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国际天文学联合会第252届研讨会

发布时间：2008/05/22

[ 会议基本信息 ]

会议名称（中文）：

国际天文学联合会第252届研讨会

会议名称（英文）：

IAU Symposium 252

所属学科：

天文学　

会议类型：

国际会议

会议论文集是否检索：

不详

开始日期：

2008-4-6

结束日期：

2008-4-11

所在国家：

中华人民共和国

所在城市：

海南省三亚市

具体地点：

主办单位：

International Astronomical Union

协办单位：

The Chinese Academy of Sciences,The National Astronomical Observatories,CAS,The National Natural Science Foundation of China

承办单位：

议题：

[ 组织结构 ]

会议主席：

Cesare Chiosi,Licai Deng

组织委员会主席：

Yanchun Liang

程序委员会主席：

会议嘉宾：

[ 重要日期 ]

摘要截稿日期：

2007-12-15

全文截稿日期：

2008-5-31

论文录用通知日期

交修订版截止日期：

[ 会务组联系方式 ]

联系人：

联系电话：

86-10-64851720

传真：

86-10-64851533

E-mail：

iaus252@bao.ac.cn

通讯地址：

20A Datun Road,Chaoyang District,Beijing,China

邮政编码：

100012

会议新闻(共0条新闻）：

会议注册费：

300$/400$

会议网站：

http://iaus252.bao.ac.cn/

会议背景介绍：

   As a unique link between sub-atomic physics and cosmological processes, stellar astrophysics has been a fundamental subject in astronomy.  The theory of stellar structure and evolution is of special astrophysical significance, in that it is related to phenomena with temporal coverage from the re-ionization of the early universe to the final stages of stars. With the advent of a new generation of large telescopes and new technologies, we will be able to explore the more remote regions of the universe, which are beyond the reach of current facilities. This in turn will make it feasible to investigate the otherwise inaccessible extreme physical conditions. Thanks to the advances in the computation technology, certain subtle yet important physical processes, which have historically been approximated or neglected because of limited computing power, can finally be incorporated into more realistic stellar evolution models. Processes now becoming accessible to more detailed modeling include convection, mass loss, events departing from spherical symmetry and processes taking place on a short time scale relative to the evolution.  Examples of the latter are supernova explosions and helium core and shell flashing.
    To reflect the recent advances and future envision of this field, the symposium will cover the following topics:
－Improvements in the physical ingredients of stellar models
－Progresses in our understanding of physical processes
－The evolution of single stars of different masses
- The evolution of close binary stars
- Constraints on stellar models in the era of very large telescopes.
   The meeting site is Sanya, the only tropical city in China. The symposium is going to take place in a very nice hotel near the beautiful bay in Sanya called Da-Dong-Hai. Sanya was only a small fishing village 20 years ago; it is now a modern city and is turning more and more international. We believe that you will enjoy this setting as well as a fruitful scientific meeting.

征文范围及要求：

    Stars are at the heart of astrophysics and constitute the link between micro-physics and large scale processes in the universe. A proper understanding of their evolution is required to address questions as the origin of the reionization which occurred in the early universe, the chemical and photometric evolution of galaxies, the dynamical evolution of the gas in galaxies, the age of remote starbursts, the origin of the dust, the nature of the progenitors of gamma ray bursts, of supernovae of different types, of neutron stars, black holes and white dwarfs, to cite only a few topical questions. With the advent of new very large telescopes as ALMA, ELT, JWSP, still farther remote regions of the Universe will be explored, allowing to observe stars in conditions which are no longer the ones encountered in the Universe today. Stars might have been much more massive, they had much lower metallicities or were even metal free, had different rotational velocities, magnetic fields, the binary fraction was maybe different. In order to extrapolate the present stellar models to these different conditions at least two prerequisites should be fulfilled: first the physics of the stellar models should be improved. This is the price for allowing extrapolations in more extreme conditions to give a reliable answer. Second, predictions of stellar models should be properly compared with well observed characteristics of nearby stars. The present symposium has for aims to explore the progresses made and expected in these two directions, improvements of the physics and improvements of the stellar predictions. The conference will focus on the hydrostatic phases of the evolution for which the observational constraints are the more numerous and will cover the following topics:
-Improvements of the physical ingredients of stellar models (opacities, nuclear reaction rates, neutrnos, e.o.s., initial composition)
-Progresses in our understanding of physical processes (convection, rotation, internal waves, magnetic fields, mass loss, tidal mixing)
-Topical question concerning the evolution of low and intermediate mass stars (see detailed program below)
-Topical question concerning the evolution of massive stars (see pgm below)
-Topical question concerning close binary evolution
-Stellar physics in the era of very large telescopes.
    The results of the theory of stellar structure and evolution have been one of the most important ingredients embedded in almost all research fields in nowadays astrophysics. The current overall picture of the Universe and the formation and evolution of structures in different scales depend very much on the output of such a theory. The currently available (one dimensional) models are able to follow all the hydrostatic phase of stellar evolution from the pre-main-sequence to the Debye phase of the cooling of WDs, and to prepare models of structure which constitute a viable input to study the hydrodynamic phases of the SN event. This does not mean that stellar evolution is resolved. In many cases, the more general studies in present day astrophysics are not fully based on computed models, but on parametric, well educated guesses of the outcome of the most difficult phases of stellar evolution. Thanks to the advances in computational technology, making stellar model beyond 1D and incorporating physical processes (rotation, realistic atmospheres, magnetic fields, mass loss and binary interactions) that have been previously neglected are now possible. The studies of helio seismology (and the brand-new technique of astero seismology) are offering a new, independent tool for understanding in detail the stellar interiors. Nevertheless, many open problems remain in the study of stellar structure, and a qualitative progress is necessary in many areas, among which we quote:
-Computation of multi-dimensional (2D and 3D) models of stellar structure, interaction of the traditional stellar community with the hydro-people;
-Realistic atmospheres must be included in the models; interaction with this community;
-Magnetic fields;
-Mixing processes (from rotation to gravity waves to hydro-instabilities)
-mass loss (from models, not from fitting formulae)
    Revisiting the classical difficulties in building up more realistic stellar models, integrating all the new developments in different fields of stellar physics into the theory and making the new models available for applications becomes necessary. Such a feeling is shared in this community.
    Among the questions to be addressed are the following:
-What do we have on stellar opacity and EOS? Do we need more?
-How do we cope with convection? Downgradient-Approximation (DGA, 1D) or 3D?
-How does rotation affect evolution of stars?
-How does mass loss affect stellar evolution in hydrodynamic models?
-How do we incorporate observations of the Sun into the evolution of low mass stars?
-What do we know about the physics of AGB stars?
-What do we know about the extremely blue horizontal branch stars?
-What do we know about low and intermediate mass stars beyond AGB?
-Do models of massive stars fit both photometric and spectroscopic observations of supergiants?
-What do we learn from the massive star population in the Galactic center?
-How does rotation affect the evolution of massive stars?
-What can we say about the properties of first stars?
-What do we know about the evolution of close binaries?
-What is the consequences of the population of interactive binaries in general?
-3D models are now available, how can we make good use of them in building up stellar models?

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