Pub Date : 2001-09-01DOI: 10.1201/9781420033304.CH11
M. Hendry
{"title":"Dynamical methods for reconstructing the large scale galaxy density and velocity fields","authors":"M. Hendry","doi":"10.1201/9781420033304.CH11","DOIUrl":"https://doi.org/10.1201/9781420033304.CH11","url":null,"abstract":"","PeriodicalId":198344,"journal":{"name":"The Restless Universe","volume":"5 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2001-09-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"126588153","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2001-06-05DOI: 10.1887/0750308222/b471c9
D. Merritt
Orbital and self-consistent dynamics of non-integrable galaxy models are reviewed. Topics covered include torus construction; resonances; triaxial systems with central singularities; mixing and collisionless relaxation; and chaos in collisional systems.
{"title":"Non-integrable galactic dynamics","authors":"D. Merritt","doi":"10.1887/0750308222/b471c9","DOIUrl":"https://doi.org/10.1887/0750308222/b471c9","url":null,"abstract":"Orbital and self-consistent dynamics of non-integrable galaxy models are reviewed. Topics covered include torus construction; resonances; triaxial systems with central singularities; mixing and collisionless relaxation; and chaos in collisional systems.","PeriodicalId":198344,"journal":{"name":"The Restless Universe","volume":"41 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2001-06-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"131047300","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2001-01-17DOI: 10.1887/0750308222/b471c10
M. Weinberg
These lectures will cover methods for studying the evolution of galaxies since their formation. Because the properties of a galaxy depend on its history, an understanding of galaxy evolution requires that we understand the dynamical interplay between all components over 10 gigayears. For example, lopsided (m = 1) asymmetries are transient with gigayear time scales, bars may grow slowly or suddenly and, under circumstances may decay as well. Recent work shows that stellar populations depend on asymmetry.
{"title":"Evolution of galaxies due to self-excitation","authors":"M. Weinberg","doi":"10.1887/0750308222/b471c10","DOIUrl":"https://doi.org/10.1887/0750308222/b471c10","url":null,"abstract":"These lectures will cover methods for studying the evolution of galaxies since their formation. Because the properties of a galaxy depend on its history, an understanding of galaxy evolution requires that we understand the dynamical interplay between all components over 10 gigayears. For example, lopsided (m = 1) asymmetries are transient with gigayear time scales, bars may grow slowly or suddenly and, under circumstances may decay as well. Recent work shows that stellar populations depend on asymmetry.","PeriodicalId":198344,"journal":{"name":"The Restless Universe","volume":"716 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2001-01-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"115127438","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2000-11-30DOI: 10.1201/9781420033304.PT3
M. Merrifield
These lectures are intended to provide an introduction to the rich interplay between N-body simulations and stellar-kinematic observations of galaxies. The first section describes the kinematic properties of galaxies that are accessible to observation, and gives a brief introduction to the stellar dynamics that one might wish to infer from such observations. In the next section, the use of N-body simulations in the study of galaxy dynamics is placed in its historical context. The next two sections provide case studies of the stellar-dynamical properties of elliptical and disk galaxies where N-body simulations have been used to explain kinematic data, to test new analysis techniques, and to motivate further observations. The final section contains some speculation as to how the symbiotic relation between observations and N-body simulations may develop in future studies of galaxy dynamics.
{"title":"Galaxies: kinematics to dynamics","authors":"M. Merrifield","doi":"10.1201/9781420033304.PT3","DOIUrl":"https://doi.org/10.1201/9781420033304.PT3","url":null,"abstract":"These lectures are intended to provide an introduction to the rich interplay between N-body simulations and stellar-kinematic observations of galaxies. The first section describes the kinematic properties of galaxies that are accessible to observation, and gives a brief introduction to the stellar dynamics that one might wish to infer from such observations. In the next section, the use of N-body simulations in the study of galaxy dynamics is placed in its historical context. The next two sections provide case studies of the stellar-dynamical properties of elliptical and disk galaxies where N-body simulations have been used to explain kinematic data, to test new analysis techniques, and to motivate further observations. The final section contains some speculation as to how the symbiotic relation between observations and N-body simulations may develop in future studies of galaxy dynamics.","PeriodicalId":198344,"journal":{"name":"The Restless Universe","volume":"47 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2000-11-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"124695997","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2000-11-15DOI: 10.1887/0750308222/b471c7
D. Heggie
This didactic paper is motivated by the problem of understanding how stars escape from globular star clusters. One formulation of this problem is known, in dynamical astronomy, as Hill's problem. Originally intended as a model for the motion of the moon around the earth with perturbations by the sun, with simple modifications it also serves as a model for the motion of a star in a star cluster with perturbations by the galaxy. The paper includes introductory sections on the derivation of the equations of motion of Hill's problem, their elementary properties, and extensions to deal with non-point masses and non-circular orbits. We then show how the rate of escape may be calculated numerically and estimated theoretically, and discuss how this simple picture is modified if the stars in a cluster are also undergoing two-body relaxation. Finally we introduce some established ideas for obtaining the distribution of escape times.
{"title":"Escape in Hill’s problem","authors":"D. Heggie","doi":"10.1887/0750308222/b471c7","DOIUrl":"https://doi.org/10.1887/0750308222/b471c7","url":null,"abstract":"This didactic paper is motivated by the problem of understanding how stars escape from globular star clusters. One formulation of this problem is known, in dynamical astronomy, as Hill's problem. Originally intended as a model for the motion of the moon around the earth with perturbations by the sun, with simple modifications it also serves as a model for the motion of a star in a star cluster with perturbations by the galaxy. \u0000The paper includes introductory sections on the derivation of the equations of motion of Hill's problem, their elementary properties, and extensions to deal with non-point masses and non-circular orbits. We then show how the rate of escape may be calculated numerically and estimated theoretically, and discuss how this simple picture is modified if the stars in a cluster are also undergoing two-body relaxation. Finally we introduce some established ideas for obtaining the distribution of escape times.","PeriodicalId":198344,"journal":{"name":"The Restless Universe","volume":"88 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2000-11-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"128338580","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"N-body simulations of the Solar System, planet formation, and galaxy clusters","authors":"T. Quinn","doi":"10.1201/9780429187148-1","DOIUrl":"https://doi.org/10.1201/9780429187148-1","url":null,"abstract":"","PeriodicalId":198344,"journal":{"name":"The Restless Universe","volume":"28 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"126672860","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
京公网安备 11010802042870号
京ICP备2023020795号-1
扫码关注我们
求助内容：
应助结果提醒方式：