Schleicher, Dominik R. G.

[["dc.bibliographiccitation.firstpage","1676"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","Monthly Notices of the Royal Astronomical Society"],["dc.bibliographiccitation.lastpage","1676"],["dc.bibliographiccitation.volume","504"],["dc.contributor.author","Navarrete, Felipe H"],["dc.contributor.author","Schleicher, Dominik R G"],["dc.contributor.author","Käpylä, Petri J"],["dc.contributor.author","Schober, Jennifer"],["dc.contributor.author","Völschow, Marcel"],["dc.contributor.author","Mennickent, Ronald E"],["dc.date.accessioned","2021-08-12T07:45:14Z"],["dc.date.available","2021-08-12T07:45:14Z"],["dc.date.issued","2021"],["dc.identifier.doi","10.1093/mnras/stab836"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/88402"],["dc.language.iso","en"],["dc.notes.intern","DOI Import GROB-448"],["dc.relation.eissn","1365-2966"],["dc.relation.iserratumof","/handle/2/75283"],["dc.relation.issn","0035-8711"],["dc.title","Erratum: Magnetohydrodynamical origin of eclipsing time variations in post-common-envelope binaries for solar mass secondaries"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.subtype","erratum_ja"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","2181"],["dc.bibliographiccitation.issue","3"],["dc.bibliographiccitation.journal","Monthly Notices of the Royal Astronomical Society"],["dc.bibliographiccitation.lastpage","2187"],["dc.bibliographiccitation.volume","441"],["dc.contributor.author","Bovino, Stefano"],["dc.contributor.author","Latif, A. H. M. Mahbub"],["dc.contributor.author","Grassi, T."],["dc.contributor.author","Schleicher, Dominik R. G."],["dc.date.accessioned","2018-11-07T09:38:12Z"],["dc.date.available","2018-11-07T09:38:12Z"],["dc.date.issued","2014"],["dc.description.abstract","While Population III (Pop III) stars are typically thought to be massive, pathways towards lower mass Pop III stars may exist when the cooling of the gas is particularly enhanced. A possible route is enhanced HD cooling during the merging of dark-matter haloes. The mergers can lead to a high ionization degree catalysing the formation of HD molecules and may cool the gas down to the cosmic microwave background temperature. In this paper, we investigate the merging of mini-haloes with masses of a few 10(5) M-aS (TM) and explore the feasibility of this scenario. We have performed three-dimensional cosmological hydrodynamics calculations with the enzo code, solving the thermal and chemical evolution of the gas by employing the astrochemistry package krome. Our results show that the HD abundance is increased by two orders of magnitude compared to the no-merging case and the halo cools down to similar to 60 K triggering fragmentation. Based on Jeans estimates, the expected stellar masses are about 10 M-aS (TM). Our findings show that the merging scenario is a potential pathway for the formation of low-mass stars."],["dc.identifier.doi","10.1093/mnras/stu714"],["dc.identifier.isi","000338763600027"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/33019"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Oxford Univ Press"],["dc.relation.issn","1365-2966"],["dc.relation.issn","0035-8711"],["dc.title","Dark-matter halo mergers as a fertile environment for low-mass Population III star formation"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A142"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","556"],["dc.contributor.author","Schleicher, Dominik R. G."],["dc.contributor.author","Beck, Rainer"],["dc.date.accessioned","2018-11-07T09:21:42Z"],["dc.date.available","2018-11-07T09:21:42Z"],["dc.date.issued","2013"],["dc.description.abstract","Context. Observations of galaxies up to z similar to 2 show a tight correlation between far-infrared and radio continuum emission, suggesting a relation between star formation activity and magnetic fields in the presence of cosmic rays. Aims. We explain the far-infrared - radio continuum correlation by relating star formation and magnetic field strength in terms of turbulent magnetic field amplification, where turbulence is injected by supernova explosions from massive stars. We assess the potential evolution of this relation at high redshift, and explore the impact on the far-infrared - radio correlation. Methods. We calculate the expected amount of turbulence in galaxies based on their star formation rates, and infer the expected magnetic field strength due to turbulent dynamo amplification. We calculate the timescales for cosmic ray energy losses via synchrotron emission, inverse Compton scattering, ionization and bremsstrahlung emission, probing up to which redshift strong synchrotron emission can be maintained. Results. We find that the correlation between star formation rate and magnetic field strength in the local Universe can be understood as a result of turbulent magnetic field amplification. The ratio of radio to far-infrared surface brightness is expected to increase with total field strength. A continuation of the correlation is expected towards high redshifts. If the typical gas density in the interstellar medium increases at high z, we expect an increase of the magnetic field strength and the radio emission, as indicated by current observations. Such an increase would imply a modification, but not a breakdown of the far-infrared -radio correlation. We expect a breakdown at the redshift when inverse Compton losses start dominating over synchrotron emission. For a given star formation surface density, we