Planetary Modulation of Solar Activity

1967 ◽  
Vol 1 (2) ◽  
pp. 53-54 ◽  
Author(s):  
E. K. Bigg ◽  
P. S. Mulhall
Keyword(s):  
Solar Activity ◽  
Solar Surface ◽  
Relative Equilibrium ◽  
High Tide ◽  
The Other ◽  
The Sun ◽  
Sunspot Numbers ◽  
Tidal Forces ◽  
Wide Range ◽  
Degree Of Control

It has recently been shown that the planet Mercury exerts a small control on relative sunspot numbers, the degree of control depending on the positions of the other planets.This paper describes the results of extending the work to include all the planets.As a working hypothesis we have assumed that gravitational tidal forces induced on the Sun by the planets may modulate solar activity and have accordingly calculated relative equilibrium ‘high tide’ displacements of the solar surface for each day from the positions, masses and distances of the first six planets. Although the tides are very slight, the mass of displaced material is appreciable and varies over the very wide range of nearly 5 to 1.

scholarly journals Closing up onto our sun: solar imaging

2020 ◽  
Vol 240 ◽  
pp. 07011
Author(s):  
Kushagra Shrivastava ◽  
Keith Wen Kai Chia ◽  
Kang Jun Wong ◽  
Alfred Yong Liang Tan ◽  
Hwee Tiang Ning
Keyword(s):  
Solar Activity ◽  
The Sun ◽  
Research Needs ◽  
Large Numbers ◽  
Wide Range ◽  
Future Science ◽  
Insight Into ◽  
Term Data ◽  
Made In

Solar activity research provides insight into the Sun’s past, future (Science Daily, 2018). The solar activity includes observations of large numbers of intense sunspots, flares, and other phenomena; and demands a wide range of techniques and measurements on the observations. This research needs long term data collection before critical analyses can occur, to generate meaningful learning and knowledge. In this project, we will use solar imaging to make observations of solar activity, and take our baby steps to make contributions in citizen science. Observations will be made in 3 wavelengths to gain a more thorough analysis by looking at different perspectives of the Sun, namely H-Alpha, Calcium-K, and white light.

scholarly journals Magnetoconvection Patterns in Rotating Convection Zones

1991 ◽  
Vol 130 ◽  
pp. 37-56
Author(s):  
Paul H. Roberts
Keyword(s):  
Convection Zone ◽  
Solar Surface ◽  
Giant Cells ◽  
Conclusive Evidence ◽  
The Other ◽  
The Sun ◽  
Solar Convection Zone ◽  
Solar Convection ◽  
Entire Thickness ◽  
Convective Motions

AbstractIn addition to the well-known granulation and supergranulation of the solar convection zone (the “SCZ”), the presence of so-called “giant cells” has been postulated. These are supposed span the entire thickness of the SCZ and to stretch from pole to pole in a sequence of elongated cells like a “cartridge belt” or a bunch of “bananas” strung uniformly round the Sun. Conclusive evidence for the existence of such giant cells is still lacking, despite strenuous observational efforts to find them. After analyses of sunspot motion, Ribes and others believe that convective motions near the solar surface occurs in a pattern that is the antithesis of the cartridge belt: a system of “toroidal” or “doughnut” cells, girdling the Sun in a sequence that extends from one pole to the other. Galloway, Jones and Roberts have recently tried to meet the resulting theoretical challenge, with the mixed success reported in this paper.

scholarly journals Solar activity and solar oscillations

1997 ◽  
Vol 181 ◽  
pp. 277-285
Author(s):  
Y. Elsworth
Keyword(s):  
Magnetic Field ◽  
Solar Activity ◽  
Radio Emission ◽  
Surface Temperature ◽  
The Sun ◽  
Solar Oscillations ◽  
Thermal Component ◽  
X Ray ◽  
Convective Flows ◽  
Wide Range

Helioseismology provides us with the tools to probe solar activity. So that we can consider how the solar oscillations are influenced by that activity, we first consider the phenomena that we associate with the active Sun. The surface of the Sun is not quiet but shows evidence of convection on a wide range of scales from a few hundred kilometres through to several tens-of-thousands of kilometres. The surface temperature shows signs of the convection structures with the temperature in the bright granules being some 100 K to 200 K hotter than the surrounding dark lanes. Sunspots, which are regions of high magnetic field that suppress convective flows, are clearly visible to even quite crude observations. They are several tens-of-thousands of kilometres in diameter and about 2000 K cooler than their surroundings. Ultraviolet and X-ray pictures from satellites show that the higher layers of the solar atmosphere are very non-uniform with bright regions of high activity. Contemporaneous magnetograms show that these regions are associated with sunspots. Flares - regions of magnetic reconnections - are seen at all wavelengths from X-ray through the visible to radio. They are the non-thermal component of the radio emission of the Sun. There are many other indicators of activity on the Sun.

