Bubble dynamics in thin liquid films and breakup at drop impact

Soft Matter ◽  
2020 ◽  
Vol 16 (46) ◽  
pp. 10397-10404
Author(s):  
Elizaveta Ya. Gatapova ◽  
Kyunney B. Gatapova
Keyword(s):  
Bubble Dynamics ◽  
Thin Liquid Film ◽  
Liquid Films ◽  
Drop Impact ◽  
Thin Liquid Films ◽  
Bubble Coalescence ◽  
Bubble Bursting ◽  
Bubble Layer ◽  
Hot Surface ◽  
Surface Bubble

A bubble layer forms in a thin liquid film at drop impact on a hot surface. Bubble coalescence and instability generated by a wave are the reason for irreversible bubble bursting, leading to film breakup at contact boiling.

The mechanism for the long-wave instability in thin liquid films

1990 ◽  
Vol 217 ◽  
pp. 469-485 ◽  
Author(s):  
Marc K. Smith
Keyword(s):  
Physical Mechanism ◽  
Thin Liquid Film ◽  
Liquid Films ◽  
Thin Liquid Films ◽  
The Other ◽  
Wave Instability ◽  
Inclined Plane ◽  
Long Wave ◽  
The Many ◽  
Large Groups

A physical mechanism for the long-wave instability of thin liquid films is presented. We show that the many diverse systems that exhibit this instability can be classified into two large groups. Each group is studied using the model of a thin liquid film with a deformable top surface flowing down a rigid inclined plane. In the first group, the top surface has an imposed stress, while in the other, an imposed velocity. The proposed mechanism shows how the details of the energy transfer from the basic state to the disturbance are handled differently in each of these cases, and how a common growth mechanism produces the unstable motion of the disturbance.

High-speed oblique drop impact on thin liquid films

2017 ◽  
Vol 29 (8) ◽  
pp. 082108 ◽  
Author(s):  
Yisen Guo ◽  
Yongsheng Lian
Keyword(s):  
High Speed ◽  
Liquid Films ◽  
Drop Impact ◽  
Thin Liquid Films

The spreading of thin liquid films on a water-air interface

1980 ◽  
Vol 101 (1) ◽  
pp. 33-51 ◽  
Author(s):  
M. Foda ◽  
R. G. Cox
Keyword(s):  
Surface Tension ◽  
Liquid Film ◽  
Constitutive Relation ◽  
Similarity Solution ◽  
Thickness Distribution ◽  
Thin Liquid Film ◽  
Liquid Films ◽  
Thin Liquid Films ◽  
Air Interface ◽  
Good Agreement

The spreading on a water–air interface of a thin liquid film is examined for the situation in which surface tension gradients drive the motion. A similarity solution is obtained numerically for unidirectional spreading when some general restrictions concerning the form of the liquid film constitutive relation is made. This solution gives the size of the film as a function of time and also the velocity and thickness distribution along the spreading film. Experiments are performed which show good agreement with the theory.

scholarly journals Adsorbed water and thin liquid films on Mars

2012 ◽  
Vol 11 (3) ◽  
pp. 169-175 ◽  
Author(s):  
C. S. Boxe ◽  
K. P. Hand ◽  
K. H. Nealson ◽  
Y. L. Yung ◽  
A. S. Yen ◽  
...  
Keyword(s):  
Liquid Film ◽  
Water Vapour ◽  
Pure Water ◽  
Thin Liquid Film ◽  
Adsorbed Water ◽  
Liquid Films ◽  
Thin Liquid Films ◽  
Atmospheric Water ◽  
Atmospheric Water Vapour ◽  
Water Ice

