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Disc-halo gas outflows driven by stellar clusters as seen in multiwavelength tracers

We consider the dynamics of and emission from growing superbubbles in astratified interstellar gaseous disc driven by energy release from supernovaeexplosions in stellar clusters with {masses $M_{cl}= 10^5-1.6\times10^6~M_\odot$}. Supernovae are spread randomly within a sphere of $r_c=60$ pc,and inject energy episodically with a specific rate $1/130~M_\odot^{-1}$proportional to the star formation rate (SFR) in the cluster. Models are runfor several values of SFR in the range $0.01$ to $0.1~M_\odot$ yr$^{-1}$, withthe corresponding average surface energy input rate $\sim 0.04-0.4$ ergcm$^{-2}$ s$^{-1}$. We find that the discrete energy injection by isolated SNeare more efficient in blowing superbubbles: asymptotically they reach heightsof up to 3 to 16 kpc for $M_{cl}=10^5-1.6\times 10^5~M_\odot$, correspondingly,and stay filled with a hot and dilute plasma for at least 30 Myr. During thistime they emit X-ray, H$\alpha$ and dust infrared emission. X-ray liminosities$L_X\propto {\rm SFR}^{3/5}$ that we derive here are consistent withobservations in star-forming galaxies. Even though dust particles of smallsizes $a\leq 0.03~\mu$m are sputtered in the interior of bubbles, larger grainsstill contribute considerably ensuring the bubble luminosity $L_{\rm IR}/{\rmSFR}\sim 5\times 10^7 L_\odot M_\odot^{-1} ~{\rm yr}$. It is shown that theorigin of the North Polar Spur in the Milky Way can be connected with activityof a cluster with the stellar mass of $\sim 10^5~M_\odot$ and the ${\rmSFR}\sim 0.1~M_\odot$ yr$^{-1}$ some 25--30 Myr ago. Extended luminous haloesobserved in edge-on galaxies (NGC 891 as an example) can be maintained by discspread stellar clusters of smaller masses $M_\ast \simlt 10^5~M_\odot$.

Chemodynamical models of our Galaxy

Dust evolution in a supernova interacting with the ISM

The fragility of thin discs in galaxies -- I. Building tailored N-body galaxy models

Thin stellar discs on both galactic and nuclear, sub-kpc scales are believedto be fragile structures that would be easily destroyed in major mergers. Inturn, this makes the age-dating of their stellar populations a usefuldiagnostics for the assembly history of galaxies. We aim at carefully exploringthe fragility of such stellar discs in intermediate- and low- mass encounters,using high-resolution N-body simulations of galaxy models with structural andkinematic properties tailored to actually observed galaxies. As a first butchallenging step, we create a dynamical model of FCC 170, a nearly edge-ongalaxy in the Fornax cluster with multiple galactic components and includingboth a galactic scale and nuclear stellar disc (NSD), using detailed kinematicdata from the Multi Unit Spectroscopic Explorer and a novel method forconstructing distribution function-based self-consistent galaxy models. We thencreate N-body realisations of this model and demonstrate that it remains inequilibrium and preserves its properties over many Gyr, when evolved with asufficiently high particle number. However, the NSD is more prone to numericalheating, which gradually increases its thickness by up to 22 per cent in 10 Gyreven in our highest-resolution runs. Nevertheless, these N-body models canserve as realistic representations of actual galaxies in merger simulations.

Dust-free starburst galaxies at redshifts $z>10$

One of the most distant galaxies GN-z11 was formed when the Universe was$\le$ 400 Myr old, and it displays a burst-like star formation rate $\sim25~M_\odot$ yr$^{-1}$ with a metallicity $Z\sim 0.2\pm 0.1Z_\odot$. Itresembles $z=2-3$ galaxies (at ``cosmic noon") except for the fact that themeasured reddening $E(B-V)=0.01\pm 0.01$ indicates the presence of little or nodust. This marked absence of dust hints towards violent dynamical events thatdestroy or evacuate dust along with gas out of the galaxy on a relatively shorttime scale and make it transparent. We apply a 3D numerical model to inferpossible physical characteristics of these events. We demonstrate that theenergetics of the observed star formation rate is sufficient to tear apart thedusty veil on time scales of $20-25$ Myr. This can explain the apparent lack ofevolution of UV luminosity function of galaxies between and $z\ge 10$ and$z\sim 7$, by compensating for the lower galaxy masses at higher redshift bythe absence of dust. We show, however, that this is a temporary phenomenon andsoon after the last of the supernovae explosions have taken place, theexpanding shell shrinks and obscures the galaxy on time scales of $\approx 5-8$Myr.

Accelerated phase-mixing in the stellar halo due to a rotating bar

In a galaxy merger, the stars tidally stripped from the satellite andaccreted onto the host galaxy undergo phase mixing and form finely-grainedstructures in the phase space. However, these fragile structures may bedestroyed in the subsequent galaxy evolution, in particular, by a rotating barthat appears well after the merger is completed. In this work, we investigatethe survivability of phase-space structures in the presence of a bar. We findthat a bar with amplitude and pattern speed similar to those of the Milky Waywould blur and destroy a substantial amount of the substructure that consistsof particles with pericentre radii comparable to the bar length. While thisappears to be in tension with the recent discovery of phase-space chevrons in\textit{Gaia} DR3 data, the most prominent chevrons in our simulations canstill be recovered when applying the same analysis procedure as inobservations. Moreover, the smoothing effect is less pronounced in thepopulation of stars whose angular momenta have the opposite sign to the barpattern speed.

Testing of various protocols for human skin cryopreservation by vitrification method

Magnetic phase diagram and possible Kitaev-like behavior of honeycomb-lattice antimonate Na3Co2SbO6

Recent theoretical studies have suggested that Kitaev physics and sucheffects as formation of a mysterious spin-liquid state can be expected not onlyin RuCl3 and iridates, but also in conventional $3d$ transition metalcompounds. Using DC and AC magnetometry, thermodynamic and $^{23}$Na nuclearmagnetic resonance measurements (NMR) we studied such a candidate materialNa3Co2SbO6. A full phase diagram of Na3Co2SbO6 in a wide range of magneticfields and temperatures is presented. The results demonstrate transformation ofthe antiferromagnetic structure under the external magnetic field, gradualdevelopment of the saturation phase, as well as evidence of gapped behavior incertain parts of the phase diagram

Magnetic circular dichroism in the dd excitation in the van der Waals magnet CrI3 probed by resonant inelastic x-ray scattering