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天文和天体物理学研究
天文和天体物理学研究

汪景琇 景益鹏

月刊

1674-4527

wenyy@bao.ac.cn

010-64853746

100717

北京朝阳区大屯路甲20号国家天文台 RAA编辑部

天文和天体物理学研究/Journal Research in Astronomy and AstrophysicsCSCD北大核心CSTPCDSCI
查看更多>>本刊1981年创刊至2000年已出版20卷。创刊时为中文期刊，2001年改为《中国天文和天体物理学报》（英文版）。主要刊登天文学和天体物理学领域的原创性研究论文。主要栏目和报道范围：“研究快报”用来报道天文观测的新结果及新理论；“特约综述”聘请国际知名天文学家就某些热点问题进行专题评述。“研究论文”具有原创性。2009年更名为《天文和天体物理学研究》（英文版），由双月刊变为月刊。
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    Probing the Kinematic Signatures of Planet Formation in the Gas Disk of MWC 480

    Min ZhaoHaochuan YuZhengxiang Li
    110-118页
    查看更多>>摘要：The disk around MWC 480 has shown multiple substructures in both dust and gas observations,possibly suggesting ongoing planet formation in situ.In this paper,we explore the gas kinematics of the MWC 480 disk by analyzing the archival Atacama Large Millimeter/submillimeter Array observations of 12CO(J=2-1),13CO(J=2-1),and C18O(J=2-1).By modeling the line-of-sight velocities,inferred from the Doppler shifts of the emission lines,we are able to decompose the three-dimensional(3D)velocity field of the disk into rotational,radial,and vertical components.Further analysis reveals the presence of large-scale gas flows in the(r,z)plane.Notably,we identify potential meridional flows across various heights as traced by all three CO isotopologues in the 80-120 au region,possibly associated with ongoing planet formation activities in this region.Moreover,we find upward flows near 200 au for all three CO isotopologues,which may point to the presence of disk winds.
      原文链接:
    • 万方数据
    • 维普

    The ALMA-QUARKS Survey.Ⅱ.The ACA 1.3 mm Continuum Source Catalog and the Assembly of Dense Gas in Massive Star-Forming Clumps

    许峰玮Ke WangTie LiuLei Zhu...
    119-139页
    查看更多>>摘要：Leveraging the high resolution,sensitivity,and wide frequency coverage of the Atacama Large Millimeter/submillimeter Array(ALMA),the QUARKS survey,standing for"Querying Underlying mechanisms of massive star formation with ALMA-Resolved gas Kinematics and Structures",is observing 139 massive star-forming clumps at ALMA Band 6(λ～1.3 mm).This paper introduces the Atacama Compact Array(ACA)7 m data of the QUARKS survey,describing the ACA observations and data reduction.Combining multi-wavelength data,we provide the first edition of QUARKS atlas,offering insights into the multiscale and multiphase interstellar medium in high-mass star formation.The ACA 1.3 mm catalog includes 207 continuum sources that are called ACA sources.Their gas kinetic temperatures are estimated using three formaldehyde transitions with a non-LTE radiation transfer model,and the mass and density are derived from a dust emission model.The ACA sources are massive(16-84 percentile values of 6-160 M⊙),gravity-dominated(M∝R11)fragments within massive clumps,with supersonic turbulence(M＞1)and embedded star-forming protoclusters.We find a linear correlation between the masses of the fragments and the massive clumps,with a ratio of 6％between the two.When considering fragments as representative of dense gas,the ratio indicates a dense gas fraction(DGF)of 6％,although with a wide scatter ranging from 1％to 10％.If we consider the QUARKS massive clumps to be what is observed at various scales,then the size-independent DGF indicates a self-similar fragmentation or collapsing mode in protocluster formation.With the ACA data over four orders of magnitude of luminosity-to-mass ratio(L/M),we find that the DGF increases significantly with L/M,which indicates clump evolutionary stage.We observed a limited fragmentation at the subclump scale,which can be explained by a dynamic global collapse process.
      原文链接:
    • 万方数据

