Niemeyer, J

[["dc.bibliographiccitation.firstpage","1683"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","The Astrophysical Journal"],["dc.bibliographiccitation.lastpage","1693"],["dc.bibliographiccitation.volume","710"],["dc.contributor.author","Schmidt, W."],["dc.contributor.author","Ciaraldi-Schoolmann, F."],["dc.contributor.author","Niemeyer, J. C."],["dc.contributor.author","Roepke, F. K."],["dc.contributor.author","Hillebrandt, W."],["dc.date.accessioned","2018-11-07T08:45:52Z"],["dc.date.accessioned","2020-07-02T14:45:12Z"],["dc.date.available","2018-11-07T08:45:52Z"],["dc.date.available","2020-07-02T14:45:12Z"],["dc.date.issued","2010"],["dc.description.abstract","The delayed detonation model describes the observational properties of the majority of Type Ia supernovae very well. Using numerical data from a three-dimensional deflagration model for Type Ia supernovae, the intermittency of the turbulent velocity field and its implications on the probability of a deflagration-to-detonation (DDT) transition are investigated. From structure functions of the turbulent velocity fluctuations, we determine intermittency parameters based on the log-normal and the log-Poisson models. The bulk of turbulence in the ash regions appears to be less intermittent than predicted by the standard log-normal model and the She-Leveque model. On the other hand, the analysis of the turbulent velocity fluctuations in the vicinity of the flame front by Ropke suggests a much higher probability of large velocity fluctuations on the grid scale in comparison to the log-normal intermittency model. Following Pan et al., we computed probability density functions for a DDT for the different distributions. The determination of the total number of regions at the flame surface, in which DDTs can be triggered, enables us to estimate the total number of events. Assuming that a DDT can occur in the stirred flame regime, as proposed by Woosley et al., the log-normal model would imply a delayed detonation between 0.7 and 0.8 s after the beginning of the deflagration phase for the multi-spot ignition scenario used in the simulation. However, the probability drops to virtually zero if a DDT is further constrained by the requirement that the turbulent velocity fluctuations reach about 500 km s(-1). Under this condition, delayed detonations are only possible if the distribution of the velocity fluctuations is not log-normal. From our calculations follows that the distribution obtained by Ropke allow for multiple DDTs around 0.8 s after ignition at a transition density close to 1 x 107 g cm(-3)."],["dc.identifier.doi","10.1088/0004-637X/710/2/1683"],["dc.identifier.isi","000274233300061"],["dc.identifier.scopus","2-s2.0-77149168162"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/20548"],["dc.identifier.url","http://www.scopus.com/inward/record.url?eid=2-s2.0-77149168162&partnerID=MN8TOARS"],["dc.language.iso","en"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.relation.eissn","1538-4357"],["dc.relation.issn","0004-637X"],["dc.title","Turbulence in a three-dimensional deflagration model for type Ia Supernovae. II. Intermittency and the deflagration-to-detonation transition probability"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","3051"],["dc.bibliographiccitation.issue","4"],["dc.bibliographiccitation.journal","Monthly Notices of the Royal Astronomical Society"],["dc.bibliographiccitation.lastpage","3077"],["dc.bibliographiccitation.volume","440"],["dc.contributor.author","Schmidt, W."],["dc.contributor.author","Almgren, A. S."],["dc.contributor.author","Braun, H."],["dc.contributor.author","Engels, Jan F."],["dc.contributor.author","Niemeyer, J. C."],["dc.contributor.author","Schulz, J."],["dc.contributor.author","Mekuria, R. R."],["dc.contributor.author","Aspden, A. J."],["dc.contributor.author","Bell, J. B."],["dc.date.accessioned","2018-11-07T09:39:46Z"],["dc.date.accessioned","2020-07-16T12:51:32Z"],["dc.date.available","2018-11-07T09:39:46Z"],["dc.date.available","2020-07-16T12:51:32Z"],["dc.date.issued","2013"],["dc.description.abstract","We investigate turbulence generated by cosmological structure formation by means of large eddy simulations using adaptive mesh refinement. In contrast to the widely used implicit large eddy simulations, which resolve a limited range of length scales and treat the effect of turbulent velocity fluctuations below the grid scale solely by numerical dissipation, we apply a subgrid-scale model for the numerically unresolved fraction of the turbulence energy. For simulations with adaptive mesh refinement, we utilize a new methodology that allows us to adjust the scale-dependent energy variables in such a way that the sum of resolved and unresolved energies is globally conserved. We test our approach in simulations of randomly forced turbulence, a