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Journal articles on the topic 'WIND INTERACTION'

Author: Grafiati

Published: 11 September 2023

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1

Colosimo, Irene, Paul L. M. de Vet, Dirk S. van Maren, Ad J. H. M. Reniers, Johan C. Winterwerp, and Bram C. van Prooijen. "The Impact of Wind on Flow and Sediment Transport over Intertidal Flats." Journal of Marine Science and Engineering 8, no. 11 (November 12, 2020): 910. http://dx.doi.org/10.3390/jmse8110910.

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Sediment transport over intertidal flats is driven by a combination of waves, tides, and wind-driven flow. In this study we aimed at identifying and quantifying the interactions between these processes. A five week long dataset consisting of flow velocities, waves, water depths, suspended sediment concentrations, and bed level changes was collected at two locations across a tidal flat in the Wadden Sea (The Netherlands). A momentum balance was evaluated, based on field data, for windy and non-windy conditions. The results show that wind speed and direction have large impacts on the net flow, and that even moderate wind can reverse the tidal flow. A simple analytical tide–wind interaction model shows that the wind-induced reversal can be predicted as a function of tidal flow amplitude and wind forcing. Asymmetries in sediment transport are not only related to the tide–wind interaction, but also to the intratidal asymmetries in sediment concentration. These asymmetries are influenced by wind-induced circulation interacting with the large scale topography. An analysis of the shear stresses induced by waves and currents revealed the relative contributions of local processes (resuspension) and large-scale processes (advection) at different tidal flat elevations.

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2

Boyko, Taras, Mariia Ruda, Serhiy Stasevych, and Olha Chaplyk. "THE WIND TURBINE AND THE ENVIRONMENT INTERACTION MODEL." Measuring Equipment and Metrology 82, no. 4 (2021): 51–60. http://dx.doi.org/10.23939/istcmtm2021.04.051.

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The modeling of the mutual influence of the wind power plant and the ecosystem is carried out. It is proposed to consider the compartment of a complex landscape complex as an elementary structural element of the ecosystem. The wind power plant is a component of a complex landscape complex and is considered during its life cycle. The categories of environmental impact and the relative contribution of harmful factors for each category have been determined. The modeling was carried out using various scenarios of waste management, which will make it possible to reduce the negative impact of harmful factors for each category. Summary data on the impact of harmful factors on the environment were obtained, and ecological profiles were constructed using the Eco-indicator methodology. Such profiles, together with the weighting factors, allow a comprehensive presentation of environmental impacts and obtaining the values of eco-indicators that characterize the damage caused by a wind turbine to the environment. The process of synthesis of an industrial cyber-physical system is carried out by five typical steps, among which the process of ‘cyber-realization’ is to create a cyber twin and compare it with the real system. To implement this process, mathematical modeling was carried out, as a result of which a system of differential equations was obtained, the input data for which were the values of environmental impacts, expressed by the specified indicators. The resulting model will act as ideal for a real system ‘wind turbine – environment”, and will allow predicting the consequences of the harmful impact of a wind turbine on a complex landscape system and will determine the main impacts to achieve its maximum efficiency and adaptation to the requirements for environmental protection and conservation. Some results obtained using the developed model are presented.

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3

Lee, Kyoungsoo, Ziaul Huque, Raghava Kommalapati, and Sang-Eul Han. "The Evaluation of Aerodynamic Interaction of Wind Blade Using Fluid Structure Interaction Method." Journal of Clean Energy Technologies 3, no. 4 (2015): 270–75. http://dx.doi.org/10.7763/jocet.2015.v3.207.

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4

Andreas, Edgar L., and Larry Mahrt. "On the Prospects for Observing Spray-Mediated Air–Sea Transfer in Wind–Water Tunnels." Journal of the Atmospheric Sciences 73, no. 1 (December 21, 2015): 185–98. http://dx.doi.org/10.1175/jas-d-15-0083.1.

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Abstract Nature is wild, unconstrained, and often dangerous. In particular, studying air–sea interaction in winds typical of tropical cyclones can place researchers, their instruments, and even their research platforms in jeopardy. As an alternative, laboratory wind–water tunnels can probe 10-m equivalent winds of hurricane strength under conditions that are well constrained and place no personnel or equipment at risk. Wind–water tunnels, however, cannot simulate all aspects of air–sea interaction in high winds. The authors use here the comprehensive data from the Air–Sea Interaction Salt Water Tank (ASIST) wind–water tunnel at the University of Miami that Jeong, Haus, and Donelan published in this journal to demonstrate how spray-mediated processes are different over the open ocean and in wind tunnels. A key result is that, at all high-wind speeds, the ASIST tunnel was able to quantify the so-called interfacial air–sea enthalpy flux—the flux controlled by molecular processes right at the air–water interface. This flux cannot be measured in high winds over the open ocean because the ubiquitous spray-mediated enthalpy transfer confounds the measurements. The resulting parameterization for this interfacial flux has implications for modeling air–sea heat fluxes from moderate winds to winds of hurricane strength.