    Astronomical Knowledge Entity Extraction in Astrophysics Journal Articles via Large Language Models

    Wujun ShaoRui ZhangPengli JiDongwei Fan...
    140-155页
    查看更多>>摘要：Astronomical knowledge entities,such as celestial object identifiers,are crucial for literature retrieval and knowledge graph construction,and other research and applications in the field of astronomy.Traditional methods of extracting knowledge entities from texts face numerous challenging obstacles that are difficult to overcome.Consequently,there is a pressing need for improved methods to efficiently extract them.This study explores the potential of pre-trained Large Language Models(LLMs)to perform astronomical knowledge entity extraction(KEE)task from astrophysical journal articles using prompts.We propose a prompting strategy called Prompt-KEE,which includes five prompt elements,and design eight combination prompts based on them.We select four representative LLMs(Llama-2-70B,GPT-3.5,GPT-4,and Claude 2)and attempt to extract the most typical astronomical knowledge entities,celestial object identifiers and telescope names,from astronomical journal articles using these eight combination prompts.To accommodate their token limitations,we construct two data sets:the full texts and paragraph collections of 30 articles.Leveraging the eight prompts,we test on full texts with GPT-4 and Claude 2,on paragraph collections with all LLMs.The experimental results demonstrate that pre-trained LLMs show significant potential in performing KEE tasks,but their performance varies on the two data sets.Furthermore,we analyze some important factors that influence the performance of LLMs in entity extraction and provide insights for future KEE tasks in astrophysical articles using LLMs.Finally,compared to other methods of KEE,LLMs exhibit strong competitiveness in multiple aspects.
      原文链接:
    • 万方数据
    • 维普

    Probing the Gamma-Ray Emission Region of Five TeV Flat Spectrum Radio Quasars

    Hu-Bing XiaoHai-Tao CaoRui XueJin-Ting Cai...
    156-169页
    查看更多>>摘要：The location of γ-ray emission of blazars remains a contested topic,inspiring the development of numerous investigative techniques to address this issue.In this work,we analyzed Fermi γ-ray light curves in the GeV and MeV bands,employing the discrete cross-correlation function method to discern time lags between the two bands.For 4C+21.35,Ton 599,B2 1420+32,and PKS 1510-089,we identified a time lag spanning several days,while for PKS 1441+25,the time lag was not statistically found.The results imply that the soft photons necessary for inverse Compton scattering predominantly originate from the dusty torus in the first four sources,whereas for PKS 1441+25,they seem to be sourced mainly from the broad-line region.Further analysis of the opacity(τγγ)and the GeV spectra study supports the conclusion that the location of the dissipation region must be beyond the BLR to avoid significant absorption.Notably,for PKS 1441+25,the emission region is also posited to lie outside yet proximate to the BLR.The parameters of describing the emission region were obtained by fitting broadband spectral energy distribution with contemporaneous observation data.Our findings suggest that for the five TeV FSRQs,during TeV flaring events,the jet appears to maintain an equilibrium between the energy density of the magnetic field and that of the particles for all investigated sources,with the exceptions of 4C+21.35 and PKS 1441+25.In terms of the overall jet power,particle energy is the dominant contributor,and the observed blazar radiation cannot be solely attributed to the magnetic field,except in the case of 4C+21.35.Consequently,magnetic reconnection is unlikely to be the primary mechanism behind particle acceleration in these systems.
      原文链接:
    • 万方数据
    • 维普

    Isochrone Fitting of Galactic Globular Clusters—Ⅵ.High-latitude Clusters NGC 5024(M53),NGC 5053,NGC 5272(M3),NGC 5466,and NGC 7099(M30)