gravitationally bound cloud in a wind, and the Santa Barbara cluster. To treat inhomogeneous turbulence, we introduce an adaptive Kalman filtering technique that separates turbulent velocity fluctuations on resolved length scales from the non-turbulent bulk flow. From the magnitude of the fluctuating component and the subgrid-scale turbulence energy, a total turbulent velocity dispersion of several 100 km/s is obtained for the Santa Barbara cluster, while the low-density gas outside the accretion shocks is nearly devoid of turbulence. The energy flux through the turbulent cascade and the dissipation rate predicted by the subgrid-scale model correspond to dynamical time scales around 5 Gyr, independent of numerical resolution."],["dc.identifier.doi","10.1093/mnras/stu501"],["dc.identifier.isi","000336213800015"],["dc.identifier.scopus","2-s2.0-84899826562"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/67192"],["dc.identifier.url","http://www.scopus.com/inward/record.url?eid=2-s2.0-84899826562&partnerID=MN8TOARS"],["dc.language.iso","en"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.relation.eissn","0035-8711"],["dc.relation.issn","1365-2966"],["dc.title","Cosmological fluid mechanics with adaptively refined large eddy simulations"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","142"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","Monthly Notices of the Royal Astronomical Society"],["dc.bibliographiccitation.lastpage","156"],["dc.bibliographiccitation.volume","470"],["dc.contributor.author","Schmidt, W."],["dc.contributor.author","Byrohl, C."],["dc.contributor.author","Engels, J. F."],["dc.contributor.author","Behrens, C."],["dc.contributor.author","Niemeyer, J. C."],["dc.date.accessioned","2020-12-10T18:19:26Z"],["dc.date.available","2020-12-10T18:19:26Z"],["dc.date.issued","2017"],["dc.identifier.doi","10.1093/mnras/stx1274"],["dc.identifier.eissn","1365-2966"],["dc.identifier.issn","0035-8711"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/75243"],["dc.language.iso","en"],["dc.notes.intern","DOI Import GROB-354"],["dc.title","Viscosity, pressure and support of the gas in simulations of merging cool-core clusters"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A14"],["dc.bibliographiccitation.firstpage","A14"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","526"],["dc.contributor.author","Seifried, D."],["dc.contributor.author","Schmidt, W."],["dc.contributor.author","Niemeyer, J. C."],["dc.date.accessioned","2018-11-07T08:59:43Z"],["dc.date.accessioned","2020-07-22T09:32:26Z"],["dc.date.available","2018-11-07T08:59:43Z"],["dc.date.available","2020-07-22T09:32:26Z"],["dc.date.issued","2010"],["dc.description.abstract","Context: The thermal instability is one of the dynamical agents for turbulence in the diffuse interstellar medium, where both, turbulence and thermal instability interact in a highly non-linear manner. Aims: We study basic properties of turbulence in thermally bistable gas for variable simulation parameters. The resulting cold gas fractions can be applied as parameterisation in simulations on galactic scales. Methods: Turbulent flow is induced on large scales by means of compressive stochastic forcing in a periodic box. The compressible Euler equations with constant UV heating and a parameterised cooling function are solved on uniform grids. We investigate several values of the mean density of the gas and different magnitudes of the forcing. For comparison with other numerical studies, solenoidal forcing is applied as well. Results: After a transient phase, we observe that a state of statistically stationary turbulence is approached. Compressive forcing generally produces a two-phase medium, with a decreasing fraction of cold gas for increasing forcing strength. This behaviour can be explained on the basis of turbulent mixing. We also find indications for power-law tails of probability density functions of the gas density. Solenoidal forcing, on the other hand, appears to prevent the evolution into a two-phase-medium for certain parameter regions. Conclusions: The dynamics of thermally bistable turbulence shows a substantial sensitivity on the initial state and the forcing properties."],["dc.description.sponsorship","DFG [BA3706]"],["dc.identifier.doi","10.1051/0004-6361/201014373"],["dc.identifier.isi","000286458400026"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/8618"],["dc.identifier.scopus","2-s2.0-78650105619"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/67384"],["dc.identifier.url","http://www.scopus.com/inward/record.url?eid=2-s2.0-78650105619&partnerID=MN8TOARS"],["dc.language.iso","en"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.relation.eissn","1432-0746"],["dc.relation.issn","0004-6361"],["dc.rights","Goescholar"],["dc.rights.uri","https://goedoc.uni-goettingen.de/licenses"],["dc.title","Forced