calculate the redshift where the far-infrared -radio correlation will break down, yielding z similar to (Sigma(SFR)/0.0045 M-circle dot kpc(-2) yr(-1))(1/( 6-alpha/2)). In this relation, the parameter a describes the evolution of the characteristic ISM density in galaxies as (1 + z)(alpha). We note that observed frequencies of 1-10 GHz are particularly well-suited to explore this relation, as bremsstrahlung losses could potentially dominate at low frequencies. Conclusions. Both the possible raise of the radio emission at high redshift and the final breakdown of the far-infrared -radio correlation at a critical redshift will be probed by the Square Kilometre Array (SKA) and its pathfinders, while the typical ISM density in galaxies will be probed with ALMA. The combined measurements will thus allow a verification of the model proposed here."],["dc.identifier.doi","10.1051/0004-6361/201321707"],["dc.identifier.isi","000323893500142"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/10870"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/29171"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","A new interpretation of the far-infrared - radio correlation and the expected breakdown at high redshift"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A22"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","572"],["dc.contributor.author","van Borm, C."],["dc.contributor.author","Bovino, Stefano"],["dc.contributor.author","Latif, A. H. M. Mahbub"],["dc.contributor.author","Schleicher, Dominik R. G."],["dc.contributor.author","Spaans, M."],["dc.contributor.author","Grassi, T."],["dc.date.accessioned","2018-11-07T09:31:57Z"],["dc.date.available","2018-11-07T09:31:57Z"],["dc.date.issued","2014"],["dc.description.abstract","Context. The seeds of the first supermassive black holes may have resulted from the direct collapse of hot primordial gas in greater than or similar to 10(4) K haloes, forming a supermassive or quasi- star as an intermediate stage. Aims. We explore the formation of a protostar resulting from the collapse of primordial gas in the presence of a strong Lyman- Werner radiation background. Particularly, we investigate the impact of turbulence and rotation on the fragmentation behaviour of the gas cloud. We accomplish this goal by varying the initial turbulent and rotational velocities. Methods. We performed 3D adaptive mesh refinement simulations with a resolution of 64 cells per Jeans length using the ENZO code, simulating the formation of a protostar up to unprecedentedly high central densities of 10(21) cm(-3) and spatial scales of a few solar radii. To achieve this goal, we employed the KROME package to improve modelling of the chemical and thermal processes. Results. We find that the physical properties of the simulated gas clouds become similar on small scales, irrespective of the initial amount of turbulence and rotation. After the highest level of refinement was reached, the simulations have been evolved for an additional similar to 5 freefall times. A single bound clump with a radius of 2 x 10(-2) AU and a mass of similar to 7 x 10(-2) M fi is formed at the end of each simulation, marking the onset of protostar formation. No strong fragmentation is observed by the end of the simulations, regardless of the initial amount of turbulence or rotation, and high accretion rates of a few solar masses per year are found. Conclusions. Given such high accretion rates, a quasi- star of 105 M fi is expected to form within 105 years."],["dc.description.sponsorship","Deutsche Forschungsgemeinschaft (DFG) [SFB 963 / 1]"],["dc.identifier.doi","10.1051/0004-6361/201424658"],["dc.identifier.fs","609689"],["dc.identifier.isi","000346101700037"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/11406"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/31640"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","1432-0746"],["dc.relation.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","Effects of turbulence and rotation on protostar formation as a precursor of massive black holes"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","1"],["dc.bibliographiccitation.issue","1-4"],["dc.bibliographiccitation.journal","Space Science Reviews"],["dc.bibliographiccitation.lastpage","35"],["dc.bibliographiccitation.volume","166"],["dc.contributor.author","Ryu, D."],["dc.contributor.author","Schleicher, Dominik R. G."],["dc.contributor.author","Treumann, Rudolf A."],["dc.contributor.author","Tsagas, Christos G."],["dc.contributor.author","Widrow, Lawrence M."],["dc.date.accessioned","2018-11-07T09:10:44Z"],["dc.date.available","2018-11-07T09:10:44Z"],["dc.date.issued","2012"],["dc.description.abstract","Magnetic fields appear to be ubiquitous in astrophysical environments. Their existence in the intracluster medium is established through observations of synchrotron emission and Faraday rotation. On the other hand, the nature of magnetic fields outside of clusters, where observations are scarce and controversial, remains largely unknown. In this chapter, we review recent developments in our understanding of the nature and origin of intergalactic magnetic fields, and in particular, intercluster fields. A plausible scenario for the origin of galactic and intergalactic magnetic fields is for seed fields, created in the early universe, to be amplified by turbulent flows induced during the formation of the large scale structure. We present several mechanisms for the generation of seed fields both