首页期刊导航|天文和天体物理学研究
期刊信息/Journal information
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。
正式出版
收录年代

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

    Wei-Nan WangJin-Song PingMing-Yuan WangWen-Zhao Zhang...
    1-6页
    查看更多>>摘要:Lunar optical polarization is a fascinating phenomenon that occurs when sunlight reflects off the surface of the Moon and becomes polarized.This study employs a novel split-focus plane polarimetric camera to conduct the initial white light polarimetric observations on the near side of the Moon.We obtained the linear degree of polarization(DOP)parameters of white light by observation from the eastern and western hemispheres of the Moon.The findings indicate that the white light polarization is lower in the lunar highland than in the lunar maria overall.Combining 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 Moon.This study may serve as a new diagnostic tool for the Moon.

    Dynamical Dark Energy in Light of Cosmic Distance Measurements.I.A Demonstration Using Simulated Datasets

    Gan GuXiaoma WangXiaoyong MuShuo Yuan...
    7-14页
    查看更多>>摘要:We develop methods to extract key dark energy information from cosmic distance measurements including the BAO scales and supernova(SN)luminosity distances.Demonstrated using simulated data sets of the complete DESI,LSST and Roman surveys designed for BAO and SN distance measurements,we show that using our method,the dynamical behavior of the energy,pressure,equation of state(with its time derivative)of dark energy and the cosmic deceleration function can all be accurately recovered from high-quality data,which allows for robust diagnostic tests for dark energy models.

    Dynamical Dark Energy in Light of Cosmic Distance Measurements.Ⅱ.A Study Using Current Observations

    Xiaoma WangGan GuXiaoyong MuShuo Yuan...
    15-20页
    查看更多>>摘要:We extract key information on dark energy from current observations of BAO,OHD and H0,and find hints of dynamical behavior of dark energy.In particular,a dynamical dark energy model whose equation of state crosses-1 is favored by observations.We also find that the Universe has started accelerating at a lower redshift than expected.

    What is the Role of Gravity,Turbulence and Magnetic Fields in High-mass Star Formation Clouds?

    An-Xu LuoHong-Li LiuGuang-Xing LiSirong Pan...
    21-27页
    查看更多>>摘要:To explore the potential role of gravity,turbulence and magnetic fields in high-mass star formation in molecular clouds,this study revisits the velocity dispersion-size(σ-L)and density-size(ρ-L)scalings and the associated turbulent energy spectrum using an extensive data sample.The sample includes various hierarchical density structures in high-mass star formation clouds,across scales of 0.01-100pc.We observe σ∝ L0.26 and ρ∝L-154 scalings,converging toward a virial equilibrium state.A nearly flat virial parameter-mass(αvir-M)distribution is seen across all density scales,with αvir values centered around unity,suggesting a global equilibrium maintained by the interplay between gravity and turbulence across multiple scales.Our turbulent energy spectrum(E(k))analysis,based on the σ-L and ρ-L scalings,yields a characteristic E(k)∝k-1.52.These findings indicate the potential significance of gravity,turbulence,and possibly magnetic fields in regulating dynamics of molecular clouds and high-mass star formation therein.

    Study of 26 Galactic Open Clusters with Extended Main-sequence Turnoffs

    Yang-Yang DengZhong-Mu Li
    28-37页
    查看更多>>摘要:Recent studies indicate that some Galactic open clusters(OCs)exhibit extended main-sequence tumoff(eMSTO)in their color-magnitude diagrams(CMDs).However,the number of Galactic OCs with eMSTO structures detected so far is limited,and the reasons for their formation are still unclear.This work identifies 26 Galactic OCs with undiscovered eMSTOs and investigates the causes of these features.Stellar population types and fundamental parameters of cluster samples are acquired using CMD fitting methods.Among them,the results of 11 OCs are reliable as the observed CMDs are well-reproduced.We propose the crucial role of stellar binarity and confirm the importance of stellar rotation in reproducing eMSTO morphologies.The results also show that the impact of age spread is important,as it can adequately explain the structure of young OCs and fit the observed CMDs of intermediate-age OCs better.

    An Asymmetric Galactic Stellar Disk Traced by OB-type Stars from LAMOST DR7

    Xiaopeng LiuHao TianWenyuan CuiLinlin Li...
    38-51页
    查看更多>>摘要:Using 9943 OB-type stars from LAMOST DR7 in the solar neighborhood,we fit the vertical stellar density profile with the model including a single exponential distribution at different positions(R,Φ).The distributions of the scale heights and scale length show that the young disk traced by the OB-type stars is not axisymmetric.The scale length decreases versus the azimuthal angleΦ,i.e.,from 1.14+0.30-0.19 kpc withΦ=-3° to 0.77+0.08-0.06kpc withΦ=9°.Meanwhile we find signal of non-symmetry in the distribution of the scale height of the north and south of the disk plane.The scale height in the north side shows signal of flaring of the disk,while that of the south disk stays almost constant around hs=130 pc.The distribution of the displacement of the disk plane Z0 also shows variance versus the azimuthal angleΦ,which displays significant differences with the warp model constrained by the Cepheid stars.We also test different values for the position of the Sun,and the distance between the Sun and the Galactic center affects the scale heights and the displacement of the disk significantly,but that does not change our conclusion that the disk is not axisymmetric.

