Schleicher, Dominik R. G.

[["dc.bibliographiccitation.firstpage","2"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","Monthly Notices of the Royal Astronomical Society"],["dc.bibliographiccitation.lastpage","17"],["dc.bibliographiccitation.volume","446"],["dc.contributor.author","Schober, Jennifer"],["dc.contributor.author","Schleicher, Dominik R. G."],["dc.contributor.author","Klessen, Ralf S."],["dc.date.accessioned","2018-11-07T10:03:45Z"],["dc.date.available","2018-11-07T10:03:45Z"],["dc.date.issued","2015"],["dc.description.abstract","The evolution of magnetic fields in galaxies is still an open problem in astrophysics. In nearby galaxies the far-infrared-radio correlation indicates the coupling between magnetic fields and star formation. The correlation arises from the synchrotron emission of cosmic ray electrons travelling through the interstellar magnetic fields. However, with an increase of the interstellar radiation field (ISRF), inverse Compton scattering becomes the dominant energy loss mechanism of cosmic ray electrons with a typical emission frequency in the X-ray regime. The ISRF depends on the one hand on the star formation rate and becomes stronger in starburst galaxies, and on the other hand increases with redshift due to the higher temperature of the cosmic microwave background. With a model for the star formation rate of galaxies, the ISRF, and the cosmic ray spectrum, we can calculate the expected X-ray luminosity resulting from the inverse Compton emission. Except for galaxies with an active galactic nucleus the main additional contribution to the X-ray luminosity comes from X-ray binaries. We estimate this contribution with an analytical model as well as with an observational relation, and compare it to the pure inverse Compton luminosity. Using data from the Chandra Deep Field Survey and far-infrared observations from Atacama Large Millimeter/Submillimeter Array, we then determine upper limits for the cosmic ray energy. Assuming that the magnetic energy in a galaxy is in equipartition with the energy density of the cosmic rays, we obtain upper limits for the magnetic field strength. Our results suggest that the mean magnetic energy of young galaxies is similar to the one in local galaxies. This points towards an early generation of galactic magnetic fields, which is in agreement with current dynamo evolution models."],["dc.identifier.doi","10.1093/mnras/stu1999"],["dc.identifier.isi","347518300001"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/38543"],["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","X-ray emission from star-forming galaxies - signatures of cosmic rays and magnetic fields"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","3112"],["dc.bibliographiccitation.issue","4"],["dc.bibliographiccitation.journal","Monthly Notices of the Royal Astronomical Society"],["dc.bibliographiccitation.lastpage","3126"],["dc.bibliographiccitation.volume","442"],["dc.contributor.author","Naumann, Peter-Thomas"],["dc.contributor.author","Schleicher, Dominik R. G."],["dc.contributor.author","Smith, Rowan J."],["dc.contributor.author","Schmidt, Wolfram"],["dc.contributor.author","Klessen, Ralf S."],["dc.date.accessioned","2018-11-07T09:36:29Z"],["dc.date.available","2018-11-07T09:36:29Z"],["dc.date.issued","2014"],["dc.description.abstract","Low-metallicity star formation poses a central problem of cosmology, as it determines the characteristic mass scale and distribution for the first and second generations of stars forming in our Universe. Here, we present a comprehensive investigation assessing the relative impact of metals and magnetic fields, which may both be present during low-metallicity star formation. We show that the presence of magnetic fields generated via the small-scale dynamo stabilizes the protostellar disc and provides some degree of support against fragmentation. In the absence of magnetic fields, the fragmentation time-scale in our model decreases by a factor of similar to 10 at the transition from Z = 0 to Z > 0, with subsequently only a weak dependence on metallicity. Similarly, the accretion time-scale of the cluster is set by the large-scale dynamics rather than the local thermodynamics. In the presence of magnetic fields, the primordial disc can become completely stable, therefore forming only one central fragment. At Z > 0, the number of fragments is somewhat reduced in the presence of magnetic fields, though the shape of the mass spectrum is not strongly affected in the limits of the statistical uncertainties. The fragmentation time-scale, however, increases by roughly a factor of 3 in the presence of magnetic fields. Indeed, our results indicate comparable fragmentation time-scales in primordial runs without magnetic fields and Z > 0 runs with magnetic