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S. Ravichandran

Publications and source records attributed to S. Ravichandran.

28 records · Page 2Linked to original sources

Non-Precipitating Shallow Cumulus Clouds: Theory and Direct Numerical Simulation

We model cumulus clouds as transient diabatic plumes, and present a single-fluid formulation for the study of the dynamics of developing shallow cumulus clouds. The fluid, air, carries water vapour and liquid water as scalars that are advected with the flow. We employ the Boussinesq approximation and a simplified form of the Clausius-Clapeyron law for phase changes. We use this formulation to study the ambient conditions required for the formation of cumulus clouds. We show that the temperature lapse rate in the ambient and the relative humidity of the ambient are crucial in deciding when cumulus clouds form. In the phase-space of these two parameters, we determine the boundary that separates the regions where cumulus clouds can form and where they cannot.

physics.flu-dyn↗

The Diffuse Ultraviolet and Optical Background: Status and Future Prospects

The ultraviolet and optical background forms a baseline for any observation of the sky. It includes emission lines and scattered light from the atmosphere; resonant scattering from the Lyman lines of interplanetary hydrogen and the scattering of sunlight from Solar System dust (zodiacal light); scattering of starlight from interstellar dust (DGL) with emission from molecular hydrogen fluorescence or from line emission in selected areas; and an extragalactic component seen most easily at high Galactic latitudes. We will discuss the different components of the diffuse radiation field in the UV and the optical. We close with a hope that there will be new observations from missions near the edge of the Solar System.

astro-ph.GA↗

Components of the Diffuse Ultraviolet Radiation at High Latitudes

We have used data from the Galaxy Evolution Explorer to study the different components of the diffuse ultraviolet background in the region between the Galactic latitudes 70-80 degree. We find an offset at zero dust column density (E(B - V) = 0) of $240 \pm 18$ photon units in the FUV (1539A) and $394 \pm 37$ photon units in the NUV (2316A). This is approximately half of the total observed radiation with the remainder divided between an extragalactic component of $114 \pm 18$ photon units in the FUV and $194 \pm 37$ photon units in the NUV and starlight scattered by Galactic dust at high latitudes. The optical constants of the dust grains were found to be a=0.4$\pm$0.1 and g=0.8$\pm$0.1 (FUV) and a=0.4$\pm$0.1 and g=0.5$\pm$0.1 (NUV). We cannot differentiate between a Galactic or extragalactic origin for the zero-offset but can affirm that it is not from any known source.

astro-ph.GA↗

Understanding droplet collisions through a model flow: Insights from a Burgers vortex

We investigate the role of intense vortical structures, similar to those in a turbulent flow, in enhancing collisions (and coalescences) which lead to the formation of large aggregates in particle-laden flows. By using a Burgers vortex model, we show, in particular, that vortex stretching significantly enhances sharp inhomogeneities in spatial particle densities, related to the rapid ejection of particles from intense vortices. Furthermore our work shows how such spatial clustering leads to an enhancement of collision rates and extreme statistics of collisional velocities. We also study the role of poly-disperse suspensions in this enhancement. Our work uncovers an important principle which, {if valid for realistic turbulent flows, may be a factor in} how small nuclei water droplets in warm clouds can aggregate to sizes large enough to trigger rain.

physics.flu-dyn↗

The Diffuse Radiation Field at High Galactic Latitudes

We have used GALEX observations of the North and South Galactic poles to study the diffuse ultraviolet background at locations where the Galactic light is expected to be at a minimum. We find offsets of 230 -- 290 photon units in the FUV (1531 Å) and 480 -- 580 photon units in the NUV (2361 Å). Of this, approximately 120 photon units can be ascribed to dust scattered light and another 110 (190 in the NUV) photon units to extragalactic radiation. The remaining radiation is, as yet, unidentified and amounts to $120 -- 180$ photon units in the FUV and $300 -- 400$ photon units in the NUV. We find that molecular hydrogen fluorescence contributes to the FUV when the 100 $μ$m surface brightness is greater than 1.08 MJy sr$^{-1}$.

