主 讲 人 ：王海峰
Inthe Gaia era, with the help of Large sky surveys such as current 2MASS, SDSS,RAVE, PanSTARRS, LAMOST, APOGEE, DES, TESS catalog and future plans such as4MOST, WEAVE, MSE,WFST, Mephisto, LSST, etc. There is no doubt that we areentering into the golden era to investigate the formation history and structureof our home galaxy in multiple stellar populations of six-phase space bychemical tagging, time tagging, kinematics and dynamics. Our home galaxy is atypical dynamic systems that are perturbed by bars, spiral structures, warp,giant molecular clouds, dark matter subhalos, Gaia–Enceladus, Sgr, LMC, SMC, tidallydisrupt satellite galaxies and so on . These processes will leave behind someimprints on stars, demonstrating abundant population structures dominated bydynamics and Galactoseismology signals. I propose a plan to Mapping the MilkyWay Disk Population Structures and Galactoseismology (MWDPSG) with large skysurveys. I will try my best to figure out : what about the populationmorphology of the outer disk? Where is the truncation of the milky way disk?What are the mechanisms for the many asymmetric substructures andGalactoseismology? How do the dark matter halo, bars, spiral arms interact withthe stellar disk? etc. Thus then, We could establish a theoretical framework inthe future to unify the global picture of the disk structures and origins with acomprehensive distribution function. There is still a long way for us to gowith this project, in this talk, I will share my recent new progress about theGalactic disk with LAMOST and Gaia data.
Hai-FengWang (王海峰)，Postdoctoral Fellow ofYunnan University (2018-present), LAMOST Fellow of Chinese Academy of Sciences (2018-present),Ph.D in Astrophysics of National Astronomical Observatories, Chinese Academy ofSciences (2013-2018).
研究领域:Chemo-DynamicalStructures of the Milky Way, Time Domain Stellar Physics, Near-Field Cosmology,Astronomical big data reduction and analysis, and etc.