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5

Kurniawati, Diniar Mungil. "Investigasi Performa Turbin Angin Crossflow Dengan Simulasi Numerik 2D." JTT (Jurnal Teknologi Terpadu) 8, no. 1 (April 27, 2020): 7–12. http://dx.doi.org/10.32487/jtt.v8i1.762.

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Wind turbine is a solution to harness of renewable energy because it requires wind as the main energy. Wind turbine work by extracting wind energy into electrical energy. Crossflow wind turbine is one of the wind turbines that are developed because it does not need wind direction to produce maximum efficiency. Crossflow wind turbines work with the concept of multiple interactions, namely in the first interaction the wind hits the first level of turbine blades, then the interaction of the two winds, the remainder of the first interaction enters the second level blades before leaving the wind turbine. In the design of crossflow wind turbine the diameter ratio and slope angle are important factors that influence to determine of performance in crossflow wind turbine. In this study varied the angle of slope 90 ° and variations in diameter ratio of 0.6 and 0.7. The study aimed to analyze the effect of diameter ratio and slope angle in performance of the crossflow wind turbine. This research was conducted with numerical simulation through 2D CFD modeling. The results showed that the best performance of crossflow wind turbine occurred at diameter ratio variation 0.7 in TSR 0.3 with the best CP value 0.34.

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6

MacLeod, Morgan, and Antonija Oklopčić. "Stellar Wind Confinement of Evaporating Exoplanet Atmospheres and Its Signatures in 1083 nm Observations." Astrophysical Journal 926, no. 2 (February 1, 2022): 226. http://dx.doi.org/10.3847/1538-4357/ac46ce.

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Abstract Atmospheric escape from close-in exoplanets is thought to be crucial in shaping observed planetary populations. Recently, significant progress has been made in observing this process in action through excess absorption in-transit spectra and narrowband light curves. We model the escape of initially homogeneous planetary winds interacting with a stellar wind. The ram pressure balance of the two winds governs this interaction. When the impingement of the stellar wind on the planetary outflow is mild or moderate, the planetary outflow expands nearly spherically through its sonic surface before forming a shocked boundary layer. When the confinement is strong, the planetary outflow is redirected into a cometary tail before it expands to its sonic radius. The resultant transmission spectra at the He 1083 nm line are accurately represented by a 1D spherical wind solution in cases of mild to moderate stellar wind interaction. In cases of strong stellar wind interaction, the degree of absorption is enhanced and the cometary tail leads to an extended egress from transit. The crucial features of the wind–wind interaction are, therefore, encapsulated in the light curve of He 1083 nm equivalent width as a function of time. The possibility of extended He 1083 nm absorption well beyond the optical transit carries important implications for planning out-of-transit observations that serve as a baseline for in-transit data.

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7

Jin, Xin, Changming Dong, Jaison Kurian, James C. McWilliams, Dudley B. Chelton, and Zhijin Li. "SST–Wind Interaction in Coastal Upwelling: Oceanic Simulation with Empirical Coupling." Journal of Physical Oceanography 39, no. 11 (November 1, 2009): 2957–70. http://dx.doi.org/10.1175/2009jpo4205.1.

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Abstract Observations, primarily from satellites, have shown a statistical relationship between the surface wind stress and underlying sea surface temperature (SST) on intermediate space and time scales, in many regions inclusive of eastern boundary upwelling current systems. In this paper, this empirical SST–wind stress relationship is utilized to provide a simple representation of mesoscale air–sea coupling for an oceanic model forced by surface winds, namely, the Regional Oceanic Modeling System (ROMS). This model formulation is applied to an idealized upwelling problem with prevailing equatorward winds to determine the coupling consequences on flow, SST, stratification, and wind evolutions. The initially uniform wind field adjusts through coupling to a cross-shore profile with weaker nearshore winds, similar to realistic ones. The modified wind stress weakens the nearshore upwelling circulation and increases SST in the coastal zone. The SST-induced wind stress curl strengthens offshore upwelling through Ekman suction. The total curl-driven upwelling exceeds the coastal upwelling. The SST-induced changes in the nearshore wind stress field also strengthen and broaden the poleward undercurrent. The coupling also shows significant impact on the developing mesoscale eddies by damaging cyclonic eddies more than anticyclonic eddies, which leads to dominance by the latter. Dynamically, this is a consequence of cyclones with stronger SST gradients that induce stronger wind perturbations in this particular upwelling problem and that are therefore generally more susceptible to disruption than anticyclones at finite Rossby number. The net effect is a weakening of eddy kinetic energy.

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8

Scherer, K., A. Noack, J. Kleimann, H. Fichtner, and K. Weis. "The interaction of multiple stellar winds in stellar clusters: potential flow." Astronomy & Astrophysics 616 (August 2018): A115. http://dx.doi.org/10.1051/0004-6361/201832696.