scholarly journals Monochromatic X-Ray Imagers of the Sun Based on the Bragg Crystal Optics

2021 ◽  
Vol 8 ◽  
Author(s):  
Anton A. Reva ◽  
Sergey V. Kuzin ◽  
Alexey S. Kirichenko ◽  
Artem S. Ulyanov ◽  
Ivan P. Loboda ◽  
...  
Keyword(s):  
Solar Activity ◽  
Solar Corona ◽  
Spectral Lines ◽  
Coronal Plasma ◽  
The Sun ◽  
Spectral Filter ◽  
Crystal Optics ◽  
X Ray ◽  
Hot Plasma ◽  
Wide Range

Investigations of solar activity require information about plasma in a wide range of temperatures. Generally, researchers require observations from telescopes producing monochromatic images of coronal plasma with cool, warm, and hot temperatures. Until now, monochromatic telescopic imaging has been made only in the Mg XII 8.42 Å line with the Mg XII spectroheliograph on board CORONAS-I, CORONAS-F, and CORONAS-PHOTON satellites. The Mg XII spectroheliograph used Bragg crystal optics. Its design is based on two main principles: (1) to select the working wavelength and the crystal in such a way that reflection occurs at small incident angles; (2) to use the aperture of the mirror as a spectral filter. We believe that these design principles can be applied to other spectral lines. In this article, we will review the design of the Mg XII spectroheliograph and present our thoughts on how to apply these principles to the Si XIV 6.18 Å and Si XIII 6.65 Å lines. A combination of the monochromatic Mg XII 8.42 Å, Si XIV 6.18 Å, and Si XIII 6.65 Å images will help us to study the dynamics of the hot plasma in the solar corona.

scholarly journals A Review of Solar Still Assessment with Various PCM Materials

2021 ◽  
pp. 14-18
Author(s):  
Pradeep Sen ◽  
Prof. Pankaj Badgaiyan ◽  
Prof. Bharat Girdhani ◽  
Prof. Shamir Daniel
Keyword(s):  
Fossil Fuels ◽  
High Salinity ◽  
The Other ◽  
Energy Sources ◽  
The Sun ◽  
Solar Still ◽  
Huge Amount ◽  
Solar Distillation ◽  
Wide Range ◽  
Shallow Basin

Solar distillation purifies water by transferring sun's heat to a simple device. A shallow basin with a glass shield makes up the majority of the system, which is usually referred to as a solar even now. Evaporation takes place when the pool water is heated by the sun. Humidity rises, condenses on the shield, and drips into a drip tray, leaving salts, minerals, as well as the majority of contaminants behind. The oceans, that have a high salinity, are now the only nearly inexhaustible source of water supply.Separating salts from seawater, on the other hand, necessitates a huge amount of energy, that also, when derived from fossil fuels, can be destructive to the environment. As a result, desalination of seawater must be done using environmentally friendly energy sources. PCM which are solar,  are widely used to store solar radiation during the day and release it in the evening, in a wide range of solar applications

scholarly journals On Activities of UV Cet-Type Flare Stars and of T Tau-Type Stars

1983 ◽  
Vol 71 ◽  
pp. 487-495
Author(s):  
R.E. Gershberg
Keyword(s):  
Solar Activity ◽  
Magnetic Fields ◽  
Physical Nature ◽  
The Other ◽  
Stellar Surface ◽  
The Sun ◽  
T Tau Type Stars ◽  
Flare Stars ◽  
Local Magnetic Fields ◽  
T Tau

Comparisons of the activities of UV Cet-type flare stars and of T Tau-type stars with solar activity permits the conclusion that non-sta-tionary processes in the UV Cet-type stars and in the Sun are of an indent ical physical nature but that they differ qualitatively from active events in the T Tau-type stars. The identity of the activity in flare stars and the Sun makes it possible to study successfully stellar activity with the help of known models of various solar events and, on the other hand, to have a more general approach to the physics and evolution of solar activity on the basis of established features of numerous flare stars of different ages and masses. The hypothesis on hydromagnetic activity of the T Tau-type stars is sketched; within this framework, one supposes that the main feature of such stars is an occurrence at every point of the stellar surface, of conditions necessary for the existence of dark spots, i.e. a lowering of the photospheric brightness due to strong local magnetic fields.

scholarly journals Panoramic Analyzer of Radio Spectra — Instrument for Measurements of Coronal Magnetic Fields on the Sun