    G.A.GontcharovS.S.SavchenkoA.A.MarchukC.J.Bonatto...
    170-190页
    查看更多>>摘要：We fit various color-magnitude diagrams(CMDs)of the high-latitude Galactic globular clusters NGC 5024(M53),NGC 5053,NGC 5272(M3),NGC 5466,and NGC 7099(M30)by isochrones from the Dartmouth Stellar Evolution Database and Bag of Stellar Tracks and Isochrones for α-enrichment[α/Fe]=+0.4.For the CMDs,we use data sets from Hubble Space Telescope,Gaia,and other sources utilizing,at least,25 photometric filters for each cluster.We obtain the following characteristics with their statistical uncertainties for NGC 5024,NGC 5053,NGC 5272,NGC 5466,and NGC 7099,respectively:metallicities[Fe/H]=-1.93±0.02,-2.08±0.03,-1.60±0.02,-1.95±0.02,and-2.07±0.04 dex with their systematic uncertainty 0.1 dex;ages 13.00±0.11,12.70±0.11,11.63±0.07,12.15±0.11,and 12.80±0.17 Gyr with their systematic uncertainty 0.8 Gyr;distances(systematic uncertainty added)18.22±0.06±0.60,16.99±0.06±0.56,10.08±0.04±0.33,15.59±0.03±0.51,and 8.29±0.03±0.27 kpc;reddenings E(B-V)=0.023±0.004,0.017±0.004,0.023±0.004,0.023±0.003,and 0.045±0.002 mag with their systematic uncertainty 0.01 mag;extinctions Av=0.08±0.01,0.06±0.01,0.08±0.01,0.08±0.01,and 0.16±0.01 mag with their systematic uncertainty 0.03 mag,which suggest the total Galactic extinction Av=0.08 across the whole Galactic dust to extragalactic objects at the North Galactic Pole.The horizontal branch morphology difference of these clusters is explained by their different metallicity,age,mass-loss efficiency,and loss of low-mass members in the evolution of the core-collapse cluster NGC 7099 and loose clusters NGC 5053 and NGC 5466.
      原文链接:
    • 万方数据

    A Possible X-ray Quasi-periodic Oscillation in the Narrow-line Seyfert 1 Galaxy Mrk 142

    Xiao-Gu ZhongJian-Cheng WangYong-Yun ChenXiao-Ling Yu...
    191-200页
    查看更多>>摘要：A possible quasi-periodic oscillation(QPO)at frequency 7.045 x 10-5 Hz is found in the narrow-line Seyfert 1 galaxy Mrk 142 in the data of XMM-Newton collected on 2020 April 11.We find that the QPO signal is statistically significantly larger than the 5σ level and highly coherent with quality factor Q＞5 at the 0.3-10 keV band by using the method of the Lomb-Scargle Periodogram,the Weighted Wavelet Z-transform and the REDFIT.We analyze the data in 0.3-0.6keV,0.6-1 keV,1-3 keV and 3-10 keV energy bands,and find obvious QPO signals at 0.3-0.6 keV and 1-3 keV bands.We then analyze the time-average spectra and time variability at the QPO frequency of 7.045 x 10-5 Hz,and use a model to fit them.We find that the QPO signal mainly comes from the X-ray hot corona.
      原文链接:
    • 万方数据
    • 维普

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

    Ao WangXiaobin WangXiaoyun XuLonghua Qin...
    201-208页
    查看更多>>摘要：The shapes and rotation states(periods and pole orientations)of main-belt asteroids are important for understanding their formation and evolution.In order to obtain sufficient photometric data covering different apparitions for asteroid(81)Terpsichore,ground-based photometric observations in 2020 and 2021 were carried out.By combining published and newly obtained photometric data,we calculated the shape and spin parameters for(81)Terpsichore using the convex inversion method.With this method,we have derived a best fitted pole orientation—(22.2±33.3°3.1,17.5±10.8°5.5)with a spin period of 10.94±0.010.01 h.Based on the derived convex shape of(81)Terpsichore,we have fitted the H,G1,G2 phase function using the calibrated TESS data and Gaia data after accounting for the lightcurve amplitude correction.As a result,we have derived its absolute magnitude H=8.68±0.220.19 mag with corresponding phase function parameters G1=0.82±0.090.10 and G2=0.02±0.030.002.
      原文链接:
    • 万方数据
    • 维普