fields."],["dc.identifier.doi","10.1093/mnras/stu1097"],["dc.identifier.isi","000339924900023"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/32628"],["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","Low-metallicity star formation: relative impact of metals and magnetic fields"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","99"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","The Astrophysical Journal"],["dc.bibliographiccitation.volume","754"],["dc.contributor.author","Schober, Jennifer"],["dc.contributor.author","Schleicher, Dominik R. G."],["dc.contributor.author","Federrath, Christoph"],["dc.contributor.author","Glover, Simon C. O."],["dc.contributor.author","Klessen, Ralf S."],["dc.contributor.author","Banerjee, Robi"],["dc.date.accessioned","2018-11-07T09:07:49Z"],["dc.date.available","2018-11-07T09:07:49Z"],["dc.date.issued","2012"],["dc.description.abstract","We study the amplification of magnetic fields during the formation of primordial halos. The turbulence generated by gravitational infall motions during the formation of the first stars and galaxies can amplify magnetic fields very efficiently and on short timescales up to dynamically significant values. Using the Kazantsev theory, which describes the so-called small-scale dynamo-a magnetohydrodynamical process converting kinetic energy from turbulence into magnetic energy-we can then calculate the growth rate of the small-scale magnetic field. Our calculations are based on a detailed chemical network and we include non-ideal magnetohydrodynamical effects such as ambipolar diffusion and Ohmic dissipation. We follow the evolution of the magnetic field up to larger scales until saturation occurs on the Jeans scale. Assuming a weak magnetic seed field generated by the Biermann battery process, both Burgers and Kolmogorov turbulence lead to saturation within a rather small density range. Such fields are likely to become relevant after the formation of a protostellar disk and, thus, could influence the formation of the first stars and galaxies in the universe."],["dc.identifier.doi","10.1088/0004-637X/754/2/99"],["dc.identifier.isi","000306666700020"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/25888"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Iop Publishing Ltd"],["dc.relation.issn","0004-637X"],["dc.title","THE SMALL-SCALE DYNAMO AND NON-IDEAL MAGNETOHYDRODYNAMICS IN PRIMORDIAL STAR FORMATION"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","3148"],["dc.bibliographiccitation.issue","4"],["dc.bibliographiccitation.journal","Monthly Notices of the Royal Astronomical Society"],["dc.bibliographiccitation.lastpage","3162"],["dc.bibliographiccitation.volume","423"],["dc.contributor.author","Sur, Sharanya"],["dc.contributor.author","Federrath, Christoph"],["dc.contributor.author","Schleicher, Dominik R. G."],["dc.contributor.author","Banerjee, Robi"],["dc.contributor.author","Klessen, Ralf S."],["dc.date.accessioned","2018-11-07T09:08:37Z"],["dc.date.available","2018-11-07T09:08:37Z"],["dc.date.issued","2012"],["dc.description.abstract","We study the influence of initial conditions on the magnetic field amplification during the collapse of a magnetized gas cloud. We focus on the dependence of the growth and saturation level of the dynamo-generated field on the turbulent properties of the collapsing cloud. In particular, we explore the effect of varying the initial strength and injection scale of turbulence and the initial uniform rotation of the collapsing magnetized cloud. In order to follow the evolution of the magnetic field in both the kinematic and the non-linear regime, we choose an initial field strength of with the magnetic to kinetic energy ratio, Em/Ek 10-4. Both gravitational compression and the small-scale dynamo initially amplify the magnetic field. Further into the evolution, the dynamo-generated magnetic field saturates but the total magnetic field continues to grow because of compression. The saturation of the small-scale dynamo is marked by a change in the slope of B/?2/3 and by a shift in the peak of the magnetic energy spectrum from small scales to larger scales. For the range of initial Mach numbers explored in this study, the dynamo growth rate increases as the Mach number increases from vrms/cs 0.2 to 0.4 and then starts decreasing from vrms/cs 1.0. We obtain saturation values of Em/Ek= 0.20.3 for these runs. Simulations with different initial injection scales of turbulence also show saturation at similar levels. For runs with different initial rotation of the cloud, the magnetic energy saturates at Em/Ek 0.20.4 of the equipartition value. The overall saturation level of the magnetic energy, obtained by varying the initial conditions, is in agreement with previous analytical and numerical studies of small-scale dynamo action where turbulence is driven by an external forcing instead of gravitational