before and after recombination. We then discuss the evolution and role of magnetic fields during the formation of the first starts. We describe the turbulent amplification of seed fields during the formation of large scale structure and the nature of the magnetic fields that arise. Finally, we discuss implications of intergalactic magnetic fields."],["dc.identifier.doi","10.1007/s11214-011-9839-z"],["dc.identifier.isi","000303862200001"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/26560"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Springer"],["dc.relation.issn","1572-9672"],["dc.relation.issn","0038-6308"],["dc.title","Magnetic Fields in the Large-Scale Structure of the Universe"],["dc.type","review"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["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.artnumber","A46"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","545"],["dc.contributor.author","Hocuk, S."],["dc.contributor.author","Schleicher, Dominik R. G."],["dc.contributor.author","Spaans, M."],["dc.contributor.author","Cazaux, S."],["dc.date.accessioned","2018-11-07T09:06:06Z"],["dc.date.available","2018-11-07T09:06:06Z"],["dc.date.issued","2012"],["dc.description.abstract","Star formation in the centers of galaxies is thought to yield massive stars with a possibly top-heavy stellar mass distribution. It is likely that magnetic fields play a crucial role in the distribution of stellar masses inside star-forming molecular clouds. In this context, we explore the effects of magnetic fields, with a typical field strength of 38 mu G, such as in RCW 38, and a field strength of 135 mu G, similar to NGC 2024 and the infrared dark cloud G28.34+0.06, on the initial mass function (IMF) near (<= 10 pc) a 10(7) solar mass black hole. Using these conditions, we perform a series of numerical simulations with the hydrodynamical code FLASH to elucidate the impact of magnetic fields on the IMF and the star-formation efficiency (SFE) emerging from an 800 solar mass cloud. We find that the collapse of a gravitationally unstable molecular cloud is slowed down with increasing magnetic field strength and that stars form along the field lines. The total number of stars formed during the simulations increases by a factor of 1.5-2 with magnetic fields. The main component of the IMF has a lognormal shape, with its peak shifted to sub-solar (<= 0.3 M-circle dot) masses in the presence of magnetic fields, due to a decrease in the accretion rates from the gas reservoir. In addition, we see a top-heavy, nearly flat IMF above similar to 2 solar masses, from regions that were supported by magnetic pressure until high masses are reached. We also consider the effects of X-ray irradiation if the central black hole is active. X-ray feedback inhibits the formation of sub-solar masses and decreases the SFEs even further. Thus, the second contribution is no longer visible. We conclude that magnetic fields potentially change the SFE and the IMF both in active and inactive galaxies, and need to be taken into account in such calculations. The presence of a flat component of the IMF would be a particularly relevant signature for the importance of magnetic fields, as it is usually not found in hydrodynamical simulations."],["dc.identifier.doi","10.1051/0004-6361/201219628"],["dc.identifier.fs","596754"],["dc.identifier.isi","000309254900046"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9614"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/25480"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","The impact of magnetic fields on the IMF in star-forming clouds near a supermassive black hole"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","37"],["dc.bibliographiccitation.issue","1-4"],["dc.bibliographiccitation.journal","Space Science Reviews"],["dc.bibliographiccitation.lastpage","70"],["dc.bibliographiccitation.volume","166"],["dc.contributor.author","Widrow, Lawrence M."],["dc.contributor.author","Ryu, Dongsu"],["dc.contributor.author","Schleicher, Dominik R. G."],["dc.contributor.author","Subramanian, Kandaswamy"],["dc.contributor.author","Tsagas, Christos G."],["dc.contributor.author","Treumann, Rudolf A."],["dc.date.accessioned","2018-11-07T09:10:45Z"],["dc.date.available","2018-11-07T09:10:45Z"],["dc.date.issued","2012"],["dc.description.abstract","We review current ideas on the origin of galactic and extragalactic magnetic fields. We begin by summarizing observations of magnetic fields at cosmological redshifts and on cosmological scales. These observations translate into constraints on the strength and scale magnetic fields must have during the early stages of galaxy formation in order to seed the galactic dynamo. We examine mechanisms for the generation of magnetic fields that operate prior during inflation and during subsequent phase transitions such as electroweak symmetry breaking and the quark-hadron phase transition. The implications of strong primordial magnetic fields for the reionization epoch as well as the first generation of stars are discussed in detail. The exotic, early-Universe mechanisms are contrasted with astrophysical processes that generate fields after recombination. For example, a Biermann-type battery can operate in a proto-galaxy during the early stages of structure formation. Moreover, magnetic fields in either an early generation of stars or active galactic nuclei can be dispersed into the intergalactic