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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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    Fermi Blazars in the Zwicky Transient Facility Survey:Properties of Large Optical Variations

    Si-Si SunZhong-Xiang WangShun-Hao Ji
    104-115页
    查看更多>>摘要：We analyze the optical light curve data,obtained with the Zwicky Transient Facility(ZTF)survey,for 47 γ-ray blazars monitored by the Large Area Telescope onboard the Fermi Gamma-ray Space Telescope(Fermi).These 47 sources are selected because they are among the Fermi blazars with the largest optical variations in the ZTF data.Two color-magnitude variation patterns are seen in them,with one being redder-to-stable-when-brighter(RSWB;in 31 sources)and the other being stable when brighter(in 16 sources).The patterns fit with the results recently reported in several similar studies with different data.Moreover,we find that the colors in the stable state of the sources share similar values,for which(after being corrected for the Galactic extinction)most sources are in a range of 0.4-0.55.This feature could be intrinsic and may be applied in,for example,study of the intragalactic medium.We also determine the turning points for the sources showing the RSWB pattern,after which the color changes saturate and become stable.We find a correlation between optical fluxes and γ-ray fluxes at the turning points.The physical implications of the correlation remain to be investigated,probably better with a sample of high-quality γ-ray flux measurements.
      原文链接:
    • 万方数据
    • 维普

    The Impact of Nova Outbursts on the Chemical Abundance of the Interstellar Medium

    Guoli HeChunhua ZhuGuoliang LüLin Li...
    116-129页
    查看更多>>摘要：Nova outbursts are the results of thermonuclear runaways,which occur when sufficient material accretes on the surfaces of white dwarfs(WDs).Using the MESA code,we construct a detailed grid for carbon-oxygen and oxygen-neon-magnesium novae.By employing population synthesis methods,we conduct a statistical analysis of the distribution of novae in the Milky Way.In our models,on average,a typical nova system may undergo about 8000 eruptions and the Galactic nova rate is ∼130 yr-1.The C,N,and O elements in nova ejecta are strongly affected by the mixing degree between WD core and accreted material.Our results show that the average value of 12C/13C in nova ejecta is about an order of magnitude lower than that on the surface of a red giant,that for 16O/17O is about 5 times lower,and that for 14N/15N is about 1.5 times lower.The annual yields of 13C,15N,and 17O from nova ejection are larger than those from AGB stars.This indicates that compared to a red giant,nova eruptions are a more important source of the odd-numbered nuclear elements of 13C,15N,and 17O in the Galactic interstellar medium.
      原文链接:
    • 万方数据
    • 维普

    FAST Observations of Four Comets to Search for the Molecular Line Emissions between 1.0 and 1.5 GHz Frequencies

    Long-Fei ChenChao-Wei TsaiJian-Yang LiBin Yang...
    130-140页
    查看更多>>摘要：We used the Five-hundred-meter Aperture Spherical radio Telescope(FAST)to search for the molecular emissions in the L-band between 1.0 and 1.5 GHz toward four comets,C/2020 F3(NEOWISE),C/2020 R4(ATLAS),C/2021 A1(Leonard),and 67P/Churyumov-Gerasimenko during or after their perihelion passages.Thousands of molecular transition lines fall in this low-frequency range,many attributed to complex organic or prebiotic molecules.We conducted a blind search for the possible molecular lines in this frequency range in those comets and could not identify clear signals of molecular emissions in the data.Although several molecules have been detected at high frequencies of greater than 100 GHz in comets,our results confirm that it is challenging to detect molecular transitions in the L-band frequency ranges.The non-detection of L-band molecular lines in the cometary environment could rule out the possibility of unusually strong lines,which could be caused by the masers or non-LTE effects.Although the line strengths are predicted to be weak,for FAST,using the ultra-wide bandwidth receiver and improving the radio frequency interference environments would enhance the detectability of those molecular transitions at low frequencies in the future.
      原文链接:
    • 万方数据
    • 维普

    Nonlinear Coupling of Kinetic Alfvén Waves and Ion Acoustic Waves in the Inner Heliosphere

    Mani K ChettriVivek ShrivastavRupak MukherjeeNidhi Gaur...
    141-158页
    查看更多>>摘要：We study the nonlinear coupling of kinetic Alfvén waves with ion acoustic waves applicable to the Earth's radiation belt and near-Sun streamer belt solar wind using dynamical equations in the form of modified Zakharov systems.Numerical simulations show the formation of magnetic field filamentary structures associated with density humps and dips which become turbulent at later times,redistributing the energy to higher wavenumbers.The magnetic power spectra exhibit an inertial range Kolmogorov-like spectral index value of-5/3 for k⊥ρi<1,followed by a steeper dissipation range spectra with indices∼-3 for the radiation belt case and∼-4 for the near-Sun streamer belt solar wind case,here k⊥ and ρi represent the wavevector component perpendicular to the background magnetic field and the ion thermal gyroradius,respectively.Applying quasilinear theory in terms of the Fokker-Planck equation in the region of wavenumber turbulent spectra,we find the particle distribution function flattening in the superthermal tail population which is the signature of particle energization and plasma heating.
      原文链接:
    • 万方数据
    • 维普