collapse."],["dc.identifier.doi","10.1111/j.1365-2966.2012.21100.x"],["dc.identifier.isi","000306003600013"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/26074"],["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","Magnetic field amplification during gravitational collapse - influence of turbulence, rotation and gravitational compression"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","531"],["dc.bibliographiccitation.issue","6"],["dc.bibliographiccitation.journal","Astronomische Nachrichten"],["dc.bibliographiccitation.lastpage","536"],["dc.bibliographiccitation.volume","334"],["dc.contributor.author","Schleicher, Dominik R. G."],["dc.contributor.author","Latif, A. H. M. Mahbub"],["dc.contributor.author","Schober, Jennifer"],["dc.contributor.author","Schmidt, Wolfram"],["dc.contributor.author","Bovino, Stefano"],["dc.contributor.author","Federrath, Christoph"],["dc.contributor.author","Niemeyer, J."],["dc.contributor.author","Banerjee, R."],["dc.contributor.author","Klessen, Ralf S."],["dc.date.accessioned","2018-11-07T09:22:39Z"],["dc.date.accessioned","2020-07-09T08:55:45Z"],["dc.date.available","2018-11-07T09:22:39Z"],["dc.date.available","2020-07-09T08:55:45Z"],["dc.date.issued","2013"],["dc.description.abstract","We explore the amplification of magnetic fields in the high-redshift Universe. For this purpose, we perform high-resolution cosmological simulations following the formation of primordial halos with \\sim10^7 M_solar, revealing the presence of turbulent structures and complex morphologies at resolutions of at least 32 cells per Jeans length. Employing a turbulence subgrid-scale model, we quantify the amount of unresolved turbulence and show that the resulting turbulent viscosity has a significant impact on the gas morphology, suppressing the formation of low-mass clumps. We further demonstrate that such turbulence implies the efficient amplification of magnetic fields via the small-scale dynamo. We discuss the properties of the dynamo in the kinematic and non-linear regime, and explore the resulting magnetic field amplification during primordial star formation. We show that field strengths of \\sim10^{-5} G can be expected at number densities of \\sim5 cm^{-3}."],["dc.identifier.doi","10.1002/asna.201211898"],["dc.identifier.isi","000325862900007"],["dc.identifier.scopus","2-s2.0-84879824861"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/66910"],["dc.identifier.url","http://www.scopus.com/inward/record.url?eid=2-s2.0-84879824861&partnerID=MN8TOARS"],["dc.language.iso","en"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.relation.eissn","0004-6337"],["dc.relation.issn","1521-3994"],["dc.title","Magnetic fields during high redshift structure formation"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","114504"],["dc.bibliographiccitation.issue","11"],["dc.bibliographiccitation.journal","Physical Review Letters"],["dc.bibliographiccitation.volume","107"],["dc.contributor.author","Federrath, Christoph"],["dc.contributor.author","Chabrier, G."],["dc.contributor.author","Schober, Jennifer"],["dc.contributor.author","Banerjee, R."],["dc.contributor.author","Klessen, Ralf S."],["dc.contributor.author","Schleicher, Dominik R. G."],["dc.date.accessioned","2018-11-07T08:51:47Z"],["dc.date.available","2018-11-07T08:51:47Z"],["dc.date.issued","2011"],["dc.description.abstract","We study the growth rate and saturation level of the turbulent dynamo in magnetohydrodynamical simulations of turbulence, driven with solenoidal (divergence-free) or compressive (curl-free) forcing. For models with Mach numbers ranging from 0.02 to 20, we find significantly different magnetic field geometries, amplification rates, and saturation levels, decreasing strongly at the transition from subsonic to supersonic flows, due to the development of shocks. Both extreme types of turbulent forcing drive the dynamo, but solenoidal forcing is more efficient, because it produces more vorticity."],["dc.identifier.doi","10.1103/PhysRevLett.107.114504"],["dc.identifier.isi","000294783900005"],["dc.identifier.pmid","22026677"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/22019"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Amer Physical Soc"],["dc.relation.issn","1079-7114"],["dc.relation.issn","0031-9007"],["dc.title","Mach Number Dependence of Turbulent Magnetic Field Amplification: Solenoidal versus Compressive Flows"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A87"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","560"],["dc.contributor.author","Schober, Jennifer"],["dc.contributor.author","Schleicher, Dominik R. G."],["dc.contributor.author","Klessen, Ralf S."],["dc.date.accessioned","2018-11-07T09:16:53Z"],["dc.date.available","2018-11-07T09:16:53Z"],["dc.date.issued","2013"],["dc.description.abstract","The Universe at present is highly magnetized, with fields of a few 10 5 G and coherence lengths