1993 ◽  
Vol 141 ◽  
pp. 306-309 ◽  
Author(s):  
V. M. Bogod ◽  
S. M. Vatrushin ◽  
V. E. Abramov-Maximov ◽  
S. V. Tsvetkov ◽  
V. N. Dikij
Keyword(s):  
Solar Activity ◽  
Magnetic Fields ◽  
Plasma Diagnostics ◽  
Solar Radio ◽  
High Spatial Resolution ◽  
Solar Radio Emission ◽  
The Sun ◽  
Wide Range ◽  
Coronal Magnetic Fields ◽  
Special Value

The study of solar radio emission in a wide (covering many octaves) wavelength range is of great importance for plasma diagnostics of all types of solar activity. Here we describe a new spectroanalyzer covering a wide range in frequency from 1 to 18 GHz, which is used at the RATAN-600 radio telescope beginning 1991 December 20. Coronal magnetic fields have been measured with the various radio astronomical methods presented in these proceedings by Gelfreikh et al. and Bogod et al.Of special value are collaborative spectral-polarization observations using the RATAN-600 and high-spatial resolution observations with the VLA and WSRT (Akhmedov et al. 1986; Bogod et al. 1992; Alissandrakis et al. 1992).

scholarly journals On the Dimension of the Solar Activity Attractor

1993 ◽  
Vol 157 ◽  
pp. 91-95
Author(s):  
C.M. Orzaru
Keyword(s):  
Dynamical System ◽  
Time Series ◽  
Solar Activity ◽  
Correlation Dimension ◽  
Chaotic Behaviour ◽  
The Other ◽  
Short Series ◽  
Sunspot Numbers ◽  
First Case ◽  
Characteristic Measure

The correlation dimension D(2) as a characteristic measure of the regular or chaotic behaviour of the solar dynamical system has been calculated. The algorithm suggested by Grassberger and Procaccia (1983) has been applied to time series of relative sunspot numbers and of areas of sunspots and faculae. In the first case, a correlation dimension D(2) ≃ 1.5 has been found; in the other two cases, the algorithm was not convergent, the results obtained being not relevant, due to the too short series of data available.

scholarly journals Are Solar Wind Measurements of Different Spacecraft Consistent?

1980 ◽  
Vol 91 ◽  
pp. 151-154
Author(s):  
R. Steinitz ◽  
M. Eyni
Keyword(s):  
Solar Wind ◽  
Solar Activity ◽  
Boundary Conditions ◽  
Activity Cycle ◽  
Solar Activity Cycle ◽  
The Other ◽  
The Sun ◽  
Spatial Gradients ◽  
Wind Measurements ◽  
The One

Results of solar wind measurements by different spacecraft are not always in full accord. Such measurements are in general not from one and the same distance r from the sun, nor are they taken at the same phase of the solar activity cycle. One would like to be able to discriminate between spacecraft calibration effects on the one hand, and solar wind variations which reflect true spatial gradients or changing boundary conditions at the sun on the other hand. Accordingly, we examine in this paper the possibility of reconciling the apparent discrepancies.

scholarly journals The connection between solar wind charged particles and tornadoes: Case analysis

2013 ◽  
Vol 28 (1) ◽  
pp. 52-59 ◽  
Author(s):  
Milan Radovanovic ◽  
Bosko Milovanovic ◽  
Mila Pavlovic ◽  
Aleksandar Radivojevic ◽  
Milan Stevancevic
Keyword(s):  
Solar Wind ◽  
Solar Activity ◽  
Low Temperatures ◽  
Charged Particles ◽  
Case Analysis ◽  
The Other ◽  
Mass Movements ◽  
The Sun ◽  
Air Mass ◽  
Potential Link

The temperature of charged particles coming from the Sun ranges from several hundred thousands to several millions ?C, in extreme cases. Theoretical possibilities of the hydrodynamic air mass seizing by charged particles, i. e. solar wind, are discussed in this paper. On one hand, they are characterized by extremely high temperatures, on the other, by the compression of cold air at an approximate altitude of 90 km towards the top of the cloud of the cyclone, they influence the phenomenon of extremely low temperatures. By using the Mann-Whitney U test we have tried to determine the potential link between certain indicators of solar activity and resulting disturbances in the atmosphere. Analyzed data refer to global daily values for the 2004-2010 period. Our results confirm the possibility of coupling between the charged particles and the vortex air mass movements, based on which a more detailed study of the appearance of a tornado near Sombor on May 12th, 2010, was carried out. It has also been proven that there are grounds for a causality between the sudden arrival of the solar wind charged particles, i. e. protons, and the appearance of a tornado. Based on the presented approach, elements for an entirely novel prediction model are given.

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