    Physics-informed Neural Network for Force-free Magnetic Field Extrapolation

    Yao ZhangLong XuYihua Yan
    159-169页
    查看更多>>摘要：In this paper,we propose a physics-informed neural network extrapolation method that leverages machine learning techniques to reconstruct coronal magnetic fields.We enhance the classical neural network structure by introducing the concept of a quasi-output layer to address the challenge of preserving physical constraints during the neural network extrapolation process.Furthermore,we employ second-order optimization methods for training the neural network,which are more efficient compared to the first-order optimization methods commonly used in classical machine learning.Our approach is evaluated on the widely recognized semi-analytical model proposed by Low and Lou.The results demonstrate that the deep learning method achieves high accuracy in reconstructing the semi-analytical model across multiple evaluation metrics.In addition,we validate the effectiveness of our method on the observed magnetogram of active region.
      原文链接:
    • 万方数据
    • 维普

    Observation of Standing Slow Magneto-acoustic Waves in a Flaring Active Region Corona Loop

    A.Abedini
    170-179页
    查看更多>>摘要：Intensity fluctuations are frequently observed in different regions and structures of the solar corona.These fluctuations may be caused by magneto-hydrodynamic(MHD)waves in coronal plasma.MHD waves are prime candidates for the dynamics,energy transfer,and anomalous temperature of the solar corona.In this paper,analysis is conducted on intensity and temperature fluctuations along the active region coronal loop(NOAA AR 13599)near solar flares.The intensity and temperature as functions of time and distance along the loop are extracted using images captured by the Atmospheric Imaging Assembly(AIA)instrument onboard the Solar Dynamics Observatory(SDO)space telescope.To observe and comprehend the causes of intensity and temperature fluctuations,after conducting initial processing,and applying spatial and temporal frequency filters to data,enhanced distance-time maps of these variables are drawn.The space-time maps of intensities show standing oscillations at wavelengths of 171,193,and 211Å with greater precision and clarity than earlier findings.The amplitude of these standing oscillations(waves)decreases and increases over time.The average values of the oscillation period,damping time,damping quality,projected wavelength,and projected phase speed of standing intensity oscillations are in the range of 15-18 minutes,24-31 minutes,1.46″-2″,132″-134″,and 81-100 km s-1,respectively.Also,the differential emission measure peak temperature values along the loop are found in the range of 0.51-3.98 MK,using six AIA passbands,including 94,131,171,193,211,and 335Å.Based on the values of oscillation periods,phase speeds,damping time,and damping quality,it is inferred that the fluctuations in intensity are related to standing slow magneto-acoustic waves with weak damping.
      原文链接:
    • 万方数据
    • 维普

    On the Energy Budget of Starquake-induced Repeating Fast Radio Bursts

    王维扬张晨周恩平刘小辉...
    180-188页
    查看更多>>摘要：With a growing sample of fast radio bursts(FRBs),we investigate the energy budget of different power sources within the framework of magnetar starquake triggering mechanism.During a starquake,the energy can be released in any form through strain,magnetic,rotational,and gravitational energies.The strain energy can be converted from three other kinds of energy during starquakes.The following findings are revealed:(1)The crust can store free magnetic energy of ∼1046 erg by existing toroidal fields,sustaining 106 bursts with frequent starquakes occurring due to crustal instability.(2)The strain energy develops as a rigid object spins down,which can be released during a global starquake accompanied by a glitch.However,it takes a long time to accumulate enough strain energy via spindown.(3)The rotational energy of a magnetar with P(≤)0.1 s can match the energy and luminosity budget of FRBs.(4)The budget of the total gravitational energy is high,but the mechanism and efficiency of converting this energy to radiation deserve further exploration.
      原文链接:
    • 万方数据
    • 维普

    The Evolution of Photospheric Current Density During an X9.3-Class Solar Flare

    Hai-Li LiHong-Fei LiangXin-Ping ZhouYu Liu...
    189-200页
    查看更多>>摘要：This paper deduced the temporal evolution of the magnetic field through a series of high-resolution vector magnetograms and calculated the fine distribution map of current density during an X9.3-class flare eruptions using Ampère's law.The results show that a pair of conjugate current ribbons exist on both sides of the magnetic neutral line in this active region,and these conjugate current ribbons persist before,during,and after the flare.It was observed that the X9.3-class flare brightened in the form of a bright core and evolved into a double-ribbon flare over time.Importantly,the position of the double-ribbon flare matches the position of the current ribbons with high accuracy,and their morphologies are very similar.By investigating the complexity of current density and flare morphology,we discovered a potential connection between the eruption of major flares and the characteristics of current density.
      原文链接:
    • 万方数据
    • 维普

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