年第11期22卷 69-77页

作者： Ahmet Bulut Department of Physics Faculty of Arts and SciencesCanakkale Onsekiz Mart UniversityTerzioglu CampusTR-17020CanakkaleTurkiye Astrophysics Research Centre and Observatory Canakkale Onsekiz Mart UniversityTerzioglu CampusTR-17020CanakkaleTurkiye

This paper presents an apsidal motion *** apsidal motion analysis of the eccentric eclipsing binaries V610 Car(P=4.84 days),V944 Cep(P=6.56 days),V2815 Ori(P=2.13 days),and V1260 Tau(P=5.43 days)was performed using minima times from the O-C Gateway database,ASAS-3,ASAS-SN,and TESS,following Lacy’s *** rates of change of periastron longitude were found to be 0.0253±0.0041,0.0347±0.0015,0.0288±0.0010 and0.0294±0°.0079 cycle^(-1),*** the light curve study,the first photometric mass ratio of V944 Cep was found to be q=1.4994±0.0012.A new light curve of V944 Cep was obtained using TESS *** first absolute dimensions of V944 Cep were M_(1)=1.10±0.01 M_(⊙),M_(2)=1.64±0.02 M_(⊙),R_(1)=2.04±0.37 R_(⊙),R_(2)=3.77±0.67 R_(⊙)for the hotter primary component(T_(1)=4925 K),and M_(1)=1.04±0.01 M_(⊙),M_(2)=1.57±0.02 M_(⊙),R_(1)=2.26±0.36 R_(⊙),R_(2)=3.74±0.59 R_(⊙)for the cooler primary component(T_(1)=4475 K).For V610 Car,V944 Cep,V2815 Ori and V1260 Tau,the apsidal motion periods were found to be 188±26 yr,186±8 yr,73±3 yr and 182±38 yr,*** V944 Cep,the internal structural constants of the component stars log_(k2,obs)=-2.05±0.01 and log_(k2,theo)=-1.83 for hotter primary component and log_(k2,obs)=-1.97±0.01 and log_(k2,theo)=-1.89 for cooler primary component were calculated.

关键词： (stars:)binaries:eclipsing stars:fundamental parameters techniques:photometric

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LISC Catalog of Open ClustersⅢ.83 Newly Found Galactic Disk Open Clusters Using Gaia EDR3

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Research in Astronomy and Astrophysics 2023年第6期23卷 74-85页

作者：迟焕斌王锋李忠木 School of Management and Economics Kunming University of Science and TechnologyKunming 650031China Center for Astrophysics Guangzhou UniversityGuangzhou 510006China Peng Cheng Laboratory Shenzhen 518000China Institute of Astronomy Dali UniversityDali 671003China

As groups of coeval stars born from the same molecular cloud,an open cluster(OC)is an ideal laboratory for studying the structure and dynamical evolution of the Milky *** release of high-precision Gaia Early Data Release 3(Gaia EDR3)and modern machine-learning methods offer unprecedented opportunities to identify *** this study,we extended conventional HDBSCAN(e-HDBSCAN)for searching for new OCs in Gaia EDR3.A pipeline was developed based on the parallel computing technique to blindly search for OCs from Gaia EDR3within Galactic latitudes∣b∣<25°.As a result,we obtained 3787 star clusters,of which 83 new OCs were reported after cross-match and visual *** the same time,the main star cluster parameters are estimated by color-magnitude diagram *** study significantly increases the sample size and physical parameters of OCs in the catalog of *** shows the incompleteness of the census of OCs across our Galaxy.

关键词： techniques:photometric galaxies:star clusters:individual(... ...) galaxies:star clusters:general

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Modified Masses and Parallaxes of Close Binary Systems: HD 39438

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Research in Astronomy and Astrophysics 2023年第11期23卷 31-37页

作者： Suhail Masda ZTYousef Mashhoor Al-Wardat Awni Al-Khasawneh Department of Physics Mahrah UniversityMahrahYemen Department of Physics Hadhramout UniversityMukallaYemen Department of Applied Physics Faculty of Science and TechnologyUniversiti Kebangsaan Malaysia43600 UKM BangiSelangorMalaysia Department of Applied Physics and Astronomy and Sharjah Academy for AstronomySpace Sciences and TechnologyUniversity of SharjahP.O.Box 27272 SharjahUnited Arab Emirates Department of Physics Al al-Bayt UniversityMafraq 25113Jordan

We present the detailed fundamental stellar parameters of the close visual binary system HD 39438 for the first time. We used Al-Wardat's method for analyzing binary and multiple stellar systems. The method implements Kurucz's plane parallel model atmospheres to construct synthetic spectral energy distributions(SEDs) for both components of the system. It then combines the results of the spectroscopic analysis with the photometric analysis and compares them with the observed ones to construct the best synthetic SED for the combined system. The analysis gives the precise fundamental parameters of the individual components of the system. Based on the positions of the components of HD 39438 on the H-R diagram, and evolutionary and isochrone tracks, we found that the system belongs to the main sequence stars with masses of 1.24 and 0.98 solar masses for the components A and B, respectively, and age of 1.995 Gyr for both components. The main result of HD 39438 is new dynamical parallax, which is estimated to be 16.689 ± 0.03 mas.

关键词： methods:analytical techniques:photometric (stars:)binaries:visual techniques:spectroscopic

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