medium."],["dc.identifier.doi","10.1007/s11214-011-9833-5"],["dc.identifier.isi","000303862200002"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/26562"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Springer"],["dc.relation.issn","1572-9672"],["dc.relation.issn","0038-6308"],["dc.title","The First Magnetic Fields"],["dc.type","review"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","77"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","Monthly Notices of the Royal Astronomical Society"],["dc.bibliographiccitation.lastpage","87"],["dc.bibliographiccitation.volume","449"],["dc.contributor.author","Latif, A. H. M. Mahbub"],["dc.contributor.author","Schleicher, Dominik R. G."],["dc.date.accessioned","2018-11-07T09:57:35Z"],["dc.date.available","2018-11-07T09:57:35Z"],["dc.date.issued","2015"],["dc.description.abstract","Our understanding of Population III star formation is still in its infancy. They are formed in dark matter minihaloes of 10(5)-10(6) M-circle dot at z = 20-30. Recent high-resolution cosmological simulations show that a protostellar disc forms as a consequence of gravitational collapse and fragments into multiple clumps. However, it is not entirely clear if these clumps will be able to survive to form multiple stars as simulations are unable to follow the disc evolution for longer times. In this study, we employ a simple analytical model to derive the properties of marginally stable steady-state discs. Our results show that the stability of the disc depends on the critical value of the viscous parameter alpha. For alpha(crit) = 1, the disc is stable for an accretion rate of <= 10(-3) M-circle dot yr(-1) and becomes unstable at radii about >= 100 au in the presence of an accretion rate of 10(-2) M-circle dot yr(-1). For 0.06 < alpha(crit) < 1, the disc can be unstable for both accretion rates. The comparison of the migration and the Kelvin-Helmholtz time-scales shows that clumps are expected to migrate inwards before reaching the main sequence. Furthermore, in the presence of a massive central star, the clumps within the central 1 au will be tidally disrupted. We also find that UV feedback from the central star is unable to disrupt the disc, and that photoevaporation becomes important only once the accretion rate has dropped to 2 x 10(-4) M-circle dot yr(-1). As a result, the central star may reach a mass of 100 M-circle dot or even higher."],["dc.description.sponsorship","European Research Council under the European Community [614199]"],["dc.identifier.doi","10.1093/mnras/stu2573"],["dc.identifier.isi","000355345600007"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/37194"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Oxford Univ Press"],["dc.relation.issn","1365-2966"],["dc.relation.issn","0035-8711"],["dc.title","Disc fragmentation and the formation of Population III stars"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","2989"],["dc.bibliographiccitation.issue","4"],["dc.bibliographiccitation.journal","Monthly Notices of the Royal Astronomical Society"],["dc.bibliographiccitation.lastpage","2996"],["dc.bibliographiccitation.volume","436"],["dc.contributor.author","Latif, A. H. M. Mahbub"],["dc.contributor.author","Schleicher, Dominik R. G."],["dc.contributor.author","Schmidt, Wolfram"],["dc.contributor.author","Niemeyer, J. C."],["dc.date.accessioned","2018-11-07T09:17:04Z"],["dc.date.accessioned","2020-07-09T08:43:58Z"],["dc.date.available","2018-11-07T09:17:04Z"],["dc.date.available","2020-07-09T08:43:58Z"],["dc.date.issued","2013"],["dc.description.abstract","Black holes of a billion solar masses are observed in the infant universe a few hundred million years after the Big Bang. The direct collapse of protogalactic gas clouds in primordial halos with $\\rm T_{vir} \\geq 10^{4} K$ provides the most promising way to assemble massive black holes. In this study, we aim to determine the characteristic mass scale of seed black holes and the time evolution of the accretion rates resulting from the direct collapse model. We explore the formation of supermassive black holes via cosmological large eddy simulations (LES) by employing sink particles and following their evolution for twenty thousand years after the formation of the first sink. As the resulting protostars were shown to have cool atmospheres in the presence of strong accretion, we assume here that UV feedback is negligible during this calculation. We confirm this result in a comparison run without sinks. Our findings show that black hole seeds with characteristic mass of $\\rm 10^{5} M_{\\odot}$ are formed in the presence of strong Lyman Werner flux which leads to an isothermal collapse. The characteristic mass is a about two times higher in LES compared to the implicit large eddy simulations (ILES). The accretion rates increase with time and reach a maximum value of 10 $\\rm M_{\\odot}/yr$ after $\\rm 10^{4}$ years. Our results show that the direct collapse model is clearly feasible as it provides the expected mass of the seed black holes."],["dc.identifier.doi","10.1093/mnras/stt1786"],["dc.identifier.isi","000327798100009"],["dc.identifier.scopus","2-s2.0-84889036204"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/66907"],["dc.identifier.url","http://www.scopus.com/inward/record.url?eid=2-s2.0-84889036204&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","The characteristic black hole mass resulting from direct collapse in the early Universe"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dspace.entity.type","Publication"]]