#simulateduniverses — Public Fediverse posts
Live and recent posts from across the Fediverse tagged #simulateduniverses, aggregated by home.social.
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A initially uniform magnetic field background (not very realistic!) is shaped across 13 billion years by the progressive formation of cosmic structures (filaments and halos) in an ideal-MHD simulation with ENZO. #SimulatedUniverses #astrophysics #physics
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The hypothetical formation history of a giant radio halo in a cluster of galaxies growing up to 1e15 solar masses in 10 billion years. While colors show the distribution of baryon density in this 20 Mpc^3 region, the contours display radio emission lighted up by the combination of shock acceleration and turbulent re-acceleration over relativistic electrons (Lorentz factor γ>1e4 here).
ENZo simulations combined with #Julia heavy post-processing. #SimulatedUniverses #Astronomy #Physics
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Same cosmic field as this previous one: https://mastodon.social/@franco_vazza/117110448311251058 but here displaying with colors the temperature of baryons.
Orange marks T>>1e6K gas, where baryons become (hypothetically) detectable in X-ray, while green and blue are for phases where the gas is not fully ionized, and filaments can be detectable (again, in principle) only via neutral Hydrogen observations, or else.
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Dancing baryons in the large regions where a cluster of galaxies forms at the crossroads of many filaments in the cosmic web.
Very old ENZO simulation of mine (2009!).
(some structures seem to appear/disappear as they cross the 2d-slab used to produce the map, which is just a fraction of a larger 3d simulated volume(
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Tens of millions of passive Lagrangian tracers to track gas motions in a simulated cluster of galaxies, using a combination of the Enzo code and of D.Wittor's Crater code for tracers.
This mess helps us visualising the actual circulation of particles in cluster of galaxies growing mass for several billions years...plus it's a very neat visualisation of complex dynamic.
#SimulatedUniverses #astrophysics #science -
A simulated radio galaxy ejects bubbles of relativstic electrons in the core of a cluster of galaxies, in an ENZO-MHD simulation I did a few years ago, superbely rendered in 3D by G
Inchingolo together with #Cineca. The yellow particles with tracks follow injected electrons, the magnetic field is in blue while gas temperature is in red. #SimulatedUniverses #astrophysics #physics -
Rich movie of the temperature fluctuations arising in the simulated intracluster medium (left) and their associated shock waves (right, detected in post-processing using a shock finder coded in #Julialang ) in a past ENZO simulation, as part of the PhD work by former student M. Angelinelli. The evolution goes from z=30 to z=0, so it covers more than 13 billions years of cosmic time.
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Continuing from: https://mastodon.social/@franco_vazza/117007687962926827
This version of the "ballet" shows instead the velocity vorticity of baryons (|curl v|=|Nabla times v|), in the rightmost panel.
The vorticity is a quick and reliable proxy for turbulent motions here.
#SimulatedUniverses #astrophysics #astronomy # science
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Similar to yesterday "ballet"
https://mastodon.social/@franco_vazza/117007687962926827This is a 4 views composition which shows the additional information of shock waves (marked by a run-time shock finder) and of the total gas velocity field for the same evolving cluster of galaxies.
I think it nicely shows how many things are going on from the dynamical viewpoint, far away from the centre of clusters, where we get most of detectable X-ray photons.
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A wonderful ballet of baryonic matter properties, in the formation volume of a "small" cluster of galaxies. The isosurfaces are generated with a code by the University of Minnesota (Tom Jones'group) over my ENZO simulations (2017).
Look at how beautifully this tool can trace the very different gas phases (hot & shocked vs cold and low entropy) which are involved in the mass growth of gas in between galaxies!
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Simulated formation of one cluster of galaxies with ENZO-MHD, the right panel shows the steady assembly of baryonic matter, the left panel shows the growing magnetic field in the region.
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Tomography of baryonic density across a 4 Gigaparsec cubic volume, in a new ENZO simulation of the local universe starting from initial conditions derived by from Manticore-Deep, i.e. a bayesian reconstruction of the local distribution of galaxies (mostly 2Mass survey) presented in https://arxiv.org/pdf/2606.10020.
Finding our local neighbourhood (Coma, Virgo, Perseus, the Milky Way..) is like looking for the proverbial needle in the haystack !
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Baryonic density accumulating along one line of sight in a continuous scan for the central 1Gpc^3 volume of (allegedly) the local Universe at z=0, in an ENZO simulation with "constrained initial conditions". The galactic observer should be at very centre of the scan, but I am struggling to identify the usual virgo-coma-centaurus-perseus to understand whether too coarse resolution has altered entirely the formation of such structures
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Complex turbulent patterns generated by the converging flows in a cosmological simulations, at the location where a massive cluster of galaxies form over timescales of billion years. All this gorgeous mess arises from initially very smooth and simple perturbations, which get amplified over time by their gravitational attraction.
Enzo simulation ran on CINECA (Italy) last year.
