The dynamics of the quiet solar atmosphere are highly nonlinear. Both the standing waves of solar oscillations and acoustic waves generated in the upper convection zone become nonlinear in the atmosphere and transform into shock waves. Interactions of shock waves, the formation of contact discontinuities, and interactions of shocks with these discontinuities will occur. The strong nonlinear dyn...

In this paper we advocate for the idea that two seemingly unrelated mysteries with almost 90 year history -- nature of dark matter and million-degree solar corona may be but sides same coin axions born in core Sun photons axion origin corona, whose modulations are controlled by anticorrelated modulation asymmetric (ADM) density interior.

We present observations of a long-lived solar filament cavity with soft X-ray sources along its axis. This structure appeared above the southern polar crown polarity-inversion line for approximately three rotations during 1997 June–August, centered at a west-limb passage on approximately July 3. At the limb, the Yohkoh soft Xray data showed a bright region situated above and around the projecte...

The temporal relationship between coronal mass ejections (CMEs) and associated solar Ñares is of great importance to understanding the origin of CMEs, but it has been difficult to study owing to the nature of CME detection. In this paper, we investigate this issue using the Large Angle and Spectrometric Coronagraph and the EUV Imaging Telescope observations combined with GOES soft X-ray observa...

The magnetic field topology at the coronal mass ejection (CME) source regions has been one of the major focuses of CME initiationmodels.While the ‘‘breakout’’ model requires a quadrupolar magnetic topology in the solar corona to enable an eruption, other models have shown that a bipolar magnetic topology can be the source region of a CME. In this paper, we use observational data and a potential...

We describe a simple analytic model for the magnetic field in the solar corona and interplanetary space which is appropriate to solar minimum conditions. The model combines an azimuthal current sheet in the equatorial plane with an axisymmetric multipole field representing the internal magnetic field of the Sun. The radial component of the field filling interplanetary space is approximately mon...

A heliospheric density model is derived by evaluating the spherical solutions of magnetohydrostatic equations including the thermal pressure and the gravitational force of the Sun. The model resulting as a special solution of Parker’s wind equation covers a range from the low corona up to 5 AU and, surprisingly, agrees very well with observations. Such a model is required for the interpretation...

Accurate determination of photospheric solar abundances requires detailed modeling of the solar granulation and accounting for departures from local thermodynamical equilibrium (LTE). We argue that the forbidden C I line at 8727 Å is largely immune to departures from LTE, and can be realistically modeled using LTE radiative transfer in a time-dependent three-dimensional simulation of solar surf...

We analyze the evolution of shock waves in high-resolution 3D radiative MHD simulations quiet Sun and their synthetic emission characteristics. The model dynamics a 12.8x12.8x15.2 Mm quiet-Sun region (including 5.2 layer upper convection zone 10 atmosphere from photosphere to corona) with an initially uniform vertical magnetic field G, naturally driven by convective flows. synthesize Mg II C sp...