[PDF] Top 20 Springel, Volker (2000): On the formation and evolution of galaxies. Dissertation, LMU München: Fakultät für Physik

... RBT| [[^]:Nx8J kFIlmH!]:N.]:xH!WK]]žN.Fx.]:V BPBBOBOBPBOBOBPBBOBPBOBOBOBPBBOBPBOBOBOBPBB†A:|>}.. *,8O{={='5X=_'5;>P6­=_3.v')#6X7Œ6ŒŠ%j_')‹@$=_'@68.t.Š+=_3+1 ‰ $%j#&<Š3.'@¤[r] ... See full document

... the formation and evolution of massive galaxies is promising but we will need to improve the models used in our simulations in the future to study the effects of galactic winds and active galactic ... See full document

... the formation and evolution of large scale structure (LSS) emerged as one of the most interesting branches of cosmology (Padmanabhan 1993; Silk 1994; Longair ...the formation and evolution of ... See full document

... Observationally, the predicted abundance of substructures in clusters is one of the major successes of the CDM model (Springel et al. 2001a), but on galactic scales, it appears that simulations predict more ... See full document

... star-forming galaxies have been considered as marginally- unstable thick disks, where the large random motions set the large masses and sizes for unstable regions collapsing into giant clumps (Bournaud et ...of ... See full document

... massive galaxies due to the deeper potential ...in galaxies have been already very strong (comparable to present-day galactic magnetic fields) at very high redshifts, at a time when the universe was only t ≈ ... See full document

... star formation rate is only slightly ...the formation of arti- cial cold blobs. We note that the star formation model as well as the feedback recipe have also signicant impact on the evolution ... See full document

... of galaxies is not well ...Guiderdoni 2000; Granato et ...luminous galaxies at high ...Lyman-Break Galaxies, the BX Galaxies (star forming galaxies at z ∼ 2) and Distant Red ... See full document

... [r] ... See full document

... the Hubble time. Observations show that a type of clusters, namely the cool-core clusters, exhibits a centrally peaked X-ray surface brightness profile (and Fe abundance profile) and a gradual drop in the ICM temperature ... See full document

... ÁÂÅÁÇË ÞTÁÂÃÃÀ7ÂÅ7ÀÈÉÃÊÎeÓ7Â͕Á9ÍbœãÂÃÅIÁÌË?ÀÚÒÑgÅIÁ9ÃÜÝË ÃÄ Î7ÆÇÅMÁ0WOËÈÉÃÖÅÆÄ ÅÑڕÏÁ9ÃÏÖӕÃÑÅÁ×7ÑEÃÖÁÂÃÀMÁÂÃÖÈÑ[Ë ÁÌË ÈÅ7Äê ë ÞÍ7Ñ. Ó7Â͕Á9ÍbœÃÕíÅӕÍÑÅÁÌË ÍœÀªWR͜×7Ä ÎlەÄËåÀÈÑEÃÅÆ[r] ... See full document

... In Zusammenarbeit mit D. Croton, G. de Lucia, V. Springel und S.D.M. White bediente ich mich der Mill- ennium Simulation, einer extrem großen ‘N-body’ Simulation der gravitativen Wechselwirkung Dunkler Materie ... See full document

... ®5BW® ݄ïw.. ­,° 780 BmBYBuBYBuBYBYBuBYBuBYBmBYBYBuBYBuBYBuBYBuBYBYBmBYBuBYBè‰v‰+c[r] ... See full document

... al., 2000 ; Arnaboldi et ...elliptical galaxies, while the ICL component dominates the diffuse light in only one field, where a ‘broad’ line-of-sight velocity distribution is measured, and all PNe are true ... See full document

... After the disc fragmentation to single clumps, they immediately group to clump clusters (CCs) on different spatial scales. In this section we identify these scales by using different beam-smearings (BS) and estimate the ... See full document

... cluster evolution and galaxy ...structure formation while incorporating ideas and theories from cosmic ray and plasma ...of galaxies and their hadronic interactions with the ambient thermal plasma ... See full document

... galaxy formation and ...the formation of lower metal- licity stars during a rapid radial collapse, which later proceeded to form the stellar ...spheroidal galaxies today observed as satellites of the ... See full document

... star formation rates of ...galaxy formation (for exam- ple see White and Frenk 1991 and Cole et al. 2000) successfully reproduce many of the the observed properties of ...of galaxies at the ... See full document

... star formation properties we tested different parameters of the adopted star formation and feedback model (Springel & Hernquist 2003) and found that the relative strength and the exact locations ... See full document

... the evolution of the ini- tial density field is followed explicitly by solving the gravitational and hydrodynamical equations (see Equations ...the evolution of gas without relying on simplified ... See full document