greater than 10 kpc in typical galaxies like the Milky Way. We propose that the magnetic field was already amplified to these values during the formation and the early evolution of galaxies. Turbulence in young galaxies is driven by accretion, as well as by supernova (SN) explosions of the first generation of stars. The small-scale dynamo can convert the turbulent kinetic energy into magnetic energy and amplify very weak primordial seed fields on short timescales. Amplification takes place in two phases: in the kinematic phase the magnetic field grows exponentially, with the largest growth rate on the smallest nonresistive scale. In the following nonlinear phase the magnetic energy is shifted toward larger scales until the dynamo saturates on the turbulent forcing scale. To describe the amplification of the magnetic field quantitatively, we modeled the microphysics in the interstellar medium (ISM) of young galaxies and determined the growth rate of the small-scale dynamo. We estimated the resulting saturation field strengths and dynamo timescales for two turbulent forcing mechanisms: accretion-driven turbulence and SN-driven turbulence. We compare them to the field strength that is reached when only stellar magnetic fields are distributed by SN explosions. We find that the small-scale dynamo is much more efficient in magnetizing the ISM of young galaxies. In the case of accretion-driven turbulence, a magnetic field strength on the order of 10 6 G is reached after a time of 24 270 Myr, while in SN-driven turbulence the dynamo saturates at field strengths of typically 10 5 G after only 4 15 Myr. This is considerably shorter than the Hubble time. Our work can help for understanding why present-day galaxies are highly magnetized."],["dc.identifier.doi","10.1051/0004-6361/201322185"],["dc.identifier.isi","000328754500087"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/10883"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/28038"],["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","Magnetic field amplification in young galaxies"],["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","L28"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","The Astrophysical Journal"],["dc.bibliographiccitation.volume","760"],["dc.contributor.author","Peters, Thomas"],["dc.contributor.author","Schleicher, Dominik R. G."],["dc.contributor.author","Klessen, Ralf S."],["dc.contributor.author","Banerjee, Robi"],["dc.contributor.author","Federrath, Christoph"],["dc.contributor.author","Smith, Rowan J."],["dc.contributor.author","Sur, Sharanya"],["dc.date.accessioned","2018-11-07T09:02:53Z"],["dc.date.available","2018-11-07T09:02:53Z"],["dc.date.issued","2012"],["dc.description.abstract","Stars form by the gravitational collapse of interstellar gas. The thermodynamic response of the gas can be characterized by an effective equation of state. It determines how gas heats up or cools as it gets compressed, and hence plays a key role in regulating the process of stellar birth on virtually all scales, ranging from individual star clusters up to the galaxy as a whole. We present a systematic study of the impact of thermodynamics on gravitational collapse in the context of high-redshift star formation, but argue that our findings are also relevant for present-day star formation in molecular clouds. We consider a polytropic equation of state, P = k rho Gamma, with both sub-isothermal exponents Gamma < 1 and super-isothermal exponents Gamma > 1. We find significant differences between these two cases. For Gamma > 1, pressure gradients slow down the contraction and lead to the formation of a virialized, turbulent core. Weak magnetic fields are strongly tangled and efficiently amplified via the small-scale turbulent dynamo on timescales corresponding to the eddy-turnover time at the viscous scale. For Gamma < 1, on the other hand, pressure support is not sufficient for the formation of such a core. Gravitational contraction proceeds much more rapidly and the flow develops very strong shocks, creating a network of intersecting sheets and extended filaments. The resulting magnetic field lines are very coherent and exhibit a considerable degree of order. Nevertheless, even under these conditions we still find exponential growth of the magnetic energy density in the kinematic regime."],["dc.identifier.doi","10.1088/2041-8205/760/2/L28"],["dc.identifier.isi","000311103000009"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/24778"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Iop Publishing Ltd"],["dc.relation.issn","2041-8205"],["dc.title","THE IMPACT OF THERMODYNAMICS ON GRAVITATIONAL COLLAPSE: FILAMENT FORMATION AND MAGNETIC FIELD AMPLIFICATION"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","066412"],["dc.bibliographiccitation.issue","6"],["dc.bibliographiccitation.journal","PHYSICAL REVIEW