astro-ph.GA↗

Dynamics of circular arrangements of vorticity in two dimensions

The merger of two like-signed vortices is a well-studied problem, but in a turbulent flow, we may often have more than two like-signed vortices interacting. We study the merger of three or more identical co-rotating vortices initially arranged on the vertices of a regular polygon. At low to moderate Reynolds numbers, we find an additional stage in the merger process, absent in the merger of two vortices, where an annular vortical structure is formed and is long-lived. Vortex merger is slowed down significantly due to this. Such annular vortices are known at far higher Reynolds numbers in studies of tropical cyclones, which have been noticed to a break down into individual vortices. In the pre-annular stage, vortical structures in a viscous flow are found here to tilt and realign in a manner similar to the inviscid case, but the pronounced filaments visible in the latter are practically absent in the former. Interestingly at higher Reynolds numbers, the merger of an odd number of vortices is found to proceed very differently from that of an even number. The former process is rapid and chaotic whereas the latter proceeds more slowly via pairing events. The annular vortex takes the form of a generalised Lamb-Oseen vortex (GLO), and diffuses inwards until it forms a standard Lamb-Oseen vortex. For lower Reynolds number, the numerical (fully nonlinear) evolution of the GLO vortex follows exactly the analytical evolution until merger. At higher Reynolds numbers, the annulus goes through instabilities whose nonlinear stages show a pronounced difference between even and odd mode disturbances. It is hoped that the present findings, that multiple vortex merger is qualitatively different from the merger of two vortices, will motivate studies on how multiple vortex interactions affect the inverse cascade in two-dimensional turbulence.

physics.flu-dyn↗

Caustics and clustering in the vicinity of a vortex

We study the formation of caustics in vortex-dominated \flows. We \find that only particles starting within a critical distance of a vortex which scales as the square roots of the particle inertia and the circulation can form sling caustics. We show that particles starting in an annular region around this critical radius contribute the densest clusters in the \flow. The large density spikes occurring for such particles, even at small inertia, are indicative that these particles will experience large collision rates.

physics.flu-dyn↗

Attracting fixed points for heavy particles in the vicinity of a vortex pair

We study the behaviour of heavy inertial particles in the flow field of two like-signed vortices. In a frame co-rotating with the two vortices, we find that stable fixed points exist for these heavy inertial particles; these stable frame-fixed points exist only for particle Stokes number $St<St_{cr}$. We estimate $St_{cr}$ and compare this with direct numerical simulations, and find that the addition of viscosity increases the $St_{cr}$ slightly. We also find that the fixed points become more stable with increasing $St$ until they abruptly disappear at $St=St_{cr}$. These frame-fixed points are between fixed points and limit cycles in character.

physics.flu-dyn↗

Large Scale Extinction Maps with UVIT

The Ultraviolet Imaging Telescope (UVIT) is scheduled to be launched as a part of the ASTROSAT satellite. As part of the mission planning for the instrument we have studied the efficacy of UVIT observations for interstellar extinction measurements. We find that in the best case scenario, the UVIT can measure the reddening to an accuracy of about 0.02 magnitudes, which combined with the derived distances to the stars, will enable us to model the three-dimensional distribution of extinction in our Galaxy. The knowledge of the distribution of the ISM will then be used to study distant objects, affected by it. This work points the way to further refining the UVIT mission plan to best satisfy different science studies.

astro-ph.IM↗

Autogenic Training With Natural Language Processing Modules: A Recent Tool For Certain Neuro Cognitive Studies

Learning to respond to voice-text input involves the subject's ability in understanding the phonetic and text based contents and his/her ability to communicate based on his/her experience. The neuro-cognitive facility of the subject has to support two important domains in order to make the learning process complete. In many cases, though the understanding is complete, the response is partial. This is one valid reason why we need to support the information from the subject with scalable techniques such as Natural Language Processing (NLP) for abstraction of the contents from the output. This paper explores the feasibility of using NLP modules interlaced with Neural Networks to perform the required task in autogenic training related to medical applications.

cs.AI↗