Solar phenomena Solar phenomena The Babcock Model describes a mechanism which can explain magnetic and sunspot patterns observed on the Sun. ...more on Wikipedia about "Babcock Model"
The Bastille Day Flare or Bastille Day Event was a powerful solar flare on July 14, 2000 occurring near the peak of the solar maximum. Active region 9077 produced an X5-class flare, which caused an S3 radiation storm on Earth fifteen minutes later as energetic protons bombarded the ionosphere. The proton event was four times more intense than any previously recorded. The flare was followed by a full-halo coronal mass ejection. ...more on Wikipedia about "Bastille Day Flare"
A coronal mass ejection (CME) is a solar event which involves a burst of plasma consisting primarily of electrons and protons (in addition to small quantities of heavier elements such as helium, oxygen, and iron). When these CMEs reach the Earth, they often disrupt the Earth's magnetosphere, compressing it on the dayside and extending the nightside tail. When the magnetosphere reconnects on the nightside, it creates trillions of watts of power which is directed back towards the Earth's upper atmosphere. This process can cause particularly strong aurora or also known as Northern Lights. CME events, along with solar flares, can disrupt radio transmissions, cause power outages (blackouts), and cause damage to satellites and electrical transmission lines. ...more on Wikipedia about "Coronal mass ejection"
The Evershed effect, named after the Britist astronomer John Evershed, is the radial flow of gas across the photospheric surface of the penumbra of sunspots from the inner border with the umbra towards the outer edge. ...more on Wikipedia about "Evershed effect"
A facula (plural: faculae) is literally a "bright spot." It is used in planetary nomenclature for naming certain surface features of planets and moons, and is also a type of surface phenomenon on the Sun. ...more on Wikipedia about "Facula"
A Forbush decrease is a rapid decrease in the observed galactic cosmic ray intensity following a coronal mass ejection (CME). It occurs due to the magnetic field of the plasma solar wind sweeping some of the galactic cosmic rays away from Earth. ...more on Wikipedia about "Forbush decrease"
The Gnevyshev-Ohl rule is an empirical rule according to which the sum of sunspot numbers over an odd cycle exceeds that of the preceding even cycle. ...more on Wikipedia about "Gnevyshev-Ohl rule"
Limb darkening refers to the diminishing of intensity in the image of a star as one moves from the center of the image to the edge or "limb" of the image. Limb darkening occurs as the result of two effects: ...more on Wikipedia about "Limb darkening"
Magnetic reconnection is the process whereby magnetic field lines from different magnetic domains are spliced to one another, changing the overall topology of a magnetic field. It is a violation of an approximate conservation law in plasma physics, and can concentrate mechanical or magnetic energy in both space and time. Solar flares, the largest explosions in the solar system, are caused by reconnection of large systems of magnetic flux on the Sun, releasing in minutes energy that is stored in the magnetic field over a period of weeks to years. Magnetic reconnection in Earth's magnetosphere is responsible for the aurora, and it is important to the science of controlled nuclear fusion because it is one mechanism preventing magnetic confinement of the fusion fuel. ...more on Wikipedia about "Magnetic reconnection"
The Maunder Minimum is the name given to the period roughly from 1645 to 1715 A.D., when sunspots became exceedingly rare, as noted by solar observers of the time. It is named after the later solar astronomer E.W. Maunder who discovered the dearth of sunspots during that period by studying records from those years. During one 30-year period within the Maunder Minimum, for example, astronomers observed only about 50 sunspots, as opposed to a more typical 40,000–50,000 spots. ...more on Wikipedia about "Maunder Minimum"
The Novaya Zemlya effect is a polar mirage caused by high refraction of sunlight between atmospheric thermoclines. The Novaya Zemlya effect will give the impression that the sun is rising earlier than it actually should (astronomically speaking) and depending on the meteorological situation the effect will present the sun as a line or a square (which is sometimes referred to as the "rectangular sun"), made up of flattened hourglass shapes. The mirage requires rays of sunlight to have an inversion layer for hundreds of kilometres (at least 400 km). The mirage depends on the inversion layer's temperature gradient. The sunlight must bend to the Earth's curvature at least 400km to allow a elevation rise of 5 degrees for sight of the sun disk. ...more on Wikipedia about "Novaya Zemlya effect"
The Schwabe-Wolf cycle is the most basic cycle present in the solar activity indices. ...more on Wikipedia about "Schwabe-Wolf cycle"