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Context. While several studies have investigated large-scale cluster winds resulting from an intra-cluster interaction of multiple stellar winds, as yet they have not provided details of the bordering flows inside a given cluster. Aims. The present work explores the principal structure of the combined flow resulting from the interaction of multiple stellar winds inside stellar clusters. Methods. The theory of complex potentials is applied to analytically investigate stagnation points, boundaries between individual outflows, and the hydrodynamic structure of the asymptotic large-scale cluster wind. In a second part, these planar considerations are extended to fully three-dimensional, asymmetric configurations of wind-driving stars. Results. We find (i) that one can distinguish regions in the large-scale cluster wind that are determined by the individual stellar winds, (ii) that there are comparatively narrow outflow channels, and (iii) that the large-scale cluster wind asymptotically approaches spherical symmetry at large distances. Conclusions. The combined flow inside a stellar cluster resulting from the interaction of multiple stellar winds is highly structured.

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9

Wang, Zhi, and Margaret Galland Kivelson. "Asteroid interaction with solar wind." Journal of Geophysical Research: Space Physics 101, A11 (November 1, 1996): 24479–93. http://dx.doi.org/10.1029/96ja02019.

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10

Sauer, K., A. Lipatov, K. Baumgärtel, and E. Dubinin. "Solar wind-Pluto interaction revised." Advances in Space Research 20, no. 2 (January 1997): 295–99. http://dx.doi.org/10.1016/s0273-1177(97)00551-6.

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11

Fujimoto, M., W. Baumjohann, K. Kabin, R. Nakamura, J. A. Slavin, N. Terada, and L. Zelenyi. "Hermean Magnetosphere-Solar Wind Interaction." Space Science Reviews 132, no. 2-4 (October 2007): 529–50. http://dx.doi.org/10.1007/s11214-007-9245-8.

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12

Herbert, Floyd. "Solar wind interaction with asteroids." Advances in Space Research 13, no. 10 (October 1993): 249–58. http://dx.doi.org/10.1016/0273-1177(93)90076-n.

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13

Michel, F. C. "Solar wind interaction with planets." Advances in Space Research 14, no. 6 (June 1994): 181. http://dx.doi.org/10.1016/0273-1177(94)90025-6.

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14

Je, Seungwoo, Hyelip Lee, Myung Jin Kim, Minkyeong Lee, Yoonji Kim, Youngkyung Choi, and Andrea Bianchi. "Wind-blaster." Interactions 26, no. 1 (December 21, 2018): 14–15. http://dx.doi.org/10.1145/3292075.

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15

Zizkovsky, Nikola, and Jan Klesa. "Wing-Propeller Interaction." MATEC Web of Conferences 304 (2019): 02019. http://dx.doi.org/10.1051/matecconf/201930402019.

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Paper describes the effect of the distributed electric propulsion system (DEP) on the aerodynamic characteristics of the airplane wing. Using CFD simulation is described the influence of the wake of the propeller on the wing for various ratios of the propeller diameter to the wing chord. Unlike the normal case of wing-propeller interaction, periodic boundary conditions are used, i.e. a rectangular wing with infinite span with propellers installed periodically its span is considered. A wind tunnel experiment will be used to verify the calculations. Propeller thrust is set to compensate for airplane drag in horizontal flight, i.e. equal to the wing segment drag, which is increased by the corresponding part of the expected drag of other parts of the airplane. The increase of the drag was determined by the aerodynamic design of a generic airplane with DEP. The benefit of the work are the input data usable for the conceptual design of the airplane wing with DEP.

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16

Torres-Albà, Núria, and Valentí Bosch-Ramon. "Gamma rays from red giant wind bubbles entering the jets of elliptical host blazars." Astronomy & Astrophysics 623 (March 2019): A91. http://dx.doi.org/10.1051/0004-6361/201833697.

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Context. Blazars in elliptical hosts have a population of red giants surrounding their jet. These stars can carry large wind-blown bubbles into the jets, leading to gamma-ray emission through bubble-jet interactions. Aims. We study the interaction dynamics and the gamma-ray emission produced when the bubbles formed by red giant winds penetrate the jet of a blazar in an elliptical galaxy. Methods. First, we characterized the masses and penetration rates of the red giant wind bubbles that enter the jet. Then, the dynamical evolution of these bubbles under the jet impact was analysed analytically and numerically, and the radiation losses of the particles accelerated in the interaction were characterised. Finally, the synchrotron and the inverse Compton contributions above ∼100 MeV were estimated under different jet magnetic fields, powers, and Lorentz factors. Results. We find that an analytical dynamical model is a reasonable approximation for the red giant wind bubble-jet interaction. The radiation produced by these wind bubbles interacting with a jet can have a duty cycle of up to ∼1. For realistic magnetic fields, gamma rays could be detectable from sources within the local universe, preferentially from those with high Lorentz factors (∼10), and this could be a relatively common phenomenon for these sources. For magnetic fields in equipartition with the jet power, and high acceleration rates, synchrotron gamma rays may be detectable even for modest Lorentz factors (∼3), but with a much lower duty cycle. Conclusions. Blazars in elliptical galaxies within the local universe can produce detectable transient or persistent gamma-ray emission from red giant wind bubbles entering their jets.

