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Precise Evolutionary Asteroseismology of High-AmplitudeδScuti Star AE Ursae Majoris

Research in Astronomy and Astrophysics 2022年第10期22卷 61-76页

作者： Hui-Fang Xue Jia-Shu Niu jian-ning fu Department of Physics Taiyuan Normal UniversityJinzhong 030619China Institute of Computational and Applied Physics Taiyuan Normal UniversityJinzhong 030619China Institute of Theoretical Physics Shanxi UniversityTaiyuan 030006China State Key Laboratory of Quantum Optics and Quantum Optics Devices Shanxi UniversityTaiyuan 030006China Department of Astronomy Beijing Normal UniversityBeijing 100875China

Stellar structure and evolution theory is one of the bases in modern *** inner structures and their evolutionary states can be precisely tested by asteroseismology,since the inner information is brought to the stellar surface by the global oscillating waves and becomes *** stellar evolutionary speed(i.e.,how long timescale does a star stay at a special evolution phase?),because of the insurmountable gap between the timescales of the evolutionary history of human civilization and a star,it can only be roughly tested by ensemble of stars in different evolutionary stages in most cases,and all the snapshots of these stars make up our global view of stellar *** effect of stellar evolution on the structure and the corresponding global size of a pulsating star will lead to tiny period variations of its pulsation modes,which are the most valuable indicators of its evolutionary state and can be used to test the stellar evolution theory by a single star rather than ensemble of ***,we report a High-AmplitudeδScuti star AE Ursae Majoris,which is located in the post main-sequence(MS)evolutionary stage and its observed linear period variation rate can be practically ascribed to its evolutionary *** result tests the stellar evolution theory from the pre-MS to post-MS with an unprecedented precision by a single star,and the framework can be extended to other type of pulsating stars to perform precise evolutionary asteroseismology,which aims to test the current stellar evolution theory in different evolutionary stages,discover the discrepancies between the theory and observations,and ultimately build a complete and precise stellar evolution theory to backtrack the history of each of these stars.

关键词： stars variables delta Scuti-stars evolution-stars oscillations(including pulsations)

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Pulsation analysis of the high amplitude δ Scuti star CW Serpentis

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Research in Astronomy and Astrophysics 2013年第10期13卷 1181-1188页

作者： Jia-Shu Niu jian-ning fu Wei-Kai Zong Department of Astronomy Beijing Normal University

Time-series photometric observations were made for the high amplitudeδScuti star CW Ser between 2011 and 2012 at the Xinglong Station of National Astronomical Observatories,Chinese Academy of *** performing the frequency analysis of the light curves,we confirmed the fundamental frequency of f=5.28677 c d 1,together with seven harmonics of the fundamental frequency,which are newly *** additional frequencies were *** O C diagram,produced with the 21 newly determined times of maximum light combined with those provided in the literature,helps to obtain a new ephemeris formula of the times of maximum light with the pulsation period of 0.189150355±0.000000003 d.

关键词： stars:variables:δ Scuti stars:individual(CW Ser) techniques:photometric

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Spot and Facula Activity Variations of the Eccentric Detached Eclipsing Binary KIC 8098300 Based on the Time-series Orbital Solutions

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Research in Astronomy and Astrophysics 2022年第1期22卷 174-188页

作者： Hu-Biao Niu jian-ning fu Jia-Xin Wang Chun-Qian Li Department of Astronomy Beijing Normal UniversityBeijing 100875China Xinjiang Astronomical Observatory Chinese Academy of SciencesUrumqi 830011China Key Laboratory of Optical Astronomy National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China School of Astronomy and Space Science University of Chinese Academy of SciencesBeijing 100049China

