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131 results for “Dissipation”
Dataset for Viscous Dissipation and Apparent Permeability of Gas Flow in Nano-Porous Media
<p>Dataset for the Publication of 'Viscous Dissipation and Apparent Permeability of Gas Flow in Nano-Porous Media'.</p>
Supplementary data to 'Do beach profiles under non-breaking waves minimize energy dissipation?'
<p>This repository contains the following files:</p> <p>1. 'data_for_tables.xlsx' summarises the results of using the codes in doi:10.5281/zenodo.3725621 for all profiles considered in this associated paper. These data feed into the tables of the paper. Additional notes can be found in the spreadsheet.</p> <p>2. Three files with extension *.sfit are sessions for the 'cftool' toolbox of Matlab (version 2017b) that give the results of the best-fits to the measured profiles.</p>
Tidal Dissipation in Evolved Low and Intermediate Mass Stars
<p>MESA inlist files used for the simulations presented in the paper "Tidal Dissipation in Evolved Low and Intermediate Mass Stars" by Mats Esseldeurs, Stéphane Mathis, and Leen Decin. The inlist files are used to run the MESA stellar evolution code release-r23.05.1 and MESA-SDK version 21.4.1.</p> <p>In addition to the inlist files, the tidal Love numbers for the equilibrium and dynamical tide are provided in the .h5 (HDF5) files. An example on how to make the images in the paper with these files is given in the Equilibrium.py file.</p> <p>This study was done in collaboration between the KU Leuven and the CEA Paris-Saclay. M. Esseldeurs and L. Decin acknowledge support from the FWO grants G099720N and G0B3823N, the KU Leuven C1 excellence grant MAESTRO C16/17/007 and the KU Leuven IDN grant ESCHER IDN/19/028. S. Mathis acknowledges support from the PLATO CNES grant at CEA/DAp, from the Programme National de Planétologie (PNP-CNRS/INSU) and from the European Research Council through HORIZON ERC SyG Grant 4D-STAR 101071505. While partially funded by the European Union, views and opinions expressed are however those of the author only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them.</p>
Bifurcation of time crystals in driven and dissipative Rydberg atomic gas
<div>These folders contain data used to reproduce figures in main text.</div> <div> </div> <div>The files "fig2a.xlsx" and "fig2d.xlsx" contain the phase diagrams in Figure 2 of the main text. The columns in fig2a.xlsx represent the voltage of the RF-field, and the rows represent the detuning. The columns in fig2d.xlsx represent the frequency of the RF field, and the rows represent the detuning. The values in the table represent transimission.</div> <div> </div> <div>The file "fig3a.xlsx" contains the phase diagram in Figure 3 of the main text. The columns of fig3a.xlsx represent the detuning and the rows represent the frequencies of the Fourier spectrum. The values in the table represent transimission.</div> <div> </div> <div>The file "fig4a.xlsx" contains the phase diagram in Figure 4 of the main text. The columns of fig4a.xlsx represent the voltage of the RF-field, and the rows represent the frequencies of the Fourier spectrum. The values in the table represent transimission.</div> <div> </div> <div>The files "fig5a.xlsx" and "fig5a.2.xlsx" contain the phase diagrams in Figure 5 of the main text. The columns in fig5a.xlsx and fig5a.2.xlsx represent the voltages of the RF-field, and the rows represent the frequencies of the Fourier spectrum. The values in the table represent transimission.</div> <div> </div> <div>The files "fig7a.xlsx" and "fig7c.xlsx" contain the phase diagrams in Figure 7 of the main text. The columns in fig7a.xlsx and fig7c.xlsx represent the voltages of the RF-field, and the rows represent the frequencies of the Fourier spectrum. The values in the table represent transimission.</div>
Effect of Aging and Aerobic Fitness Level on Heat Dissipation
ClinicalTrials.gov study NCT04241900. IPD Sharing: UNDECIDED. Countries: 1. Publications: 0.
Data from: Cohort variation in individual body mass dissipates with age in large herbivores
Open the record for dataset details and reuse information.
Stellar models used in the paper "An efficient tidal dissipation mechanism via stellar magnetic fields"
<p>Data for stellar models used in the paper "An efficient tidal dissipation mechanism via stellar magnetic fields" (2024). </p> <p> </p> <p>We used MESA version r22.11.1 for these calculations.</p>
Suppression of dormancy through enhanced respiratory electron dissipation extends the lifespan of mycobacterial biofilms
GEO Series GSE305991. Mycolicibacterium smegmatis MC2 155. 12 samples. Type: Expression profiling by high throughput sequencing.
Imaging of Non-local Hot Electron Energy Dissipation via Shot Noise: Data deposit
<p>This content of this data deposit is the following:</p> <p>Archives ‘Data (Fig.1-3, and Fig.S1-S11)’: Raw data and executable files related to figures 1 to 3, and figures S1 to S11 of the publication</p>
In-situ Eddy Dissipation Rate (EDR) data (2019-2020) collected by aircraft of the China Eastern Airlines
<p>EDR observations are recorded onboard by equipment on the Boeing 737-8, B777-300ER, 109B787-9, and Airbus A319-115/-132/-133, A320-214/-232/-251N, A321-211/-231 of the CEA. These observations cover the whole year of 2019 and 2020. Each record contains: flight number, plane number, departure airport, destination airport, latitude, longitude, year, month, day, hour, minute, altitude(ft), air temperature, wind direction, wind speed, 1-min mean EDR<sup>1⁄3</sup> and 1-min peak EDR<sup>1⁄3</sup>.</p>
Tidal dissipation modelling in gas giant planets
<p>Gas giant planets are turbulent rotating magnetic objects that have strong and complex interactions with their environment. In such systems, the dissipation of tidal waves excited by tidal forces shape the orbital architecture and the rotational dynamics of the planets. During the last decade, a revolution has occurred for our understanding of tides in these systems and for our knowledge of the interiors of giant planets thanks to the space mission JUNO and the grand finale of the CASSINI mission. Our objective is thus to predict tidal dissipation using internal structure models, which agree with these latest observational constrains.</p> <p>To accomplish that, we build a new ab-initio model of tidal dissipation in giant planets that coherently takes into account the interactions of tidal waves with their complex structure. This model is a semi-global model in the planetary equatorial plane. We study the linear excitation of tidal (magneto-)gravito-inertial progressive waves and standing modes. We present here the general formalism and the potential regimes of parameters that should be explored. This will pave the way for full 3D numerical simulations that will take into account complex internal structure and dynamics of gas giant (exo-)planets.</p>
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