arXiv subjects

G. Kishore

Publications and source records attributed to G. Kishore.

5 recordsLinked to original sources

arXiv2025

The spectra of solar magnetic energy and helicity

Previous studies have used magnetic energy and helicity spectra, the latter computed using the two-scale method, to search for signatures of mean-field dynamos. In this study, we compare cotemporal HMI and SOLIS magnetograms to illustrate the instrument-dependence of even qualitative features of the energy and helicity spectra. Around the minimum between solar cycles 24 and 25, we find that the magnetic energy spectrum computed from HMI observations exhibits two distinct peaks. One of these peaks is only present near the cycle minimum, and corresponds to large-scale magnetic fields at high latitudes. Nevertheless, such magnetic fields are not present in contemporaneous synoptic vector magnetograms from SOLIS. Further, even when magnetograms from both the instruments are apodized, the helicity spectra calculated using the two-scale method disagree (on both the sign and the value of the fractional helicity). This suggests that currently available synoptic magnetograms are not reliable enough for such studies.

astro-ph.SR↗

arXiv2025

Rotational effects on the small-scale dynamo

Using direct numerical simulations of forced rotating turbulence, we study the effect of rotation on the growth rate and the saturation level of the small-scale dynamo. For slow rotation rates, increasing the rotation rate reduces both the growth rate and the saturation level. Once the rotation rate crosses a threshold, large-scale vortices are formed which enhance the growth rate and the saturation level. Below this threshold, the suppression of the small-scale dynamo with increasing rotation is explained by the fact that at scales close to, but smaller than, the forcing scale, rotating turbulence is one-dimensionalized, with the velocity component along the rotation axis being larger than the other two components. This is due to the rotational destabilization of vortices produced by the forcing function. While the rotational effect on the growth rate becomes small at high Re, the ratio of the steady-state magnetic to kinetic energies remains suppressed by up to 35% as compared to the non-rotating case.

physics.flu-dyn↗

arXiv2025

Turbulent transport in a non-Markovian velocity field

The commonly used quasilinear approximation allows one to calculate the turbulent transport coefficients for the mean of a passive scalar or a magnetic field in a given velocity field. Formally, the quasilinear approximation is exact when the correlation time of the velocity field is zero. We calculate the lowest-order corrections to the transport coefficients due to the correlation time being nonzero. For this, we use the Furutsu-Novikov theorem, which allows one to express the turbulent transport coefficients in a Gaussian random velocity field as a series in the correlation time. We find that the turbulent diffusivities of both the mean passive scalar and the mean magnetic field are suppressed. Nevertheless, contradicting a previous study, we show that the turbulent diffusivity of the mean magnetic field is smaller than that of the mean passive scalar. We also find corrections to the $\alpha$ effect.

physics.flu-dyn↗

arXiv2024

Strengthening of the f mode due to subsurface magnetic fields in simulations of convection

Previous studies have found that localized strengthening of the f mode recedes the emergence of active regions on the Sun by one day to three days. To help interpret these observations, we have performed nonlinear simulations of convection with imposed magnetic fields at different depths. We find that the f mode is strengthened when a super-equipartition magnetic field is imposed near the top of the domain. However, neither a magnetic field of equal strength near the bottom of the domain nor an equipartition magnetic field near the top of the domain have a significant effect. Our results suggest that the magnetic precursors of active regions are present near the surface of the Sun for much longer than would be expected if active regions were formed by flux tubes rising from deep within the convection zone. Application to observations should account for the fact that the effects we observe are transient.

astro-ph.SR↗

arXiv2021

Local time of an Ornstein-Uhlenbeck particle

In this paper, we study the local time spent by an Ornstein-Uhlenbeck particle at some location till time t. Using the Feynman-Kac formalism, the computation of the moment generating function of the local time can be mapped to the problem of finding the eigenvalues and eigenfunctions of a quantum particle. We employ quantum perturbation theory to compute the eigenvalues and eigenfunctions in powers of the argument of the moment generating function which particularly help to directly compute the cumulants and correlations among local times spent at different locations. In particular, we obtain explicit expressions of the mean, variance, and covariance of the local times in the presence and in the absence of an absorbing boundary, conditioned on survival. In the absence of absorbing boundaries, we also study large deviations of the local time and compute exact asymptotic forms of the associated large deviation functions explicitly. In the second part of the paper, we extend our study of the statistics of local time of the Ornstein-Uhlenbeck particle to the case not conditioned on survival. In this case, one expects the distribution of the local time to reach a stationary distribution in the large time limit. Computations of such stationary distributions are known in the literature as the problem of first passage functionals. In this paper, we study the approach to this stationary state with time by providing a general formulation for evaluating the moment generating function. From this moment generating function, we compute the cumulants of the local time exhibiting the approach to the stationary values explicitly for a free particle and a Ornstein-Uhlenbeck particle. Our analytical results are verified and supported by numerical simulations.

cond-mat.stat-mech↗