substructure formation
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Nanomaterials ◽  
2021 ◽  
Vol 11 (11) ◽  
pp. 2811
Author(s):  
Dora Kroisová ◽  
Štěpánka Dvořáčková ◽  
Petr Kůsa

Plant and animal surfaces have become a model for preparing special synthetic surfaces with low wettability, reflectivity, or antibacterial properties. Processes that lead to the creation of replicas of natural character use two-step imprinting methods. This article describes a technique of synthetic polymer surface preparation by the process of two-stage imprinting. The laboratory-prepared structure copies the original natural pattern at the micrometer and sub-micrometer levels, supplemented by a new substructure. The new substructure identified by the scanning electron microscope is created at the nanometer level during the technological process. The nanostructure is formed only under the conditions that a hierarchical structure forms the surface of the natural replicated pattern, the replication mold is from a soft elastomeric material, and the material for producing the synthetic surface is a polymer capable of crystallizing. A new nanometer substructure formation occurs when the polymer cools to standard laboratory temperature and atmospheric pressure.



Author(s):  
Dengcui Yang ◽  
Yanjun Yin ◽  
Xinfeng Kan ◽  
Yan Zhao ◽  
Zhengzhi Zhao ◽  
...  


Materialia ◽  
2021 ◽  
pp. 101042
Author(s):  
S.R. Das ◽  
S. Shyamal ◽  
T. Sahu ◽  
J.I. Kömi ◽  
P.C. Chakraborti ◽  
...  




2020 ◽  
Vol 895 (1) ◽  
pp. L2
Author(s):  
Riouhei Nakatani ◽  
Hauyu Baobab Liu ◽  
Satoshi Ohashi ◽  
Yichen Zhang ◽  
Tomoyuki Hanawa ◽  
...  


2019 ◽  
Vol 55 (2) ◽  
pp. 273-288
Author(s):  
D. A. Noreña ◽  
J. C. Muñoz-Cuartas ◽  
L. F. Quiroga ◽  
N. Libeskind

In this work, we explore the idea that substructures like stellar clusters could be formed from the tidal stream produced in galactic minor mergers. We use N -body and SPH simulations of satellite galaxies interacting with a larger galaxy. We study the distribution of mass in streams to identify overdensity regions in which a substructure could be formed. We find that without gas, no substructure forms as none of the overdensities shows a definite morphology nor dynamical stability. Including gas we find that several clumps appear and prove to be real long standing physical structures (t ≥ 1 Gyr). We analyze the orbits, ages and masses of these structures, finding their correspondence with the halo subsystems. We conclude that it is possible to form cluster-like structures from the material in tidal streams and find evidence in favour of the presence of dark matter in these systems.



2019 ◽  
Vol 25 (S2) ◽  
pp. 208-209
Author(s):  
Daniel L. Foley ◽  
Cassandra Pate ◽  
Kyle Matthews ◽  
Xingyuan Zhao ◽  
Nicolas Savino ◽  
...  


2019 ◽  
Vol 488 (1) ◽  
pp. 306-323 ◽  
Author(s):  
M Behrendt ◽  
M Schartmann ◽  
A Burkert

ABSTRACTGiant clumps on ∼kpc scales and with masses of $10^8\rm {-}10^9 \, \mathrm{M_{\odot }}$ are ubiquitous in observed high-redshift disc galaxies. Recent simulations and observations with high spatial resolution indicate the existence of substructure within these clumps. We perform high-resolution simulations of a massive galaxy to study the substructure formation within the framework of gravitational disc instability. We focus on an isolated and pure gas disc with an isothermal equation of state with T = 104 K that allows capturing the effects of self-gravity and hydrodynamics robustly. The main mass of the galaxy resides in rotationally supported clumps which grow by merging to a maximum clump mass of $10^8 \, \mathrm{M_{\odot }}$ with diameter ∼120 pc for the dense gas. They group to clump clusters (CCs) within relatively short times ($\ll 50 \, \mathrm{Myr}$), which are present over the whole simulation time. We identify several mass and size scales on which the clusters appear as single objects at the corresponding observational resolution between ${\sim } 10^8 \,\rm{and}\, 10^9 \, \mathrm{M_{\odot }}$. Most of the clusters emerge as dense groups and for larger beams they are more likely to be open structures represented by a single object. In the high-resolution runs higher densities can be reached, and the initial structures can collapse further and fragment to many clumps smaller than the initial Toomre length. In our low-resolution runs, the clumps directly form on larger scales 0.3–1 kpc with $10^8\rm {-}10^9 \, \mathrm{M_{\odot }}$. Here, the artificial pressure floor which is typically used to prevent spurious fragmentation strongly influences the initial formation of clumps and their properties at very low densities.



2019 ◽  
Vol 21 (1) ◽  
pp. 160-170 ◽  
Author(s):  
Jan C. Thater ◽  
Cosima Stubenrauch ◽  
Otto Glatter ◽  
Helge Klemmer ◽  
Thomas Sottmann

Role of EAN substructure formation in both oil-in-EAN and EAN-in-oil microemulsions revealed by SANS.



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