turbulence in thermally bistable gas: A parameter study"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","265"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","281"],["dc.bibliographiccitation.volume","450"],["dc.contributor.author","Schmidt, W."],["dc.contributor.author","Niemeyer, J. C."],["dc.contributor.author","Hillebrandt, W."],["dc.date.accessioned","2020-07-22T09:41:38Z"],["dc.date.available","2020-07-22T09:41:38Z"],["dc.date.issued","2006"],["dc.description.abstract","We present a one-equation subgrid scale model that evolves the turbulence energy corresponding to unresolved velocity fluctuations in large eddy simulations. The model is derived in the context of the Germano consistent decomposition of the hydrodynamical equations. The eddy-viscosity closure for the rate of energy transfer from resolved toward subgrid scales is localised by means of a dynamical procedure for the computation of the closure parameter. Therefore, the subgrid scale model applies to arbitrary flow geometry and evolution. For the treatment of microscopic viscous dissipation a semi-statistical approach is used, and the gradient-diffusion hypothesis is adopted for turbulent transport. A priori tests of the localised eddy-viscosity closure and the gradient-diffusion closure are made by analysing data from direct numerical simulations. As an a posteriori testing case, the large eddy simulation of thermonuclear combustion in forced isotropic turbulence is discussed. We intend the formulation of the subgrid scale model in this paper as a basis for more advanced applications in numerical simulations of complex astrophysical phenomena involving turbulence."],["dc.identifier.doi","10.1051/0004-6361:20053617"],["dc.identifier.scopus","2-s2.0-33645821906"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/67391"],["dc.identifier.url","http://www.scopus.com/inward/record.url?eid=2-s2.0-33645821906&partnerID=MN8TOARS"],["dc.language.iso","en"],["dc.relation.eissn","1432-0746"],["dc.relation.issn","0004-6361"],["dc.title","A localised subgrid scale model for fluid dynamical simulations in astrophysics I. Theory and numerical tests"],["dc.type","journal_article"],["dc.type.internalPublication","no"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","Code 103036"],["dc.bibliographiccitation.firstpage","79"],["dc.bibliographiccitation.lastpage","91"],["dc.contributor.author","Schmidt, W."],["dc.contributor.author","Maier, A."],["dc.contributor.author","Hupp, M."],["dc.contributor.author","Federrath, C."],["dc.contributor.author","Niemeyer, J."],["dc.contributor.editor","Wagner, Siegfried"],["dc.contributor.editor","Steinmetz, Matthias"],["dc.contributor.editor","Bode, Arndt"],["dc.contributor.editor","Brehm, Matthias"],["dc.date.accessioned","2020-07-09T08:29:54Z"],["dc.date.available","2020-07-09T08:29:54Z"],["dc.date.issued","2009"],["dc.description.abstract","For the treatment of astrophysical flows with high Mach numbers and high Reynolds numbers, we proposed a method called FEARLESS (Fluid mEchanics with Adaptively Refined Large-Eddy SimulationS) that combines adaptive methods and subgrid scale modeling. The basic idea is to resolve anisotropic, supersonic flow features (shocks, collapsing regions) using AMR (AdaptiveMesh Refinement), whereas length scales dominated by isotropic, subsonic turbulence are described by a subgrid scale model. Implementing FEARLESS into the open source AMR code Enzo, we successfully tested the new method both in hydrodynamic and selfgravitating turbulence simulations. In the next phase of the project, FEARLESS will be applied to star formation and galactic disk simulations."],["dc.identifier.doi","10.1007/978-3-540-69182-2_7"],["dc.identifier.scopus","2-s2.0-84897691411"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/66904"],["dc.identifier.url","http://www.scopus.com/inward/record.url?eid=2-s2.0-84897691411&partnerID=MN8TOARS"],["dc.language.iso","en"],["dc.publisher","Kluwer Academic Publishers"],["dc.relation.conference","2007 3rd Joint HLRB and KONWIHR Result and Reviewing Workshop"],["dc.relation.eventend","2007-12-04"],["dc.relation.eventlocation","Garching/Munich"],["dc.relation.eventstart","2007-12-03"],["dc.relation.isbn","978-354069181-5"],["dc.relation.ispartof","High Performance Computing in Science and Engineering, Garching/Munich 2007 - Transactions of the 3rd Joint HLRB and KONWIHR Status and Result Workshop"],["dc.title","Star Formation in the Turbulent Interstellar Medium and Its Implications on Galaxy