Solar cosmic rays are cosmic rays that originate from the Sun. Most are made of protons; these rays are relatively low in energy (10-100 keV). The average composition is similar to that of the Sun itself. The name solar cosmic ray itself is a misnomer, but it has stuck. High energy (Mev and above) cosmic rays come mainly from outside the solar system, while the particles in the solar case are energized near the Sun's surface by the action of magnetic fields. The misnomer arose because there is continuity in the energy spectra, i.e. the flux of particles as a function of their energy, because the low energy solar cosmic rays fade more or less smoothly into the galactic ones as one looks at higher and higher energies. Until the mid 1960's the energy distributions were generally averaged over long time intervals, which also obscured the difference. Later, it was found that the solar cosmic rays vary widely in their intensity and spectrum, increasing in strength after some solar events such as solar flares. Further, an increase in the intensity of solar cosmic rays is followed by a decrease in the galactic cosmic rays, called the Forbush decrease after their discoverer, the physicist Scott Forbush. These decreases are due to the solar wind with its entrained magnetic field sweeping some of the galactic cosmic rays outwards, away from the Sun and Earth. The overall or average rate of Forbush decreases tends to follow the 11 year sunspot cycle, but individual events are tied to events on the Sun, as explained above. ...more on Wikipedia about "Solar cosmic ray"
The Schwabe solar cycle is the eleven-year cycle of solar activity of the sun. ...more on Wikipedia about "Solar cycle"
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Solar maximum or solar max is the period of greatest solar activity in the solar cycle of the sun. During solar maximum, sunspots appear. The last solar maximum was in 2001. Solar maximum is contrasted with solar minimum. Solar maximum is the period when the suns magnetic field lines are the most distorted due to the magnetic field on the solar equator rotating at a slightly faster pace than at the solar poles. The sun takes about 11 years to go from one solar maximum to another and 22 years to complete a full cycle (where the magnetic charge on the poles is the same). ...more on Wikipedia about "Solar maximum"
Solar minimum is the period of least solar activity in the solar cycle of the sun. During this time sunspot and solar flare activity diminishes, and often does not occur for days at a time. The date of the minimum is described by a smoothed average over 12 months of sunspot activity, so identifying the date of the solar minimum usually can only happen 6 months after the minimum takes place. ...more on Wikipedia about "Solar minimum"
A Solar proton event occurs when high-energy protons, ejected from the sun's surface during a solar flare, get caught by the Earth's magnetic field and cause ionization in the ionosphere. The effect is similar to auroral events, the difference being that electrons and not protons are involved. The events typically occur where the Earth's magnetic field is lowest, at the north pole, south pole, and South Atlantic magnetic anomaly. The more severe proton events can cause widespread disruption to electrical grids and the propagation of electromagnetic signals. ...more on Wikipedia about "Solar proton event"
Solar variations are fluctuations in the amount of energy emitted by the Sun. Small variations have been measured from satellites during recent decades. Of interest to climate scientists is whether these variations have a significant effect on the temperature of the earth's atmosphere. ...more on Wikipedia about "Solar variation"
:Ion storm redirects here. For information about the games software company, see Ion Storm Inc. For the British comic, see Solar Wind (comic). For the ground weather phenomenon in RTS game Command & Conquer: Tiberian Sun, see Ion Storm (C&C). ...more on Wikipedia about "Solar wind"
The Space Environment Center (SEC) is a laboratory in the National Oceanic and Atmospheric Administration (NOAA)/ Office of Oceanic and Atmospheric Research (OAR). ...more on Wikipedia about "Space Environment Center"
A spicule is a dynamic jet of about 500km diameter on the Sun. It moves upwards at about 20 km/s from the photosphere They were discovered in 1877 by Father Angelo Secchi of the Vatican Observatory in Rome, ...more on Wikipedia about "Spicule (solar physics)"
Spörer's law predicts the variation of sunspot latitudes during a solar cycle. It was discovered by English astronomer Richard Christopher Carrington around 1861. Carrington's work was refined by German astronomer Gustav Spörer. ...more on Wikipedia about "Spörer's law"
Sunrise, also called sunup in some American English dialects, is the time at which the first part of the Sun appears above the horizon in the east. Sunrise should not be confused with dawn, which is the (variously defined) point at which the sky begins to lighten, some time before the sun itself appears, ending twilight. ...more on Wikipedia about "Sunrise"
Sunset, also called sundown in some American English dialects, is the time at which the Sun disappears below the horizon in the west. It should not be confused with dusk, which is the (variously defined) point at which darkness falls, some time after the Sun itself sets (which begins twilight). ...more on Wikipedia about "Sunset"
A sunspot is a region on the Sun's surface ( photosphere) that is marked by a lower temperature than its surroundings and intense magnetic activity. Although they are blindingly bright, at temperatures of roughly 5000 K, the contrast with the surrounding material at some 6000 K leaves them clearly visible as dark spots. If they were isolated from the surrounding photosphere they would be brighter than an electric arc. ...more on Wikipedia about "Sunspot" My way is shortopedia Solar_phenomena
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