E"],["dc.bibliographiccitation.volume","86"],["dc.contributor.author","Schober, Jennifer"],["dc.contributor.author","Schleicher, Dominik R. G."],["dc.contributor.author","Bovino, Stefano"],["dc.contributor.author","Klessen, Ralf S."],["dc.date.accessioned","2018-11-07T09:02:11Z"],["dc.date.available","2018-11-07T09:02:11Z"],["dc.date.issued","2012"],["dc.description.abstract","The present-day Universe is highly magnetized, even though the first magnetic seed fields were most probably extremely weak. To explain the growth of the magnetic field strength over many orders of magnitude, fast amplification processes need to operate. The most efficient mechanism known today is the small-scale dynamo, which converts turbulent kinetic energy into magnetic energy leading to an exponential growth of the magnetic field. The efficiency of the dynamo depends on the type of turbulence indicated by the slope of the turbulence spectrum v(l) proportional to l(I),where v(l) is the eddy velocity at a scale l. We explore turbulent spectra ranging from incompressible Kolmogorov turbulence with I = 1/3 to highly compressible Burgers turbulence with I = 1/2. In this work, we analyze the properties of the small-scale dynamo for low magnetic Prandtl numbers Pm, which denotes the ratio of the magnetic Reynolds number, Rm, to the hydrodynamical one, Re. We solve the Kazantsev equation, which describes the evolution of the small-scale magnetic field, using the WKB approximation. In the limit of low magnetic Prandtl numbers, the growth rate is proportional to Rm((1-I)/(1+I)). We furthermore discuss the critical magnetic Reynolds number Rm(crit), which is required for small-scale dynamo action. The value of Rm(crit) is roughly 100 for Kolmogorov turbulence and 2700 for Burgers. Furthermore, we discuss that Rm(crit) provides a stronger constraint in the limit of low Pm than it does for large Pm. We conclude that the small-scale dynamo can operate in the regime of low magnetic Prandtl numbers if the magnetic Reynolds number is large enough. Thus, the magnetic field amplification on small scales can take place in a broad range of physical environments and amplify week magnetic seed fields on short time scales. DOI: 10.1103/PhysRevE.86.066412"],["dc.identifier.doi","10.1103/PhysRevE.86.066412"],["dc.identifier.isi","000312838400007"],["dc.identifier.pmid","23368064"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/24617"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Amer Physical Soc"],["dc.relation.issn","1539-3755"],["dc.title","Small-scale dynamo at low magnetic Prandtl numbers"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","154"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","The Astrophysical Journal"],["dc.bibliographiccitation.volume","761"],["dc.contributor.author","Smith, Rowan J."],["dc.contributor.author","Iocco, Fabio"],["dc.contributor.author","Glover, Simon C. O."],["dc.contributor.author","Schleicher, Dominik R. G."],["dc.contributor.author","Klessen, Ralf S."],["dc.contributor.author","Hirano, Shingo"],["dc.contributor.author","Yoshida, Naoki"],["dc.date.accessioned","2018-11-07T09:02:14Z"],["dc.date.available","2018-11-07T09:02:14Z"],["dc.date.issued","2012"],["dc.description.abstract","We present the first three-dimensional simulations to include the effects of dark matter annihilation feedback during the collapse of primordial minihalos. We begin our simulations from cosmological initial conditions and account for dark matter annihilation in our treatment of the chemical and thermal evolution of the gas. The dark matter is modeled using an analytical density profile that responds to changes in the peak gas density. We find that the gas can collapse to high densities despite the additional energy input from the dark matter. No objects supported purely by dark matter annihilation heating are formed in our simulations. However, we find that dark matter annihilation heating has a large effect on the evolution of the gas following the formation of the first protostar. Previous simulations without dark matter annihilation found that protostellar disks around Population III stars rapidly fragmented, forming multiple protostars that underwent mergers or ejections. When dark matter annihilation is included, however, these disks become stable to radii of 1000 AU or more. In the cases where fragmentation does occur, it is a wide binary that is formed."],["dc.identifier.doi","10.1088/0004-637X/761/2/154"],["dc.identifier.isi","000312090300073"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/24631"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Iop Publishing Ltd"],["dc.relation.issn","0004-637X"],["dc.title","WEAKLY INTERACTING MASSIVE PARTICLE DARK MATTER AND FIRST STARS: SUPPRESSION OF FRAGMENTATION IN PRIMORDIAL STAR FORMATION"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]