Evolution"],["dc.type","conference_paper"],["dc.type.internalPublication","no"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","363"],["dc.bibliographiccitation.lastpage","384"],["dc.contributor.author","Hillebrandt, W."],["dc.contributor.author","Reinecke, M."],["dc.contributor.author","Schmidt, W."],["dc.contributor.author","Röpke, F. K."],["dc.contributor.author","Travaglio, C."],["dc.contributor.author","Niemeyer, J. C."],["dc.contributor.editor","Warnecke, G."],["dc.date.accessioned","2020-07-09T08:04:23Z"],["dc.date.available","2020-07-09T08:04:23Z"],["dc.date.issued","2005"],["dc.description.abstract","Type Ia supernovae, i.e. stellar explosions which do not have hydrogen in their spectra, but intermediate-mass elements such as silicon, calcium, cobalt, and iron, have recently received considerable attention because it appears that they can be used as ”standard candles” to measure cosmic distances out to billions of light years away from us. Observations of type Ia supernovae seem to indicate that we are living in a universe that started to accelerate its expansion when it was about half its present age. These conclusions rest primarily on phenomenological models which, however, lack proper theoretical understanding, mainly because the explosion process, initiated by thermonuclear fusion of carbon and oxygen into heavier elements, is difficult to simulate even on supercomputers. Here, we investigate a new way of modeling turbulent thermonuclear deflagration fronts in white dwarfs undergoing a type Ia supernova explosion. Our approach is based on a level set method which treats the front as a mathematical discontinuity and allows for full coupling between the front geometry and the flow field. New results of the method applied to the problem of type Ia supernovae are obtained. It is shown that in 2-D with high spatial resolution and a physically motivated subgrid scale model for the nuclear flames numerically “converged” results can be obtained, but for most initial conditions the stars do not explode. In contrast, simulations in 3-D do give the desired explosions and many of their properties, such as the explosion energies, lightcurves and nucleosynthesis products, are in very good agreement with observed type Ia supernovae."],["dc.identifier.doi","10.1007/3-540-27907-5_16"],["dc.identifier.scopus","2-s2.0-35348925773"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/66897"],["dc.identifier.url","http://www.scopus.com/inward/record.url?eid=2-s2.0-35348925773&partnerID=MN8TOARS"],["dc.language.iso","en"],["dc.publisher","Springer"],["dc.publisher.place","Berlin, Heidelberg"],["dc.relation.doi","10.1007/3-540-27907-5"],["dc.relation.eisbn","978-3-540-27907-5"],["dc.relation.isbn","978-3-540-24834-7"],["dc.relation.ispartof","Analysis and Numerics for Conservation Laws"],["dc.title","Simulations of turbulent thermonuclear burning in type Ia supernovae"],["dc.type","book_chapter"],["dc.type.internalPublication","no"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","L3"],["dc.bibliographiccitation.firstpage","L3"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","The Astrophysical Journal"],["dc.bibliographiccitation.volume","772"],["dc.contributor.author","Latif, A. H. M. Mahbub"],["dc.contributor.author","Schleicher, Dominik R. G."],["dc.contributor.author","Schmidt, W."],["dc.contributor.author","Niemeyer, J."],["dc.date.accessioned","2018-11-07T09:22:19Z"],["dc.date.accessioned","2020-07-21T06:05:19Z"],["dc.date.available","2018-11-07T09:22:19Z"],["dc.date.available","2020-07-21T06:05:19Z"],["dc.date.issued","2013"],["dc.description.abstract","Population III stars forming in the infant universe at z = 30 heralded the end of the cosmic dark ages. They are presumed to be assembled in the so-called minihalos with virial temperatures of a few thousand K where collapse is triggered by molecular hydrogen cooling. A central question concerns their final masses, and whether fragmentation occurs during their formation. While studies employing Lagrangian codes suggest fragmentation via a self-gravitating disk, recent high-resolution simulations indicated that disk formation is suppressed. Here we report the first high-resolution large-eddy simulations performed with the Eulerian grid-based code Enzo following the evolution beyond the formation of the first peak to investigate the accretion of the central massive clump and potential fragmentation. For a total of three halos, we see that a disk forms around the first clump. The central clump reaches similar to 10 solar masses after 40 yr, while subsequent accretion is expected at a rate of 10(-2) solar masses per year. In one of these halos, additional clumps form as a result of fragmentation which proceeds at larger scales. We note that subgrid-scale (SGS) turbulence yields relevant contributions to the stability of the protostellar disks. Both with and without the SGS model, the disk evolution appears rather stable during the timescale considered here. We conclude that the first protostar may reach masses up to 40-100 M-circle dot, which are only limited by the effect of radiative feedback."],["dc.description.sponsorship","Deutsche