Search arXiv⌕ Search

arXiv · 1001.4331

On the flare induced high-frequency global waves in the Sun

Abstract

Recently, Karoff and Kjeldsen (2008) presented evidence of strong correlation between the energy in the high-frequency part (5.3<ν<8.3 mHz) of the acoustic spectrum of the Sun and the solar X-ray flux. They have used disk-integrated intensity observations of the Sun obtained from the VIRGO (Variability of solar IRradiance and Gravity Oscillations) instrument on board SOHO (Solar and Heliospheric Observatory) spacecraft. Similar signature of flares in velocity observations has not been confirmed till now. The study of low-degree high-frequency waves in the Sun is important for our understanding of the dynamics of the deeper solar layers. In this paper, we present the analysis of the velocity observations of the Sun obtained from the MDI (Michelson and Doppler Imager) and the GOLF (Global Oscillations at Low Frequencies) instruments on board SOHO for some major flare events of the solar cycle 23. Application of wavelet techniques to the time series of disk-integrated velocity signals from the solar surface using the full-disk Dopplergrams obtained from the MDI clearly indicates that there is enhancement of high-frequency global waves in the Sun during the flares. This signature of flares is also visible in the Fourier Power Spectrum of these velocity oscillations. On the other hand, the analysis of disk-integrated velocity observations obtained from the GOLF shows only marginal evidence of effects of flares on high-frequency oscillations.

Explore related subjects

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

Brajesh Kumar, Savita Mathur, R. A. Garcia, P. Venkatakrishnan. 2010-01-25. On the flare induced high-frequency global waves in the Sun. https://doi.org/10.1088/2041-8205%2F711%2F1%2Fl12

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

High-Precision Differential Radial Velocities of C3PO Wide Binaries: A Test of Modified Newtonian Dynamics (MOND)

Wide-binary stars, separated by thousands of AU, reside in low-acceleration regimes where Modified Newtonian Dynamics (MOND) predicts deviation from Newtonian gravity. However, Gaia radial velocities (RVs) lack the precision to resolve the small velocity differences expected in these systems, limiting previous MOND analyses to two-dimensional kinematics. In this paper, we introduce a technique to measure differential RVs of wide binary stars using high resolution, high signal-to-noise spectra. We apply this method to measure differential RVs of 85 wide-binaries from the C3PO survey and achieved precisions of $\sim$8-15 m/s per binary pair, a $\sim 10$-$100\times$ improvement (median $\sim 24\times$) over Gaia DR3. After applying a selection criterion based on the scaled velocity, we retain 57 gravitationally bound systems for further analysis. Combining these measurements with Gaia astrometry, we construct a hierarchical Bayesian model to infer the orbital elements of all wide-binary pairs and the global MOND acceleration scale ($a_0$). We test two commonly used interpolating functions in MOND formulation: the simple form ($b=1$, $μ= x/(1+x)$) and the standard form ($b=2$, $μ= x/\sqrt{1+x^2}$). Our results indicate tension with MOND at the presently accepted $a_0$ value: for $b=1$, the canonical value is excluded at $2.5σ$, while for $b=2$, the exclusion is at $1.5σ$. We discuss how systematic uncertainties in the external field effect treatment, particularly in the transition regime, may affect these conclusions.

astro-ph.SR↗

Collisionless stationary states of a stratified plasma in an expanding magnetic tube with stochastic heating

We investigate the collisionless kinetic structure of the upper solar atmosphere in an expanding magnetic field. Building on established velocity-filtration models, we extend the stochastic multi-temperature framework developed in previous works by including magnetic-field expansion and magnetic-moment conservation. Stochastic heating generates a non-Maxwellian boundary distribution through the superposition of particle populations associated with different temperatures. We consider a stationary two-component plasma confined within an expanding magnetic flux tube and subject to gravity, self-consistent electrostatic interactions, the Pannekoek--Rosseland electric field, and magnetic-moment conservation. Starting from the Vlasov equation, we derive fully analytical expressions for the distribution functions, density, and parallel, perpendicular, and total temperature profiles. The combined conservation of energy and magnetic moment generates a loss-cone distribution, reducing the density relative to the unmagnetized case and producing temperature anisotropy. For a single-temperature boundary, the competition between gravity and magnetic-moment conservation produces a maximum in the parallel temperature, for which we derive and numerically validate analytical scaling laws. With stochastic heating, gravitational filtering enhances the contribution of hotter populations at coronal heights, while magnetic-moment conservation amplifies the velocity-space anisotropy. Our analytical solution provides a collisionless benchmark for future kinetic models incorporating more realistic magnetic-field geometries, Coulomb collisions, and turbulent particle scattering.

astro-ph.SR↗

3D simulations of magnetospheric accretion in T Tauri stars: I. Disk truncation, stellar torques, and application to observations

Young stars accrete material from their circumstellar disk through their magnetosphere and undergo contraction; these two processes impact their rotational evolution. We investigate stable and unstable accretion regimes (due to the interchange instability) and examine the associated stellar torques to assess the spin evolution of young stars. We performed 3D MHD simulations of disk accretion onto an inclined stellar dipole. We ran 21 simulations with varying stellar rotation rates, dipole field strengths and obliquities, and mass accretion rates. We find that stars with a ratio of truncation to corotation radius $R_t/R_{co} \gtrsim 0.80-0.85$ accrete via a stable regime, while accretion becomes unstable otherwise. In addition, our $R_t/R_{\ast}$ parametrization weakly depends on the mass accretion rate and the dipolar intensity, while strongly depending on the stellar rotation rate. We derive torque formulae for each flow component affecting the stellar rotation, i.e., accretion, magnetospheric ejections and stellar winds. Finally, we apply our results to a sample of young stars with measured magnetic fields, mass accretion rates, and rotational periods and find that most of them should currently accrete in an unstable regime and undergo spin-up torques. Our study confirms and expands upon previous results. Unstable accretion should lead to a net spin-up torque on the central star, while stable accretion can lead to stellar spin-down. When applying our truncation radius and torque prescriptions to observational data, we find that most young stars in our sample should be in a spin-up state. Thus, the angular momentum problem for young stars remains.

astro-ph.SR↗