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17

Gayley, Kenneth G., and Stanley P. Owocki. "Dynamics and variability of winds in WR+O binaries." Symposium - International Astronomical Union 193 (1999): 168–76. http://dx.doi.org/10.1017/s0074180900205275.

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The presence of a nearby O star offers the potential for studying the response of a Wolf-Rayet wind to external irradiation from a well-understood UV source. The O starlight offers not only a passive diagnostic probe, but also the potential for a dynamical interaction whose nature relates directly to fundamental issues of how WR winds are driven. It may even decelerate the WR wind prior to the wind/wind interaction, an effect we term radiative braking. We report on recent progress in WR+O wind-wind interaction models that incorporate the influence of the O starlight on the incident WR wind, and also the effect of the WR starlight on the acceleration of the O-star wind. A recurrent theme is the importance of feedback between the line force and the gas dynamics, and the leveraging that results.

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18

Reid, JS. "Observational evidence of the interaction of ocean wind-sea with swell." Marine and Freshwater Research 46, no. 2 (1995): 419. http://dx.doi.org/10.1071/mf9950419.

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More than 10 000 spectra of ocean wave data were acquired from a series of buoys moored in the Southern Ocean off the west coast of Tasmania for a period of seven years. Spectra were grouped according to the wind speed and whether the wind direction was onshore or offshore and the mean spectrum found for each group. The frequencies of the low frequency cut-offs and of the spectral peaks of the resulting mean spectra were found to be independent of the wind speed in contrast to self-similar standard spectra such as JONSWAP. This property is attributed to the presence of a swell background which controls the evolution of wind-seas in the open ocean. During offshore winds, the spectral variance between 0.04 Hz and 0.16 Hz was found to be negatively correlated with wind speed indicating that swell is in turn shaped either by the wind-sea or by the wind itself. Relationships between various spectral and time domain parameters and the wind speed were investigated empirically. The slope/acceleration measures such as m4, the spectral fourth moment, were found to be highly correlated with wind speed.

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19

van Marle, Allard Jan, and Rony Keppens. "Numerical simulations of the circumstellar medium of massive binaries." Proceedings of the International Astronomical Union 6, S271 (June 2010): 405–6. http://dx.doi.org/10.1017/s1743921311018011.

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AbstractWe have made 3-D models of the collision of binary star winds and followed their interaction over multiple orbits. This allows us to explore how the wind-wind interaction shapes the circumstellar environment. Specifically, we can model the highly radiative shock that occurs where the winds collide. We find that the shell that is created at the collision front between the two winds can be highly unstable, depending on the characteristics of the stellar winds.

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20

Kocewiak, Łukasz Hubert, Jesper Hjerrild, and Claus Leth Bak. "Wind turbine converter control interaction with complex wind farm systems." IET Renewable Power Generation 7, no. 4 (July 2013): 380–89. http://dx.doi.org/10.1049/iet-rpg.2012.0209.

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21

Wang, Yining, Da Xie, Xitian Wang, and Yu Zhang. "Prediction of Wind Turbine-Grid Interaction Based on a Principal Component Analysis-Long Short Term Memory Model." Energies 11, no. 11 (November 20, 2018): 3221. http://dx.doi.org/10.3390/en11113221.

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The interaction between the gird and wind farms has significant impact on the power grid, therefore prediction of the interaction between gird and wind farms is of great significance. In this paper, a wind turbine-gird interaction prediction model based on long short term memory (LSTM) network under the TensorFlow framework is presented. First, the multivariate time series was screened by principal component analysis (PCA) to reduce the data dimensionality. Secondly, the LSTM network is used to model the nonlinear relationship between the selected sequence of wind turbine network interactions and the actual output sequence of the wind farms, it is proved that it has higher accuracy and applicability by comparison with single LSTM model, Autoregressive Integrated Moving Average (ARIMA) model and Back Propagation Neural Network (BPNN) model, the Mean Absolute Percentage Error (MAPE) is 0.617%, 0.703%, 1.397% and 3.127%, respectively. Finally, the Prony algorithm was used to analyze the predicted data of the wind turbine-grid interactions. Based on the actual data, it is found that the oscillation frequencies of the predicted data from PCA-LSTM model are basically the same as the oscillation frequencies of the actual data, thus the feasibility of the model proposed for analyzing interaction between grid and wind turbines is verified.

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22

Frank, A., B. Lui, J. Carroll-Nellenback, A. C. Quillen, E. G. Blackman, J. Kasting, and I. Dobbs-Dixon. "Planetary Evaporation and the Dynamics of Planet Wind/Stellar Wind Bow Shocks." Proceedings of the International Astronomical Union 10, S314 (November 2015): 237–40. http://dx.doi.org/10.1017/s1743921315006675.

