Zobrazeno 1 - 10
of 44
pro vyhledávání: '"Bertram, Erik"'
We run numerical simulations of molecular clouds (MCs), adopting properties similar to those found in the Central Molecular Zone (CMZ) of the Milky Way. For this, we employ the moving mesh code Arepo and perform simulations which account for a simpli
Externí odkaz:
http://arxiv.org/abs/1509.06649
We use the Arepo moving mesh code to simulate the evolution of molecular clouds exposed to a harsh environment similar to that found in the galactic center (GC), in an effort to understand why the star formation efficiency (SFE) of clouds in this env
Externí odkaz:
http://arxiv.org/abs/1505.04403
We employ the Delta-variance analysis and study the turbulent gas dynamics of simulated molecular clouds (MCs). Our models account for a simplified treatment of time-dependent chemistry and the non-isothermal nature of the gas. We investigate simulat
Externí odkaz:
http://arxiv.org/abs/1504.07137
We compute structure functions and Fourier spectra of 2D centroid velocity (CV) maps in order to study the gas dynamics of typical molecular clouds (MCs) in numerical simulations. We account for a simplified treatment of time-dependent chemistry and
Externí odkaz:
http://arxiv.org/abs/1410.6508
Autor:
Bertram, Erik, Shetty, Rahul, Glover, Simon C. O., Klessen, Ralf S., Roman-Duval, Julia, Federrath, Christoph
We use Principal Component Analysis (PCA) to study the gas dynamics in numerical simulations of typical MCs. Our simulations account for the non-isothermal nature of the gas and include a simplified treatment of the time-dependent gas chemistry. We m
Externí odkaz:
http://arxiv.org/abs/1402.2101
We describe a simple method for estimating the vertical column density in Smoothed Particle Hydrodynamics (SPH) simulations of discs. As in the method of Stamatellos et al. (2007), the column density is estimated using pre-computed local quantities a
Externí odkaz:
http://arxiv.org/abs/1207.6513
We study the mass-to-flux ratio (M/\Phi) of clumps and cores in simulations of supersonic, magnetohydrodynamical turbulence for different initial magnetic field strengths. We investigate whether the (M/\Phi)-ratio of core and envelope, R = (M/\Phi)_{
Externí odkaz:
http://arxiv.org/abs/1111.5539