    Stellar Populations of AGN-host Dwarf Galaxies Selected with Different Methods

    Xiejin Li赵应和Jinming Bai
    52-67页
    查看更多>>摘要:In this paper we investigate the stellar populations and star formation histories of 235 active galactic nucleus(AGN)-host dwarf galaxies,consisting of four samples identified separately with different methods(i.e.,radio,X-ray,mid-IR and variability),utilizing the synthesis code STARLIGHT and spectra from the Sloan Digital Sky Survey Data Release 8.Our results show that the variability sample is the oldest,while the mid-IR sample is the youngest,for which the luminosity at 4020 Å is dominated(>50%)by the young population(t<108 yr).The light-weighted mean stellar age of the whole sample is in general about 0.7 dex younger than the optical sample studied in Cai et al.We compare the population results between fitting models with and without a power-law(PL)component and find that the neglect of a PL component would lead to an under-and over-estimation by 0.2 and 0.1 dex for the light-and mass-weighted mean stellar age,respectively,for our sample of dwarf galaxies,which has a mean fractional contribution of~16%from the AGN.In addition,we obtain further evidence for a possible suppression of star formation in the host galaxy by the central AGN.We also find that there exists an anti-correlation between the extinction-corrected[O m]luminosity and light-weighted mean stellar age,confirming our previous finding that there is a physical connection between AGN and star-forming activities in AGN-host dwarfs.

    Inelastic Scattering of Dark Matter with Heavy Cosmic Rays

    Keyu LuYue-Lin Sming TsaiQiang YuanLe Zhang...
    68-80页
    查看更多>>摘要:We investigate the impact of inelastic collisions between dark matter(DM)and heavy cosmic ray(CR)nuclei on CR propagation.We approximate the fragmentation cross-sections for DM-CR collisions using collider-measured proton-nuclei scattering cross-sections,allowing us to assess how these collisions affect the spectra of CR boron and carbon.We derive new CR spectra from DM-CR collisions by incorporating their cross-sections into the source terms and solving the diffusion equation for the complete network of reactions involved in generating secondary species.In a specific example with a coupling strength of bx=0.1 and a DM mass of mx=0.1 GeV,considering a simplified scenario where DM interacts exclusively with oxygen,a notable modification in the boron-to-carbon spectrum due to the DM-CR interaction is observed.Particularly,the peak within the spectrum,spanning from 0.1 to 10 GeV,experiences an enhancement of approximately 1.5 times.However,in a more realistic scenario where DM particles interact with all CRs,this peak can be amplified to twice its original value.Utilizing the latest data from AMS-02 and DAMPE on the boron-to-carbon ratio,we estimate a 95%upper limit for the effective inelastic cross-section of DM-proton as a function of DM mass.Our findings reveal that at mx(≈)2 MeV,the effective inelastic cross-section between DM and protons must be less than O(10-32)cm2.

    Study of Complex Nitrogen and Oxygen-bearing Molecules toward the High-mass Protostar IRAS 18089-1732

    Arijit MannaSabyasachi PalTapas BaugSougata Mondal...
    81-93页
    查看更多>>摘要:The observation of oxygen(O)-and nitrogen(N)-bearing molecules gives an idea about the complex prebiotic chemistry in the interstellar medium.Recent millimeter and submillimeter wavelength observations have shown the presence of complex O-and N-bearing molecules in the star formation regions.So,the investigation of those molecules is crucial to understanding the chemical complexity in the star-forming regions.In this article,we present the identification of the rotational emission lines of N-bearing molecules ethyl cyanide(C2H5CN)and cyanoacetylene(HC3N),and O-bearing molecule methyl formate(CH3OCHO)toward high-mass protostar IRAS 18089-1732 using the Atacama Compact Array.We also detected the emission lines of both the N-and O-bearing molecule formamide(NH2CHO)in the envelope of IRAS 18089-1732.We have detected the v=0 and 1 state rotational emission lines of CH3OCHO.We also detected the two vibrationally excited states of HC3N(v7=1 and v7=2).The estimated fractional abundances of C2H5CN,HC3N(v7=1),HC3N(v7=2),and NH2CHO toward IRAS 18089-1732 are(1.40±0.5)x 10-10,(7.5±0.7)× 10-11,(3.1±0.4)x 10-11,and(6.25±0.82)x 10-11 respectively.Similarly,the estimated fractional abundances of CH3OCHO(v=0)and CH3OCHO(v=1)are(1.90±0.9)x 10-9 and(8.90±0.8)× 10-10,respectively.We also created the integrated emission maps of the detected molecules,and the observed molecules may have originated from the extended envelope of the protostar.We show that C2H5CN and HC3N are most probably formed via the subsequential hydrogenation of the CH2CHCN and the reaction between C2H2 and CN on the grain surface of IRAS 18089-1732.We found that NH2CHO is probably produced due to the reaction between NH2 and H2CO in the gas phase.Similarly,CH3OCHO is possibly created via the reaction between radical CH3O and radical HCO on the grain surface of IRAS 18089-1732.

    Study of Secondary Cosmic Rays and Astronomical X-Ray Sources using Small Stratospheric Balloons

    Rupnath SikdarSandip K.ChakrabartiDebashis Bhowmick
    94-109页
    查看更多>>摘要:The X-ray sources of the universe are extraterrestrial in nature which emit X-ray photons.The closest strong X-ray source is the Sun,which is followed by various compact sources such as neutron stars,black holes,the Crab pulsar,etc.In this paper,we analyze the data received from several low-cost lightweight meteorological balloon-borne missions launched by the Indian Centre for Space Physics.Our main interest is to study the variation of the vertical intensity of secondary cosmic rays,the detection of strong X-ray sources,and their spectra in the energy band of~10-80 keV during the complete flights.Due to the lack of an onboard pointing system,low exposure time,achieving a maximum altitude of only~42 km,and freely rotating the payload about its axis,we modeled the background radiation flux for the X-ray detector using physical assumptions.We also present the source detection method,observation of the pulsation of the Crab(~33 Hz),and spectra of some sources such as the quiet Sun and the Crab pulsar.