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AbstractWe present initial results of a new campaign of simulations focusing on the interaction of planetary winds with stellar environments using Adaptive Mesh Refinement methods. We have confirmed the results of Stone & Proga (2009) that an azimuthal flow structure is created in the planetary wind due to day/night temperatures differences. We show that a backflow towards the planet will occur with a strength that depends on the escape parameter. When a stellar outflow is included, we see unstable bow waves forming through the outflow's interaction with the planetary wind.

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23

Rozhkova, Ludmila, Tibor Krenicky, Eduard Kuznetsov, and Volodymyr Nahornyi. "Blades Interaction and Non-Stationarity of Flow in Vertical-Axial Wind Turbines." Management Systems in Production Engineering 29, no. 4 (December 1, 2021): 280–86. http://dx.doi.org/10.2478/mspe-2021-0035.

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Abstract Until recently, horizontal-axial wind turbines with blades having a wing profile occupied a predominant position in the world wind energy market. But currently, vertical-axial wind units are of increasing interest and this is understandable from the point of view of their important features as: no requirements for the orientation of the wind turbine to the wind, the possibility of placing electrical and other equipment on the ground, no requirements for changes of blade chord installation angle along its length. The article discusses the aerodynamics of the vertical-axis wind turbines: the range of changes of angles of incoming flow attack on the blade, the dynamics of changes in the magnitude of the absolute speed of flow of the blade on a circular trajectory of its movement depending on the turbine rapidity, and also obtained in experiments interaction effect of the blades in the rotor. The experiments were carried out on wind turbines with original blades (basic version), which were designed to eliminate the shortcomings of low-speed rotors Savonius (low coefficient of use of wind energy) and high-speed rotors Darrieus (lack of self-start).

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24

Roul, Rajendra, and Awadhesh Kumar. "Fluid-Structure Interaction of Wind Turbine Blade Using Four Different Materials: Numerical Investigation." Symmetry 12, no. 9 (September 7, 2020): 1467. http://dx.doi.org/10.3390/sym12091467.

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The interaction of a flexible system with a moving fluid gives rise to a wide variety of physical phenomena with applications in various engineering fields, such as aircraft wing stability, arterial blood progression, high structure reaction to winds, and turbine blade vibration. Both the structure and fluid need to be modeled to understand these physical phenomena. However, in line with the overall theme of this strength, the focus here is to investigate wind turbine aerodynamic and structural analysis by combining computational fluid dynamics (CFD) and finite element analysis (FEA). One-way coupling is chosen for the fluid-structure interaction (FSI) modeling. The investigation is carried out with the use of commercialized ANSYS applications. A total of eight different wind velocities and five different angles of pitch are considered in this analysis. The effect of pitch angles on the output of a wind turbine is also highlighted. The SST k-ω turbulence model has been used. A structural analysis investigation was also carried out and is carried out after importing the pressure load exerted from the aerodynamic analysis and subsequently finding performance parameters such as deformation and Von-Mises stress.

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25

Zhekov, Svetozar A., A. V. Myasnikov, and E. V. Barsky. "Colliding stellar winds: magnetic field structure in the interaction region." Symposium - International Astronomical Union 193 (1999): 400–401. http://dx.doi.org/10.1017/s0074180900205937.

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The geometry structure of the magnetic field in colliding stellar winds is studied. It is shown that the magnetic field influence in the interaction region depends mainly on the ratio of the wind ram pressures of the components, the ratio of the stellar linear rotational velocity to the wind velocity of the magnetized star, and the stellar separation. For the radiative colliding winds the magnetic field influence increases with the importance of the radiative losses. An asymmetric magnetic field structure appears for a given set of binary parameters and the interaction region might be an asymmetric source of non-thermal radio emission.

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26

Vidotto, A. A. "Incorporating magnetic field observations in wind models of low-mass stars." ASTRA Proceedings 1 (June 6, 2014): 19–22. http://dx.doi.org/10.5194/ap-1-19-2014.

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Abstract. Stellar winds of cool, main-sequence stars are very tenuous and difficult to observe. Despite carrying away only a small amount of the stellar mass, they are important for regulating the rotation of the star and, consequently, its activity and magnetism. As it permeates the interplanetary space, the stellar wind interacts with any exoplanet encountered on its way, until it reaches the interstellar medium (ISM). These interactions can result in complex physical processes that depend on the characteristics of the wind. To better constrain the wind characteristics, more realistic wind models that account for factors such as stellar rotation and the complex/diverse observationally-derived stellar magnetic field configurations of cool stars are required. In this paper, I present a three-dimensional model of the wind of cool stars, which adopt as boundary condition observationally-derived magnetic maps. I also discuss how these studies are relevant for, e.g., the characterisation of the interaction between stellar winds and planets/ISM, and the propagation of cosmic rays.