AbstractAt present, bulk liquid water on the surface and near-subsurface of Mars does not exist due to the scarcity of condensed- and gas-phase water, pressure and temperature constraints. Given that the nuclei of soil and ice, that is, the soil solid and ice lattice, respectively, are coated with adsorbed and/or thin liquid films of water well below 273 K and the availability of water limits biological activity, we quantify lower and upper limits for the thickness of such adsorbed/water films on the surface of the Martian regolith and for subsurface ice. These limits were calculated based on experimental and theoretical data for pure water ice and water ice containing impurities, where water ice containing impurities exhibit thin liquid film enhancements, ranging from 3 to 90. Close to the cold limit of water stability (i.e. 273 K), thin liquid film thicknesses at the surface of the Martian regolith is 0.06 nm (pure water ice) and ranges from 0.2 to 5 nm (water ice with impurities). An adsorbed water layer of 0.06 nm implies a dessicated surface as the thickness of one monolayer of water is 0.3 nm but represents 0.001–0.02% of the Martian atmospheric water vapour inventory. Taking into account the specific surface area (SSA) of surface-soil (i.e. top 1 mm of regolith and 0.06 nm adsorbed water layer), shows Martian surface-soil may contain interfacial water that represents 6–66% of the upper- and lower-limit atmospheric water vapour inventory and almost four times and 33%, the lower- and upper-limit Martian atmospheric water vapour inventory. Similarly, taking the SSA of Martian soil, the top 1 mm or regolith at 5 nm thin liquid water thickness, yields 1.10×1013and 6.50×1013litres of waters, respectively, 55–325 times larger than Mars’ atmospheric water vapour inventory. Film thicknesses of 0.2 and 5 nm represent 2.3×104–1.5×106litres of water, which is 6.0×10−7–4.0×10−4%, respectively, of a 10 prμm water vapour column, and 3.0×10−6–4.0×10−4% and 6.0×10−6–8.0×10−4%, respectively, of the Martian atmospheric water vapour inventory. Thin liquid film thicknesses on/in subsurface ice were investigated via two scenarios: (i) under the idealistic case where it is assumed that the diurnal thermal wave is equal to the temperature of ice tens of centimetres below the surface, allowing for such ice to experience temperatures close to 273 K and (ii) under the, likely, realistic scenario where the diurnal thermal wave allows for the maximum subsurface ice temperature of 235 K at 1 m depth between 30°N and 30°S. Scenario 1 yields thin liquid film thicknesses ranging from 11 to 90 nm; these amounts represent 4×106–3.0×107litres of water. For pure water ice, Scenario 2 reveals that the thickness of thin liquid films contained on/within Martian subsurface is less than 1.2 nm, several molecular layers thick. Conversely, via the effect of impurities at 235 K allows for a thin liquid film thickness on/within subsurface ice of 0.5 nm, corresponding to 6.0×104litres of water. The existence of thin films on Mars is supported by data from the Mars Exploration Rovers (MERs) Spirit and Opportunity's Alpha Proton X-ray Spectrometer instrumentation, which have detected increased levels of bromine beneath the immediate surface, suggestive of the mobilization of soluble salts by thin films of liquid water towards local cold traps. These findings show that biological activity on the Martian surface and subsurface is not limited by nanometre dimensions of available water.

scholarly journals The Rupture of Thin Liquid Films Placed on Solid and Liquid Substrates in Gravity Body Forces

2015 ◽  
Vol 17 (5) ◽  
pp. 1301-1319 ◽  
Author(s):  
A. L. Kupershtokh ◽  
E. V. Ermanyuk ◽  
N. V. Gavrilov
Keyword(s):  
Temperature Distribution ◽  
Liquid Film ◽  
Thin Liquid Film ◽  
Liquid Films ◽  
Solid Substrate ◽  
Immiscible Fluids ◽  
Thin Liquid Films ◽  
Temperature Perturbation ◽  
Rectangular Cell ◽  
Axisymmetric Temperature

AbstractThis paper presents a numerical and experimental study on hydrodynamic behavior of thin liquid films in rectangular domains. Three-dimensional computer simulations were performed using the lattice Boltzmann equation method (LBM). The liquid films laying on solid and liquid substrates are considered. The rupture of liquid films in computations is initiated via the thermocapillary (Marangoni) effect by applying an initial spatially localized temperature perturbation. The rupture scenario is found to depend on the shape of the temperature distribution and on the wettability of the solid substrate. For a wettable solid substrate, complete rupture does not occur: a residual thin liquid film remains at the substrate in the region of pseudo-rupture. For a non-wettable solid substrate, a sharp-peaked axisymmetric temperature distribution induces the rupture at the center of symmetry where the temperature is maximal. Axisymmetric temperature distribution with a flat-peaked temperature profile initiates rupture of the liquid film along a circle at some distance from the center of symmetry. The outer boundary of the rupture expands, while the inner liquid disk transforms into a toroidal figure and ultimately into an oscillating droplet.We also apply the LBM to simulations of an evolution of one or two holes in liquid films for two-layer systems of immiscible fluids in a rectangular cell. The computed patterns are successfully compared against the results of experimental visualizations. Both the experiments and the simulations demonstrate that the initially circular holes evolved in the rectangular cell undergoing drastic changes of their shape under the effects of the surface tension and gravity. In the case of two interacting holes, the disruption of the liquid bridge separating two holes is experimentally observed and numerically simulated.

Thermographic characterization of thin liquid film formation and evaporation in microchannels

Lab on a Chip ◽  
2019 ◽  
Vol 19 (15) ◽  
pp. 2610-2618 ◽  
Author(s):  
Meisam Habibi Matin ◽  
Abdolreza Fazeli ◽  
Saeed Moghaddam
Keyword(s):  
Liquid Film ◽  
Film Formation ◽  
Thin Liquid Film ◽  
Liquid Films ◽  
Thin Liquid Films

Using novel microsensors, the formation and evaporation of thin liquid films in microchannels are characterized.

scholarly journals Flower Patterns in Drop Impact on Thin Liquid Films

2010 ◽  
Vol 105 (18) ◽  
Author(s):  
Guillaume Lagubeau ◽  
Marco A. Fontelos ◽  
Christophe Josserand ◽  
Agnès Maurel ◽  
Vincent Pagneux ◽  
...  
Keyword(s):  
Liquid Films ◽  
Drop Impact ◽  
Thin Liquid Films
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