https://ankitbarik.github.io/tags/fluid-dynamics/Fluid DynamicsHugoBlox Kit (https://hugoblox.com)en-usSun, 01 Jan 2017 00:00:00 +0000https://ankitbarik.github.io/media/icon_hu_448d1a2715075a0c.pnghttps://ankitbarik.github.io/tags/fluid-dynamics/https://ankitbarik.github.io/project/couette/Sun, 01 Jan 2017 00:00:00 +0000https://ankitbarik.github.io/project/couette/<img src="vpInerMod.png"> <p style="text-align: justify;">The spherical Couette system is the spherical analogue of the classic Taylor-Couette setup, with two concentric coaxial differentially rotating spherical spheres. The space between the spheres is filled with a fluid which is viscously driven. This is the setup used by the new generation of dynamo experiments such as the three meter experiment in College Park, Maryland and the DTS Experiment in Grenoble, France. This provides a more accurate geometry akin to planetary and stellar interiors and provides a relatively simpler system to study various fluid instabilities and turbulence in spherical shells.</p> <p style="text-align: justify;">I studied this system during my PhD (see thesis ). My simulations successfully reproduced experimental observations in the experiments at Cottbus by . There are a number of interesting questions that we attempted to answer in our work. First was the onset of <strong>global inertial modes</strong> by differential rotation itself. Second is the <strong>transition to turbulence</strong> at a critical differential rotation. Our addresses the first question while the second is under review which addresses the second question.</p>https://ankitbarik.github.io/project/convection/Mon, 01 Jan 0001 00:00:00 +0000https://ankitbarik.github.io/project/convection/<img src="sol_quad.png" width=80%> <p style="text-align: justify;">Convection in rotating spherical shells is ubiquitous in planets and stars. Before fully understanding the nonlinear process, we must make efforts in understanding the linear part - the onset of convection. Though this has been an active area of research since the times of Chandrasekhar, very little work had been done in understanding how the critical parameters of convection vary with the aspect ratio of a spherical shell $\chi=r_i/r_o$ . We used the eigenvalue code to compute the critical onset of convection across four decades in rotation rate (Ekman number) and for $0.05\leq\chi\leq 0.95$ , spanning almost all possible cases in astrophysical objects. The database has been made openly available and is being used by other publications to understand where in the physical regime their simulations are. For more information, you can read the (open access) publication.</p>