The LAMOST spectra and Kepler light curves are combined to investigate the detached eclipsing binary KIC 8098300,which shows the O’Connell effect caused by spot/facula *** radial velocity(RV)measurements are derived by using the tomographic spectra disentangling *** mass ratio q=K1/K2=0.812±0.007,and the orbital semimajor axis a sin i=14.984±0.048 R_(⊙)are obtained by fitting the RV *** optimize the binary model concerning the spot/facula activity with the code PHOEBE and obtain precise parameters of the orbit including the eccentricity e=0.0217±0.0008,the inclination i=87°.71±0°.04,and the angle of periastronω=284°.1±0°.*** masses and radii of the primary and secondary star are determined as M_(1)=1.3467±0.0001 M_(⊙),R_(1)=1.569±0.003 R_(⊙),and M_(2)=1.0940±0.0001 M_(⊙),R_(2)=1.078±0.002 R_(⊙),*** ratio of temperatures of the two component stars is r_(teff)=0.924±*** also obtain the periastron precession speed of 0.000024±0.000001 day *** residuals of out-of-eclipse are analyzed using the auto-correlation function and the discrete Fourier *** spot/facula activity is relatively weaker,but the lifetime is longer than that of most single main sequence stars in the same temperature *** average rotation period of the spots P_(rot)=4.32 days is slightly longer than the orbital period,which may be caused by either the migration of spots/faculae along the longitude or the latitudinal differential *** activity may be spot-dominated for the secondary star and facula-dominated for the primary *** method of this work can be used to analyze more eclipsing binaries with the O’Connell effect in the Kepler field to obtain the precise parameters and investigate the difference of spot behavior between binaries and single *** is helpful for a deeper understanding of the stellar magnetic activity and dynamo theory.

关键词： (stars:)binaries:eclipsing (stars:)starspots stars:individual(KIC 8098300)

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Variability Study of the SX Phoenicis Star BL Camelopardalis

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Chinese Journal of Astronomy and Astrophysics 2008年第2期8卷 237-244页

作者： jian-ning fu Chao Zhang Kanokwan Marak Chayan Boonyarak PongsakKhokhuntod Shi-Yang jiang Department of Astronomy Beijing Normal University Beijing 100875 Faculty of Science Naresuan University Phitsanulok 65000 Thailand National Astronomical Observatories Chinese Academy of Sciences Beijing 100012

New time-series photometric observations of BL Cam in the V band and white light were made during 2005 to 2007 at the Xinglong Station of China. The frequency analysis confirms two closely separated frequencies, 25.181 d^-1 and 25.571 d^-1, but the frequency of 31-32 d^- 1 reported in the literature was not detected in the new data. New times of maximum light were determined from both our light curves and those available on Internet, allowing a more comprehensive study of the O - C diagram, together with the times of maximum light in the literature. A new interpretation, including the period increasing before 1988 and decreasing since 1992 of BL Cam and the light-time effect in a binary system, looks plausible.

关键词： techniques: photometric -- stars: variables: delta Scuff -- stars: individual: BL Cam

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The Physical Properties and Starspot Activity of the Triple System KIC 6525196

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Research in Astronomy and Astrophysics 2022年第7期22卷 214-223页

作者： Yang Pan jian-ning fu Xiao-Bin Zhang Jia-Xin Wang Chun-Qian Li School of Physics and Astronomy China West Normal UniversityNanchong 637002China Department of Astronomy Beijing Normal UniversityBeijing 100875China Key Laboratory of Optical Astronomy National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100012China School of Science Chongqing University of Posts and TelecommunicationsChongqing 400065China School of Astronomy and Space Science University of Chinese Academy of SciencesBeijing 100049China

We present the results of photometric and spectroscopic analyses for the triple-lined system KIC 6525196,an eclipsing binary accompanied by a third *** modeling the Kepler light curves and radial velocities from LAMOST and HIDES observations,absolute parameters of the system are *** components of the eclipsing binary are found to be solar-like stars with masses and radii of M= 1.0286 ± 0.0026 M,R= 1.127 ± 0.008 *** M=0.9667 ± 0.0024 M,R=0.963 ± 0.007 *** mass of the third star is determined to be M= 0.772 ± 0.010 *** the out-of-eclipse light residuals,we measure rotation period and decay timescale of an active region by using the autocorrelation *** comparison to the Sun,the activity level of the system is significantly *** addition,a possible short photometric activity cycle of~244 days is detected.