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27

Kwok, Sun. "Wind Accretion and Interaction in Long Period Binary Systems." Highlights of Astronomy 7 (1986): 189–95. http://dx.doi.org/10.1017/s1539299600006407.

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AbstractRecent observations of the class of objects called symbiotic nova are reviewed. They are suggested to be widely-separated long-period binary systems undergoing mass exchange by wind accretion. Their radio, infrared, optical and X-ray properties are explained by a model of interacting winds.

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28

Lockwood, Jeffrey A. "NONSEXUAL INTERACTIONS IN THE BIG-HEADED GRASSHOPPER AULOCARA ELLIOTTI (THOMAS) (ORTHOPTERA: ACRIDIDAE)." Journal of Entomological Science 23, no. 4 (October 1, 1988): 383–93. http://dx.doi.org/10.18474/0749-8004-23.4.383.

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Nonsexual interactions of the big-headed grasshopper, Aulocara elliotti (Thomas), were examined under natural conditions in context of intrinsic (age and conspecificity of grasshoppers, speed and direction of movement and duration of interaction) and extrinsic (date, time of day, soil and air temperature, relative humidity, wind speed and sunlight) factors. With respect of intrinsic factors, the developmental stage and conspecificity of interacting grasshoppers and the direction of approach by the individual initiating an interaction significantly affected interactive behaviors, including kicking, shifting, approaching, contact and pursuit. These three factors also influenced the outcome of interaction, especially the frequency of avoidance by residents. Among the extrinsic factors, time of day, soil temperature and relative humidity had the greatest affects on the aforementioned interactive behaviors. The time of year, relative humidity and wind speed significantly affected the outcome of interactions. Physical contact and pursuit were the only behaviors to significantly affect the outcome of interactions. Inferential evidence indicates that aggressive interactions may be the result of defense of territories based on limited, suitable microhabitats.

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29

Kim, Y. M., N. H. Ko, and K. P. You. "Wind-generated interaction between tall buildings." Civil Engineering Innovation 3, no. 1 (March 3, 2009): 7–17. http://dx.doi.org/10.1680/einn.2009.3.1.7.

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Kim, Y. M., K. P. You, and N. H. Ko. "Wind-generated interaction between tall buildings." Proceedings of the Institution of Civil Engineers - Structures and Buildings 160, no. 5 (October 2007): 295–303. http://dx.doi.org/10.1680/stbu.2007.160.5.295.

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Kim, Young-Moon, Ki-Pyo You, and Nag-Ho Ko. "Wind-generated interaction between tall buildings." Civil Engineering Innovation 3, no. 1 (January 2009): 07–17. http://dx.doi.org/10.1680/jciei.2009.3.1.7.

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32

Mellen, R. H., and D. Middleton. "On the wind‐wave interaction mechanism." Journal of the Acoustical Society of America 78, S1 (November 1985): S2. http://dx.doi.org/10.1121/1.2022738.

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33

Bagenal, Fran, and Ralph L. McNutt. "Pluto‧s interaction with the solar wind." Geophysical Research Letters 16, no. 11 (November 1989): 1229–32. http://dx.doi.org/10.1029/gl016i011p01229.

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34

IP, W. H. "Solar wind interaction with Uranus' atmosphere." Nature 319, no. 6051 (January 1986): 268. http://dx.doi.org/10.1038/319268a0.

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35

Delamere, P. A., and F. Bagenal. "Solar wind interaction with Jupiter's magnetosphere." Journal of Geophysical Research: Space Physics 115, A10 (October 2010): n/a. http://dx.doi.org/10.1029/2010ja015347.

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36

Guirguis, N. M., G. B. Hanna, M. F. Kotkata, and I. A. Gad. "An investigation of building/wind interaction." Renewable Energy 15, no. 1-4 (September 1998): 383–86. http://dx.doi.org/10.1016/s0960-1481(98)00191-8.

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37

Galeev, A. A. "Solar wind interaction with comet Halley." Advances in Space Research 5, no. 12 (January 1985): 155–63. http://dx.doi.org/10.1016/0273-1177(85)90081-x.

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Zanon, Mario, Sébastien Gros, Johan Meyers, and Moritz Diehl. "Airborne Wind Energy: Airfoil-Airmass Interaction." IFAC Proceedings Volumes 47, no. 3 (2014): 5814–19. http://dx.doi.org/10.3182/20140824-6-za-1003.00258.

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39

Cravens, T. E., and D. F. Strobel. "Pluto’s solar wind interaction: Collisional effects." Icarus 246 (January 2015): 303–9. http://dx.doi.org/10.1016/j.icarus.2014.04.011.

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40

Hale, J. P. M., and C. S. Paty. "Pluto–Charon solar wind interaction dynamics." Icarus 287 (May 2017): 131–39. http://dx.doi.org/10.1016/j.icarus.2016.11.036.