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Building the Faraday Rotation sky (well, a tiny fraction of it) one layer at a time.
The color coding gives the Rotation Measure along the line of sight, which is a measure of how much can the magnetised screen of plasma in the cosmic web affect the polarised emission by distant sources emitting towards us. -
Three models of primordial magnetic field seeds evolving in the same cubic 10 Megaparsec box. The extreme left is for an inflationary-like spectrum (fluctuations correlated on large scales), the middle is for a causal post-inflationary model (fluctuations only on <<Mpc scales), the extreme right is for a uniform magnetic field. Especially in voids, the memory of the seed structure is retained even until at present.
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Baryon density, baryon temperature and magnetic field strength steadily evolving in the cosmic region where a massive cluster of galaxies forms, in and ENZO magneto-hydrodynamical simulation.
Jesus I have this and other 19 simulations like this since a year and I still need to find the strength to make a paper out of this 😩
But there is the #Wimbledon final today, and the football world cup...
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#SimulatedUniverses Formation and evolution of a cluster of galaxies simulated with adaptive mesh refinement (with the ENZO code), for a total of about 10 billion years in this movie.
the left panel shows the projected baryon density while the right one the baryon temperature.
#astronomy #astrodon #science #physics -
Following https://mastodon.social/@franco_vazza/116888868544158023
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this is the example of a complex dynamical interaction between the radio plasma ejected by an active galactic nucleus and cluster-wide turbulence, which might explain the fuzzy patterns observed in a source like the Treble Clef.It's an ENZO-MHD simulation of a few years ago with own cutomizations in the code to couple AGNs and magnetic fields and cosmic rays.
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A rotation around the central axis of a massive simulated cluster of galaxies, comparing its bremsstrahlung emission (left) and its volume-weighted temperature along the line of sight (right).
We are scrutinising these data to understand whether important small-scale features driven by MHD dynamics can also lead to detectable patterns in X-ray emission (very hard to say at the moment). -
3-dimensional rotation around the z=0 snapshot of a Coma-like cluster of galaxies in an ideal MHD simulation with the ENZO code (Constrained Transport MHD method here). The Left panel shows the X-ray surface brightness while the Right panel shows the magnetic field strength. A lot of filaments resulting from the steady growth of magnetic fields excited by turbulent dynamo here! The resolution of the simulation is 4kpc per cell.
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#SimulatedUniverses a movie showing the development over time of injected cosmic ray electrons by three different mechanisms, color-coded in different ways:
a) blue=cosmic rays from star formation b) red=from shocks c) green=from active galactic nuclei.In reality these relativistic particles are very hard to observe, and it's impossible to know their origin, but with simulations we can refine theoretical ideas.
ENZO simulation run at CINECA.
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A glimpse into the invisibile magnetic threads of the cosmic web:
green=magnetic field strength
red=pressure of thermal gaszoom into a massive galaxy cluster region at z=0 in an ENZO-MHD simulation
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A new version of seeding of B-fields from galaxy formation (star feedback+AGN) in green colors, overlayed to gas density (in red) in recent ENZO simulations run at CINECA.
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Fun workshop at the Institute for Fundamental Physics of the Universe in #Trieste about magnetic fields in high redshift galaxies.
I am presenting tomorrow, here is a flashy view of how magnetic fields (green) may emerge in large-scales structures as a combined effect of amplification of primordial ones and of the additional release by galaxies, in an ENZO simulation.
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collapse of dark matter particles under the effect of self-gravity in a tiny tiny tiny cosmological simulation
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Continuing from https://mastodon.social/@franco_vazza/116770056034131728
Three animated GIFS to compare the volume filling factors of magnetic fields expelled by star formation or AGN or just dynamo at z=2, z=1 an z=0 for the same models
Highest filling factors for AGN, followed by star formation and then dynamo (which is just limited within halos)
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Continuing from this https://mastodon.social/@franco_vazza/116765043276312496
Here is also the comparison with a model in which there is only a primordial week seed field, and a sub-grid recipe to incorporate the effect of turbulent dynamo amplification.
The latter is very crude recipe, yet it shows how in the long run the effect of star formation feedback is very similar to the dynamo in halos, while only AGN feedback (centre) can push a substantial amount of B-fields outside of halos.
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Two #SimulatedUniverses to separately test the effect of feedback (=winds) from star formation or active galactic nuclei (=jets) in expelling magnetic fields from galaxies into the cosmic web.
The left simulation only has the first, the right simulation only has the second.The simulation goes from z=4 to z=0.
Clearly, at least in all my models, while stellar feedback start magnetising first, AGN feedback is by far the dominant one at all scales. -
Structure formation, galaxy evolution and the pollution of cosmic rays and magnetic fields on top of a possible primordial magnetic field background in an Enzo-MHD simulation run on Leonardo at Cinema.
Here is the overlay between the projected temperature of gas (colors) and the radio emitting structures forming in the volume (black countours) from z=10 to z=0 for 85Mpc^3.