    Timing and Spectral Analysis of the Black Hole X-Ray Binary MAXI J1803-298 with Insight-HXMT Data

    Ying-Chen XuJin-Lu QuM.MéndezRui-Can Ma...
    209-224页
    查看更多>>摘要：We present a comprehensive analysis of the 2021 Outburst of MAXI J1803-298 utilizing observations of the Insight-Hard X-ray Modulation Telescope(Insight-HXMT)spanning from the low hard state to the high soft state.Within the Insight-HXMT data set,compared to the previous work,we identify a more prolonged presence of type-C quasi-periodic oscillations(QPOs)with centroid frequencies ranging from～0.16 to 6.3 Hz,which present correlations with the hardness ratio and the photon index of the Comptonized component.For QPO frequencies less than～2 Hz,the QPO phase lags are hard(photons of 10-19 keV arrive later than those of 1-4 keV),while at higher frequencies,the lags become soft at and above～4 Hz.Furthermore,the spectra in all Insight-HXMT observations consist of a multi-color blackbody component and a Comptonized component,as commonly observed in classical black hole X-ray binaries.We analyze state transitions and the evolution of accretion geometry in this work.The fitted inner disk radius increases abnormally during the low hard state,hypothesized to result from the corona condensing onto the inner disk.Additionally,two significant drops in flux are observed during the soft intermediate state,maybe implying changes in the corona/jet and the disk,respectively.
      原文链接:
    • 万方数据
    • 维普

    Temporal and Spectral Characteristics of Persistent Emission and Special Bursts of Magnetar SGR J1935+2154 Based on Insight-HXMT

    Xue-Feng LuLi-Ming SongMing-Yu GeShuang-Nan Zhang...
    225-233页
    查看更多>>摘要：In October 2022,the magnetar SGR J1935+2154 entered the active outburst state.During the episode,the Insight-HXMT satellite carried out a long observation that lasted for 20 days.More than 300 bursts were detected,and a certain amount of persistent radiation signals were also accumulated.This paper mainly introduces the results of persistent radiation profile folding and period search based on Insight-HXMT data.At the same time,the burst phase distribution characteristics,spectral lag results of burst,the spectral characteristics of zero-lag bursts and the time-resolved spectral evolution characteristics of high-flux bursts are reported.We found that there is no significant delay feature during different energy bands for the bursts of SGR J1935+2154.The observed zero-lag burst does not have a unique spectrum.The time-resolved spectrum of the individual burst has consistent spectral types and spectral parameters at different time periods of the burst.We also find that the burst number phase distribution and the burst photon phase distribution have the same tendency to concentrate in specific regions of the persistent emission profile.
      原文链接:
    • 万方数据
    • 维普

    Feedback of Efficient Shock Acceleration on Magnetic-field Structure Inside Young Type Ia Supernova Remnants

    Jun-Yu ShenBi-Wen BaoLi Zhang
    234-244页
    查看更多>>摘要：Using an effective adiabatic index γeff to mimic the feedback of efficient shock acceleration,we simulate the temporal evolution of a young type Ia supemova remnant(SNR)with two different background magnetic field(BMF)topologies:a uniform and a turbulent BMF.The density distribution and magnetic-field characteristics of our benchmark SNR are studied with two-dimensional cylindrical magnetohydrodynamic simulations.When γeff is considered,we find that:(1)the two-shock structure shrinks and the downstream magnetic-field orientation is dominated by the Rayleigh-Taylor instability structures;(2)there exists more quasi-radial magnetic fields inside the shocked region;and(3)inside the intershock region,both the quasi-radial magnetic energy density and the total magnetic energy density are enhanced:in the radial direction,with γeff=1.1,they are amplified about 10-26 times more than those with γeff=5/3.While in the angular direction,the total magnetic energy densities could be amplified about 350 times more than those with γeff=5/3,and there are more grid cells within the intershock region where the magnetic energy density is amplified by a factor greater than 100.
      原文链接:
    • 万方数据
    • 维普