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41

Lindkvist, Jesper, Mats Holmström, Shahab Fatemi, Martin Wieser, and Stas Barabash. "Ceres interaction with the solar wind." Geophysical Research Letters 44, no. 5 (March 4, 2017): 2070–77. http://dx.doi.org/10.1002/2016gl072375.

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McComas, D. J., H. A. Elliott, S. Weidner, P. Valek, E. J. Zirnstein, F. Bagenal, P. A. Delamere, et al. "Pluto's interaction with the solar wind." Journal of Geophysical Research: Space Physics 121, no. 5 (May 2016): 4232–46. http://dx.doi.org/10.1002/2016ja022599.

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Beer, Tom. "The interaction of wind and fire." Boundary-Layer Meteorology 54, no. 3 (February 1991): 287–308. http://dx.doi.org/10.1007/bf00183958.

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Ramachandran, Varsha. "Winds of OB stars: impact of metallicity, rotation and binary interaction." Proceedings of the International Astronomical Union 17, S370 (August 2021): 223–29. http://dx.doi.org/10.1017/s1743921322004720.

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AbstractWinds of massive stars are an important ingredient in determining their evolution, final remnant mass, and feedback to the surrounding interstellar medium. We compare empirical results for OB star winds at low metallicity with theoretical predictions. Observations suggest very weak winds at SMC metallicity, but there are exceptions. We identified promising candidates for rotationally enhanced mass-loss rates with two component wind and partially stripped stars hiding among OB stars with slow but dense wind in the SMC. A preliminary analysis of these systems, derived parameters, and their implications are discussed. Finally, we briefly discuss the interaction of OB winds near black holes in X-ray binaries.

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CAI, C. S., WEI ZHANG, XIANZHI LIU, WEI PENG, S. R. CHEN, Y. HAN, and J. X. HU. "FRAMEWORK OF WIND–VEHICLE–BRIDGE INTERACTION ANALYSIS AND ITS APPLICATIONS." Journal of Earthquake and Tsunami 07, no. 03 (September 2013): 1350020. http://dx.doi.org/10.1142/s1793431113500206.

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Under strong winds, bridges may exhibit large dynamic responses. Wind may also endanger the safety of moving vehicles on the roadways as well as on bridges. For regular aerodynamic study of long-span bridges, traffic loads are not typically considered, assuming that bridges will be closed to traffic at high wind speeds. Therefore, bridges are usually tested in wind tunnels or analyzed numerically without considering moving vehicles on them. However, there are numerous possible scenarios under which vehicles may still be on the bridge when higher wind speeds occur. These scenarios include unexpected increase in hurricane forward speed or intensity, evacuation traffic gridlock, accidents/stalled vehicles or rainfall flooding blocking the road ahead, etc. Wind, together with vehicles, will also cause serviceability and bridge fatigue damage issues. The present study will present the framework of wind–vehicle–bridge interaction analysis and its applications, developed in the last decade by the authors' group, focused on the vehicle and bridge safety issues. It consists of the following five parts: (1) A three dimensional finite element analysis framework considering the interaction of wind, bridge and vehicles; (2) experimental facilities development and studies for both static and aerodynamic tests of bridge section models and vehicles; (3) Computation fluid dynamic (CFD) prediction of loading on vehicles; (4) performance evaluation of vehicle safety and bridge fatigue; and (5) bridge vibration mitigations. Case study will also be presented and future research needs are discussed.

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Shen, Ken J., and Eliot Quataert. "Binary Interaction Dominates Mass Ejection in Classical Novae." Astrophysical Journal 938, no. 1 (October 1, 2022): 31. http://dx.doi.org/10.3847/1538-4357/ac9136.

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Abstract Recent observations suggest our understanding of mass loss in classical novae is incomplete, motivating a new theoretical examination of the physical processes responsible for nova mass ejection. In this paper, we perform hydrodynamical simulations of classical nova outflows using the stellar evolution code MESA. We find that, when the binary companion is neglected, white dwarfs with masses ≳0.8 M ⊙ successfully launch radiation-pressure-driven optically thick winds that carry away most of the envelope. However, for most of the mass-loss phase, these winds are accelerated at radii beyond the white dwarf’s Roche radius assuming a typical cataclysmic variable donor. This means that, before a standard optically thick wind can be formed, mass loss will instead be initiated and shaped by binary interaction. An isotropic, optically thick wind is only successfully launched when the acceleration region recedes within the white dwarf’s Roche radius, which occurs after most of the envelope has already been ejected. The interaction between these two modes of outflow—a first phase of slow, binary-driven, equatorially focused mass loss encompassing most of the mass ejection and a second phase consisting of a fast, isotropic, optically thick wind—is consistent with observations of aspherical ejecta and signatures of multiple outflow components. We also find that isolated lower-mass white dwarfs ≲0.8 M ⊙ do not develop unbound optically thick winds at any stage, making it even more crucial to consider the effects of the binary companion on the resulting outburst.