关键词： stars:activity (stars:)binaries:eclipsing (stars:)binaries:spectroscopic

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Pulsation and Long-Term Variability of the High-Amplitude δ Scuti Star AD Canis Minoris

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Chinese Journal of Astronomy and Astrophysics 2007年第3期7卷 421-427页

作者： Pongsak Kholkhuntod jian-ning fu Chayan Boonyarak Kanokwan Marak Li Chen Shi-Yang jiang Faculty of Science Naresuan University Phitsanulok 65000 Thailand Department of Astronomy Beijing Normal University Beijing 100875 National Astronomical Observatories Chinese Academy of Sciences Beijing 100012

Time-series photometry was made for the large-amplitude δ Scuff star AD CMi in 2005 and 2006. High-quality photometric data provided in the literature were used to analyze the pulsation of the star, with the derived multiple frequencies fitted to our new data. Besides the dominant frequency and its harmonics, one low frequency （2.27402 c d^-1） is discovered, which provides a reasonable interpretation for the long-noticed luminosity variation at the maximum and minimum light. Combining the nine new times of light maxima determined from the new data with the 64 times collected from the literature, we analyzed the long-term variability of AD CMi with the O - C technique. The results provide the updated value of period of 0.122974478 days, and seem to be in favor of the model of combination of the evolutionary effect and light-time effect of a binary system, of which some parameters are hereby deduced.

关键词： techniques photometric - stars variables δ Scuti - stars individual ADCMi

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A triplet of the only pulsation mode detected in the DAV star G132–12

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Research in Astronomy and Astrophysics 2021年第6期21卷 276-280页

作者： Wen-Chao Su jian-ning fu jian-Xing Chen Lester Fox-Machado Shi-Jie Zhao Carmen Ayala-Loera jiang-Tao Wang Yang Pan Department of Astronomy Beijing Normal UniversityBeijing 100012China Dipartimento di Fisica e Astronomia Alma Mater Studiorum Universita’di Bolognavia Piero Gobetti 93/21-40129 BolognaItaly INAF-Osservatorio di Astrofisica e Scienze dello Spazio di Bologna Via Piero Gobetti 93/31-40129 BolognaItaly Instituto de Astronomia Universidad Nacional Autonoma de MexicoApartado Postal 87722800 EnsenadaBaja CaliforniaMexico Institute of Astronomy&Astrophysics Academia SinicaTaipeiChina

Hydrogen atmosphere pulsating white dwarfs,also known as DAV stars,are the most abundant type of pulsating white ***-temperature DAV stars in general exhibit a small number of pulsation modes and stable frequencies.G132-12 is one of the pulsating hydrogen atmosphere white dwarf stars which lies close to the blue edge of the instability *** researches reported that G132-12 might have only one pulsation mode with the period of 212.69 *** study the pulsation properties of G132-12 in detail,we carried out a bi-site observation campaign in October *** series photometric data were collected during around 154 h in total.A Fourier analysis reveals three frequencies which are identified as the triplet of an l=1 g-mode pulsation with the period of 212.499 *** rotational period is derived as Prot=35.0±6.7 h and the inclination of the rotational axis to the line of sight is 70°.G132-12 could be an ideal target for measuring the cooling scale of this white dwarf star with only one excited pulsation mode detected.

关键词： white dwarfs oscillations photometric

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Pulsations of the High-Amplitude δ Scuti star YZ Bootis

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Research in Astronomy and Astrophysics 2018年第1期18卷 11-20页

作者： Tao-Zhi Yang Ali Esamdin jian-ning fu Hu-Biao Niu Guo-Jie Feng Fang-Fang Song Jin-Zhong Liu Lu Ma Xinjiang Astronomical Observatory Chinese Academy of Sciences Urumqi 830011 China University of Chinese Academy of Sciences Beijing 100049 China Department of Astronomy Beijing Normal University Beijing 100875 China

We present a study on pulsations of the high-amplitudeδScuti star YZ Boo based on photometric observations in Johnson V and R bands with both the Nanshan 1-m telescope of Xinjiang Astronomical Observatory（XAO）and the Xinglong 85-cm telescope of National Astronomical Observatories,Chinese Academy of Sciences（NAOC）.Fourier analysis of the light curves reveals the fundamental radial mode and its five harmonics,with the fourth and fifth being newly *** new times of maximum light are determined from the light curves,and combined with those in the literature,we construct the O-C diagram,derive a new ephemeris and determine a new value for the updated period of 0.104091579（2）.In addition,the O-C diagram reveals an increasing rate of period change for YZ *** models are calculated and constrained with the observationally determined parameters of YZ *** mass and age of YZ Boo are hence derived as M=1.61±0.05 M_⊙ and age=（1.44±0.14）×10~9 yr,*** both the frequency of the fundamental radial mode and the rate of period change,YZ Boo is located at the post main sequence stage.

