448 research outputs found
A refined sub-grid model for black hole accretion and AGN feedback in large cosmological simulations
In large scale cosmological hydrodynamic simulations simplified sub-grid
models for gas accretion onto black holes and AGN feedback are commonly used.
Such models typically depend on various free parameters, which are not well
constrained. We present a new advanced model containing a more detailed
description of AGN feedback, where those parameters reflect the results of
recent observations. The model takes the dependency of these parameters on the
black hole properties into account and describes a continuous transition
between the feedback processes acting in the so-called radio-mode and
quasar-mode. In addition, we implement a more detailed description of the
accretion of gas onto black holes by distinguishing between hot and cold gas
accretion. Our new implementations prevent black holes from gaining too much
mass, particularly at low redshifts so that our simulations are now very
successful in reproducing the observed present-day black hole mass function.
Our new model also suppresses star formation in massive galaxies slightly more
efficiently than many state-of-the-art models. Therefore, the simulations that
include our new implementations produce a more realistic population of
quiescent and star-forming galaxies compared to recent observations, even if
some discrepancies remain. In addition, the baryon conversion efficiencies in
our simulation are - except for the high mass end - consistent with
observations presented in literature over the mass range resolved by our
simulations. Finally, we discuss the significant impact of the feedback model
on the low-luminous end of the AGN luminosity function.Comment: 25 pages, 19 figures. MNRAS accepted. Magneticum website:
http://www.magneticum.or
Origin and properties of dual and offset active galactic nuclei in a cosmological simulation at z=2
In the last few years, it became possible to observationally resolve galaxies
with two distinct nuclei in their centre. For separations smaller than 10kpc,
dual and offset active galactic nuclei (AGN) are distinguished: in dual AGN,
both nuclei are active, whereas in offset AGN only one nucleus is active. To
study the origin of such AGN pairs, we employ a cosmological, hydrodynamic
simulation with a large volume of (182Mpc)^3 from the set of Magneticum
Pathfinder Simulations. The simulation self-consistently produces 35 resolved
black hole (BH) pairs at redshift z=2, with a comoving distance smaller than
10kpc. 14 of them are offset AGN and nine are dual AGN, resulting in a fraction
of (1.2 \pm 0.3)% AGN pairs with respect to the total number of AGN. In this
paper, we discuss fundamental differences between the BH and galaxy properties
of dual AGN, offset AGN and inactive BH pairs and investigate their different
triggering mechanisms. We find that in dual AGN the BHs have similar masses and
the corresponding BH from the less massive progenitor galaxy always accretes
with a higher Eddington ratio. In contrast, in offset AGN the active BH is
typically more massive than its non-active counterpart. Furthermore, dual AGN
in general accrete more gas from the intergalactic medium than offset AGN and
non-active BH pairs. This highlights that merger events, particularly minor
mergers, do not necessarily lead to strong gas inflows and thus, do not always
drive strong nuclear activity.Comment: 17 pages, 18 figures, accepted for publication in MNRAS, website:
http://www.magneticum.or
Connecting Angular Momentum and Galactic Dynamics: The complex Interplay between Spin, Mass, and Morphology
The evolution and distribution of the angular momentum of dark matter (DM)
halos have been discussed in several studies over the past decades. In
particular, the idea arose that angular momentum conservation should allow to
infer the total angular momentum of the entire DM halo from measuring the
angular momentum of the baryonic component, which is populating the center of
the halo, especially for disk galaxies. To test this idea and to understand the
connection between the angular momentum of the DM halo and its galaxy, we use
the Magneticum simulations. We successfully produce populations of spheroidal
and disk galaxies self-consistently. Thus, we are able to study the dependence
of galactic properties on their morphology. We find that (1) the specific
angular momentum of stars in disk and spheroidal galaxies as a function of
their stellar mass compares well with observational results; (2) the specific
angular momentum of the stars in disk galaxies is slightly smaller compared to
the specific angular momentum of the cold gas, in good agreement with
observations; (3) simulations including the baryonic component show a dichotomy
in the specific stellar angular momentum distribution when splitting the
galaxies according to their morphological type (this dichotomy can also be seen
in the spin parameter, where disk galaxies populate halos with slightly larger
spin compared to spheroidal galaxies); (4) disk galaxies preferentially
populate halos in which the angular momentum vector of the DM component in the
central part shows a better alignment to the angular momentum vector of the
entire halo; and (5) the specific angular momentum of the cold gas in disk
galaxies is approximately 40 percent smaller than the specific angular momentum
of the total DM halo and shows a significant scatter.Comment: 25 pages, accepted by ApJ, www.magneticum.or
Machine Learning based Operating Region Extension of Modular Multilevel Converters under Unbalanced Grid Faults
Modelling and simulation of VSC-HVDC connection for offshore wind power plants
Several large offshore wind power plants (WPP)
are planned in the seas around Europe. VSC-HVDC is a suitable
means of integrating such large and distant offshore WPP which
need long submarine cable transmission to the onshore grid.
Recent trend is to use large wind turbine generators with full
scale converters to achieve an optimal operation over a wide
speed range. The offshore grid then becomes very much different
from the conventional power system grid, in the sense that it is
connected to power electronic converters only. A model of the
wind power plant with VSC-HVDC connection is developed in
PSCAD for time-domain dynamic simulation. This paper
presents the modelling and simulation of such a system. A single
line to ground fault has been simulated and fault currents for the
grounded and ungrounded offshore grid system is obtained
through simulation and then compared.Postprint (published version
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