Abstract The solar meridional flow is a crucial ingredient in modern dynamo theory. Seismic estimates of this have, however, been contradictory deeper layers below about <?CDATA $0.9\,{R}_{\odot }$?> . Results from time−distance helioseismology have so far obtained using the ray approximation. Here, we perform inversions Born initial result similar to previously by Jackiewicz et al. kernels while same set GONG data and SOLA inversion technique. However, show that assumption uncorrelated...

We extend an existing Born approximation method for calculating the linear sensitivity of helioseismic travel times to flows from Cartesian spherical geometry. This development is necessary using inferring large-scale in deep solar interior. In a first sanity check, we compare two $f-$mode kernels our and method. The horizontal total integrals agree within 0.3 %. As second consistency test, consider uniformly rotating Sun distance 42 degrees. analytical travel-time difference agrees with...

Context. Solar gravity modes ( g modes) are buoyancy waves that trapped in the solar radiative zone and have been very difficult to detect at surface. would complement pressure p probing central regions of Sun, for example rotation rate core. Aims. A detection using changes large frequency separation has recently reported. However, it is unclear how interact. The aim this study evaluate what extent can perturb frequencies modes. Methods. We computed first-order perturbation global -mode due...

The precise mechanism that forms jets and large-scale vortices on the giant planets is unknown. An inverse cascade has been suggested. Alternatively, energy may be directly injected by small-scale convection. Our aim to clarify whether an feeds zonal eddies in a system of rapidly rotating, deep, geostrophic spherical-shell We analyze nonlinear scale-to-scale transfer kinetic such simulations as function azimuthal wave number, m. find main driving associated with upscale from small convective...

Accurate measurements of deep solar meridional flow are vital interest for understanding the dynamo. In this paper, we validate a recently developed method obtaining sensitivity functions (kernels) travel-time to interior flows using Born approximation in spherical geometry, which is expected be more accurate than classical ray approximation. Furthermore, develop numerical approach efficiently compute large number kernels based on separability eigenfunctions into their horizontal and radial...

All planets and stars rotate. gas in our solar system, the Sun, many show a pattern of east- or westward mean flows. This phenomenon is known as differential rotation stellar zonal jets planetary context. Observations, laboratory experiments simulations that flow kinetic energy scales like $\ell^{-5}$, where $\ell$ spherical harmonic degree (which effectively latitudinal wave number). Here, we analyze observation well dynamics Saturn outer atmosphere an ultra-hot Jupiter. While these systems...

Hot Jupiters are tidally-locked Jupiter-sized planets close to their host star. They have equilibrium temperatures above about 1000 K. Photometric observations find that the hotspot, hottest location in atmosphere, is shifted with respect substellar point. Some show eastward and some westward hotspot offsets, while hydrodynamic simulations an offset due advection by characteristic mean flow. In particular for ultra-hot 2000 Kelvin, electromagnetic effects must be considered since...

Context. The spatial power spectrum of supergranulation does not fully characterize the underlying physics turbulent convection. For example, it describe non-Gaussianity in horizontal flow divergence. Aims. Our aim is to statistically pattern solar beyond spectrum. next-order statistic bispectrum. It measures correlations three Fourier components and related nonlinearities physics. Methods. We estimated bispectrum supergranular surface divergence maps that were obtained using local...

Abstract Recent helioseismic estimates of the deep solar meridional flow have been contradictory. Using two years worth GONG data, I show here that detection is ambiguous below about 0.85 radii.

Context. Understanding convection is important in stellar physics, for example, when it an input evolution models. Helioseismic estimates of convective flow amplitudes deeper regions the solar interior disagree by orders magnitude among themselves and with simulations. Aims. We aim to assess validity existing upper limit at a depth 0.96 radii obtained using time-distance helioseismology several simplifying assumptions. Methods. generated synthetic observations fields from magnetohydrodynamic...

&amp;lt;p&amp;gt;In this study, we analyse the non-linear transfer of kinetic energy in simulations convection a 3D rotating shell. Our aim is to understand role upscale and potential inverse cascade for formation zonal jets and&amp;amp;#160;large vortices on giant planets Jupiter Saturn. We find that main driving associated with directly from scale jets. This mediated by Reynolds stresses, i.e. statistical correlations velocity components small-scale flow.&amp;amp;#160; Intermediate scales...

The precise mechanism that forms jets and large-scale vortices on the giant planets is unknown. An inverse cascade has been suggested. Alternatively, energy may be directly injected by small-scale convection. Our aim to clarify whether an feeds zonal eddies in a system of rapidly rotating, deep, geostrophic spherical-shell We analyze nonlinear scale-to-scale transfer kinetic such simulations as function azimuthal wave number, m. find main driving associated with upscale from small convective...

&amp;lt;p&amp;gt;Turbulent convection is generally believed to occur on the Sun three different characteristic length scales. These are smaller granulation scale, intermediate supergranulation and potentially existing giant cell scale. While mostly understood, there several competing theories for emergence of supergranules as a scale coherent phenomenon. prevailing approaches assume convective origin supergranulation, others follow path potential wave-like behaviour these features, because...