Forschungsgemeinschaft (DFG) [SFB 963/1, A12]; HLRN [nip00029]"],["dc.identifier.doi","10.1088/2041-8205/772/1/L3"],["dc.identifier.isi","000321696500003"],["dc.identifier.scopus","2-s2.0-84880624699"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/29315"],["dc.identifier.url","http://www.scopus.com/inward/record.url?eid=2-s2.0-84880624699&partnerID=MN8TOARS"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.relation.eissn","2041-8213"],["dc.relation.issn","2041-8205"],["dc.title","The formation of massive population III stars in the presence of turbulence"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","431"],["dc.bibliographiccitation.issue","1-4 SPEC. ISS."],["dc.bibliographiccitation.journal","Nuclear Physics. A, Nuclear and Hadronic Physics"],["dc.bibliographiccitation.lastpage","438"],["dc.bibliographiccitation.volume","758"],["dc.contributor.author","Niemeyer, J. C."],["dc.contributor.author","Schmidt, W."],["dc.contributor.author","Klingenberg, C."],["dc.date.accessioned","2020-07-22T09:33:34Z"],["dc.date.available","2020-07-22T09:33:34Z"],["dc.date.issued","2005"],["dc.description.abstract","We present an overview of the current state of multidimensional modelling of type Ia supernovae and an example for surprising consequences of impoving the physics of the model. In this case, an improved handling of subgrid scale turbulence gives rise to lower burning rates and a decreased global energy release. While this result is too preliminary to be interpreted quantitatively, it shows that much work remains to be done before the turbulent deflagration model can be declared to be understood and/or insufficient to explain normal type Ia supernovae."],["dc.identifier.doi","10.1016/j.nuclphysa.2005.05.080"],["dc.identifier.scopus","2-s2.0-20944432720"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/67385"],["dc.identifier.url","http://www.scopus.com/inward/record.url?eid=2-s2.0-20944432720&partnerID=MN8TOARS"],["dc.language.iso","en"],["dc.relation.issn","0375-9474"],["dc.title","Modelling turbulent deflagrations in type Ia supernovae"],["dc.type","journal_article"],["dc.type.internalPublication","no"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","701"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","Monthly Notices of the Royal Astronomical Society"],["dc.bibliographiccitation.lastpage","719"],["dc.bibliographiccitation.volume","459"],["dc.contributor.author","Schmidt, W."],["dc.contributor.author","Engels, J. F."],["dc.contributor.author","Niemeyer, Jens"],["dc.contributor.author","Almgren, A. S."],["dc.date.accessioned","2018-11-07T10:12:48Z"],["dc.date.accessioned","2020-07-16T13:44:02Z"],["dc.date.available","2018-11-07T10:12:48Z"],["dc.date.available","2020-07-16T13:44:02Z"],["dc.date.issued","2016"],["dc.description.abstract","The gas in galaxy clusters is heated by shock compression through accretion (outer shocks) and mergers (inner shocks). These processes additionally produce turbulence. To analyse the relation between the thermal and turbulent energies of the gas under the influence of non-adiabatic processes, we performed numerical simulations of cosmic structure formation in a box of 152 Mpc comoving size with radiative cooling, UV background, and a subgrid scale model for numerically unresolved turbulence. By smoothing the gas velocities with an adaptive Kalman filter, we are able to estimate bulk flows toward cluster cores. This enables us to infer the velocity dispersion associated with the turbulent fluctuation relative to the bulk flow. For halos with masses above 0^{13}\\,M_\\odot$, we find that the turbulent velocity dispersions averaged over the warm-hot intergalactic medium (WHIM) and the intracluster medium (ICM) are approximately given by powers of the mean gas temperatures with exponents around 0.5, corresponding to a roughly linear relation between turbulent and thermal energies and transonic Mach numbers. However, turbulence is only weakly correlated with the halo mass. Since the power-law relation is stiffer for the WHIM, the turbulent Mach number tends to increase with the mean temperature of the WHIM. This can be attributed to enhanced turbulence production relative to dissipation in particularly hot and turbulent clusters."],["dc.identifier.doi","10.1093/mnras/stw632"],["dc.identifier.isi","000376386600056"],["dc.identifier.scopus","2-s2.0-84970006648"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/67199"],["dc.identifier.url","http://www.scopus.com/inward/record.url?eid=2-s2.0-84970006648&partnerID=MN8TOARS"],["dc.language.iso","en"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.relation.eissn","1365-2966"],["dc.relation.issn","0035-8711"],["dc.title","Hot and turbulent gas in clusters"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dspace.entity.type","Publication"]]