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Ham, Yoo-Geun, Jong-Seong Kug, and Mi-Jung Lim. "Rectification Feedback of High-Frequency Atmospheric Variability into Low-Frequency Zonal Flows in the Tropical Pacific." Journal of Climate 25, no. 14 (July 15, 2012): 5088–101. http://dx.doi.org/10.1175/jcli-d-11-00303.1.

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Abstract In this study, the rectification process of high-frequency (HF) zonal-wind variability on the low-frequency (LF) zonal wind is investigated through an idealized experiment using an atmospheric general circulation model (AGCM). Through an idealized AGCM experiment with a fixed SST boundary forcing, it is shown that there is positive (negative) correlation between HF (2–90-day period) zonal-wind variance and LF (3-month average) zonal wind where the HF zonal-wind variance is positively (negatively) skewed because the stronger HF westerly (easterly) wind events than HF easterly (westerly) wind events induce a residual westerly (easterly), and it results in an additional rectified LF westerly (easterly) anomaly. This means that, over regions with positively skewed HF zonal winds, LF westerly anomalies are generated due to the residuals of the HF zonal winds. It implies that the LF zonal wind can be generated through internal processes of the atmosphere without external forcing and the interaction between LF and HF is not a one-way process from LF to HF but, rather, a two-way interaction process.

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Kim Dung, Hoang Thi, and Nguyen Phu Khanh. "SIMULATION RESEARCH ON INTERACTION BETWEEN WIND AND SOLAR PHOTOVOLTAICS SYSTEMS." ASEAN Engineering Journal 12, no. 1 (February 28, 2022): 141–48. http://dx.doi.org/10.11113/aej.v12.17265.

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There are many options for reducing greenhouse gas emissions from energy systems while still meeting the global energy needs. One of the options could be renewable energy. Renewable energy has a huge potential to mitigate climate change, that can also provide people with utilities when using them. Renewable energy, if properly implemented, would contribute to socio-economic development, access to energy as a safe source of energy, and reduction of negative impacts on the environment and health. In the most demanding conditions, increasing the share of renewable energy in the energy mix will require policies to stimulate changes in the energy system. This research was focused on the solar photovoltaics (PV) system, especially on the interaction between wind and the PV system. The wind had a cooling effect to the PV system. The wind speed could greatly affect the operating performance of a PV system, especially in windy locations. In this paper, different velocity (from 3 to 15m/s) and incident angle of wind (from 0 to 180 degree) were used to carry out first the strength of PV system and then the influence of wind to the PV system by using ANSYS software. The PV system was found durable under these conditions. Velocity and direction of wind had strong effect to aerodynamic characteristics of solar panels.

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Hansen, Anca D., Poul Sørensen, Frede Blaabjerg, and John Becho. "Dynamic Modelling of Wind Farm Grid Interaction." Wind Engineering 26, no. 4 (July 2002): 191–210. http://dx.doi.org/10.1260/030952402321039403.

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This paper describes a dynamic model of a wind farm and its nearest utility grid. It is intended to use this model in studies addressing the dynamic interaction between a wind farm and a power system, both during normal operation of the wind farm and during transient grid fault events. The model comprises the substation where the wind farm is connected, the internal power collection system of the wind farm, the electrical, mechanical and aerodynamic models for the wind turbines, and a wind model. The integrated model is built to enable the assessment of power quality and control strategies. It is implemented in the commercial dedicated power system simulation tool DIgSILENT.

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Hanley, Kirsty E., Stephen E. Belcher, and Peter P. Sullivan. "A Global Climatology of Wind–Wave Interaction." Journal of Physical Oceanography 40, no. 6 (June 1, 2010): 1263–82. http://dx.doi.org/10.1175/2010jpo4377.1.

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Abstract Generally, ocean waves are thought to act as a drag on the surface wind so that momentum is transferred downward, from the atmosphere into the waves. Recent observations have suggested that when long wavelength waves—which are characteristic of remotely generated swell—propagate faster than the surface wind, momentum can also be transferred upward. This upward momentum transfer acts to accelerate the near-surface wind, resulting in a low-level wave-driven wind jet. Previous studies have suggested that the sign reversal of the momentum flux is well predicted by the inverse wave age, the ratio of the surface wind speed to the speed of the waves at the peak of the spectrum. Data from the 40-yr ECMWF Re-Analysis (ERA-40) have been used here to calculate the global distribution of the inverse wave age to determine whether there are regions of the ocean that are usually in the wind-driven wave regime and others that are generally in the wave-driven wind regime. The wind-driven wave regime is found to occur most often in the midlatitude storm tracks where wind speeds are generally high. The wave-driven wind regime is found to be prevalent in the tropics where wind speeds are generally light and swell can propagate from storms at higher latitudes. The inverse wave age is also a useful indicator of the degree of coupling between the local wind and wave fields. The climatologies presented emphasize the nonequilibrium that exists between the local wind and wave fields and highlight the importance of swell in the global oceans.

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