关键词： stars:variables:δ Scuti star stars:individual(YZ Boo) stars:oscillations

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Overview of the LAMOST-Kepler project

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Research in Astronomy and Astrophysics 2020年第10期20卷 343-352页

作者： jian-ning fu Peter De Cat Weikai Zong Antonio Frasca Richard O.Gray An-Bin Ren Joanna Molenda-Zakowicz Christopher J.Corbally Giovanni Catanzaro jian-Rong Shi A-Li Luo Hao-Tong Zhang Department of Astronomy Beijing Normal UniversityBeijing 100875China Royal Observatory of Belgium Ringlaan 3B-1180 BrusselBelgium INAF-Osservatorio Astrofisico di Catania Via S.Sofia 781-95123 CataniaItaly Department of Physics and Astronomy Appalachian State UniversityBooneNC 28608USA Department of Astronomy China West Normal UniversityNanchong 637002China Astronomical Institute of the University of Wroclaw ul.Kopernika 1151-622 WroclawPoland Vatican Observatory Research Group University of ArizonaTucsonAZ 85721-0065USA Key Lab for Optical Astronomy National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China

The NASA Kepler mission obtained long-term high-quality photometric observations for a large number of stars in its original field of view from 2009 to *** provide reliable stellar parameters in a homogeneous way,the LAMOST telescope began to carry out low-resolution spectroscopic observations for as many stars as possible in the Kepler field in *** June 2018,238386 low-resolution spectra with SNRg≥6 had been collected for 155623 stars in the Kepler field,enabling the determination of atmospheric parameters and radial velocities,as well as spectral classification of the target *** information has been used by astronomers to carry out research in various fields,including stellar pulsations and asteroseismology,exoplanets,stellar magnetic activity and flares,peculiar stars and the Milky Way,binary stars,*** summarize the research progress in these fields where the usage of data from the LAMOST-Kepler(LK)project has played a *** addition,time-domain medium-resolution spectroscopic observations have been carried out for about 12000 stars in four central plates of the Kepler field since *** currently available results show that the LAMOST-Kepler medium resolution(LKMRS)observations provide qualified data suitable for research in additional science projects including binaries,high-amplitude pulsating stars,*** LAMOST is continuing to collect both low-and mediumresolution spectra of stars in the Kepler field,we expect more data to be released continuously and new scientific results to appear based on the LK project data.

关键词： astronomical database:miscellaneous technique:spectroscopy stars:general stars:statistics

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Upgraded photometric system on the 85-cm telescope at Xinglong station

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Research in Astronomy and Astrophysics 2018年第9期18卷 21-30页

作者： Chun-Hai Bai jian-ning fu Tao-Ran Li Zhou Fan jiang-Hua Wu Yong Zhao Xian-Qun Zeng Wen-Zhao Zhang Peng Qiu Guo-Jie Feng Xiao-Jun jiang National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China University of Chinese Academy of Sciences Beijing 100049China Xinjiang Astronomical Observatory Chinese Academy of SciencesUrumqi 830011China Department of Astronomy Beijing Normal UniversityBeijing 100875China

The 85-cm telescope at Xinglong station is a prime focus system that operates well with high science outputs. The telescope has been upgraded since 2014 with a new corrector, and new filters and camera, which are provided by Beijing Normal University. The filter set is the Johnson-Cousins UBV RI system. We report the test results of the new system including bias, dark current, linearity, gain and readout noise of the CCD camera. Then we derive accurate instrumental calibration coefficients in UBV RI bands with Landolt standard stars during photometric nights. Finally, we give the limiting magnitudes with various exposure times and signal-to-noise ratios for observers as references.

关键词： telescope instrumentation CCD photometry

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