Solar Activity

The Sun is the closest star to Earth. The Sun is a huge mass of hot, glowing gas. The Sun is a huge mass of hot, glowing gas. The strong gravitational pull of the Sun holds Earth and the other planets in the solar system in orbit. The Sun's light and heat influence all of the objects in thesolar system and allow life to exist on Earth.

The Sun is an average star its size, age, and temperature fall in about the middle of the ranges of these properties for all stars.

Astronomers believe that the Sun is about 4.6 billion years old and will keep shining for about another 7 billion years.

For humans, the Sun is beautiful and useful, but also powerful and dangerous.

As Earth turns, the Sun rises over the eastern horizon in the morning, passes across the sky during the day, and sets in the west in the evening. This movement of the Sun across the sky marks the passage of time during the day (see Sundial). The Sun's movement can produce spectacular sunrises and sunsets under the right atmospheric conditions. At night, reflected sunlight makes the Moon and planets bright in the night sky.

The Sun provides Earth with vast amounts of energy every day. The oceans and seas store this energy and help keep the temperature of Earth at a level that allows a wide variety of life to exist. Plants use the Sun's energy to make food, and plants provide food for other organisms. The Sun's energy also creates wind in Earth���s atmosphere. This wind can be harnessed and used to produce power.

While it lights our day and provides energy for life, sunlight can also be harmful to people. Human skin is sensitive to ultraviolet light emitted from the Sun. Earth's atmosphere blocks much of the harmful light, but sunlight is still strong enough to burn skin under some conditions (see Burn). Sunburn is one of the most important risk factors in the development of skin cancers, which can be fatal. Sunlight is also very harmful to human eyes. A person should never look directly at the Sun, even with sunglasses or during an eclipse. The Sun influences Earth with more than just light. Particles flowing from the Sun can disrupt Earth's magnetic field, and these disruptions can interfere with electronic communications.

Physical Characteristics

The Sun is large and massive compared to the other objects in the solar system. The Sun's radius (the distance from its center to its surface) is 695,508 km (432,169 mi), 109 times as large as Earth's radius. If the Sun were hollow, a million Earths could fit inside it. The Sun has a mass of 1.989 X 1027 metric tons. This number is very large. Written out, it would be the digits 1989 followed by 24 zeroes.

The Sun is 333,000 times as massive as Earth is. Despite its large mass, the Sun has a lower density, or mass per unit volume, than Earth. The Sun's average density is only 1.409 g/cu cm (1.188 oz/cu in), which is a quarter of the average density of Earth.

The Sun produces an enormous amount of light. It generates 3.83 X 1026 watts of power in the form of light. In comparison, an incandescent lamp emits 60 to 100 watts of power. The temperature of the outer, visible part of the Sun is 5500��C (9900��F).

From Earth the Sun looks small, because it is far away. Its average distance from Earth is 150 million km (93 million mi). Light from the Sun takes about eight minutes to reach Earth. This light is still strong enough when it reaches Earth, however, to damage human eyes when viewed directly. The Sun is much closer to Earth than any other star is. The Sun's nearest stellar neighbor, Proxima Centauri (part of the triple star Alpha Centauri), is 4.3 light-years from our solar system, meaning light from Proxima Centauri takes 4.3 years to reach the Sun. The Sun is so much closer to Earth than all other stars are that the intense light of the Sun keeps us from seeing any other stars during the day.

Importance to Earth

Earth would not have any life on it without the Sun�s energy, which reaches Earth in the form of heat and light. This energy warms our days and illuminates our world. Green plants absorb sunlight and convert it to food, which these plants then use to live and grow. In this process, the plants give off the oxygen that animals breathe. Animals eat these plants for nourishment. All plant and animal life relies on the Sun�s presence.

The Sun also provides - directly or indirectly - much of the energy on Earth that people use for fuel. Devices called solar cells turn sunlight into electricity. Sunlight can heat a gas or liquid, which can then be circulated through a building to heat the building. The energy stored in fossil fuels originally came from the Sun. Ancient plants used sunlight as fuel to grow. Animals consumed these plants. The plants and animals stored the energy of sunlight in the organic material that composed them. When the ancient plants and animals died and decayed, this organic material was buried and gradually turned into the petroleum, coal, and natural gas people use today. The Sun�s energy produces the winds and the movements of water that people harness to produce electricity. The Sun heats Earth�s oceans and land, which in turn heat the air and make it circulate in the atmosphere as wind. The Sun fuels Earth�s water cycle, evaporating water from the oceans, seas, and lakes. This water returns to the ground in the form of precipitation, flowing back to the oceans through the ground and in rivers. The energy of water�s motion in rivers can be harnessed with dams.

Role in the Solar System

The Sun�s gravitational pull holds the solar system together. The planets, asteroids, comets, and dust that make up our solar system are strongly attracted to the Sun�s huge mass. This gravitational attraction keeps these bodies in orbit around the Sun. The Sun also influences the solar system with its diffuse outer atmosphere, which expands outward in all directions. This expanding atmosphere fills the solar system with a constant flow of tiny, fast, electrically charged particles. This flow is called the solar wind. The region through which the solar wind blows is called the heliosphere. The heliosphere extends outward from the Sun to about 150 times the distance between Earth and the Sun. Interstellar winds may give the heliosphere an egg shape. The solar wind spreads out as it leaves the Sun. The point at which the solar wind is so diffuse that it stops having an effect on its surroundings is called the heliopause. The heliopause marks the outer edge of the solar system.

Within the heliosphere, the Sun provides most of the heat and light that are present, and the particles in the solar wind interact with the planets and satellites in the solar system. The solar wind causes auroras�displays of colored light�in the atmosphere of Earth�s polar regions. The solar wind also carries remnants of the Sun�s magnetic field, which affect the magnetic fields of the planets and larger satellites. The solar wind pushes the planets� magnetic fields away from the Sun, turning them into elongated, windsock shapes. For more information, see the Solar Wind section of this article.

The Sun as a Star

The Sun is extremely important to Earth and to our solar system, but on the scale of the galaxy and the universe, the Sun is just an average star. It is one of hundreds of billions of stars in our galaxy, the Milky Way, which is just one of more than 100 billion galaxies in the observable universe.

The Sun�s Place in the Milky Way

The Milky Way Galaxy contains about 100 billion stars. All of these stars, and the gas and dust between them, are rotating about a galactic center. Stars that are farther away from the center move at slower speeds and take longer to go around it.

The Sun is located in the outer part of the galaxy, at a distance of 2.6 � 1017 km (1.6 � 1017 mi) from the center. The Sun, which is moving around the center at a velocity of 220 km/s (140 mi/s), takes 250 million years to complete one trip around the center of the galaxy. The Sun has circled the galaxy more than 18 times during its 4.6-billion-year lifetime.

Comparisons with Other Stars

A star is a ball of hot, glowing gas that is hot enough and dense enough to trigger nuclear reactions, which fuel the star. In comparing the mass, light production, and size of the Sun to other stars, astronomers find that the Sun is a perfectly ordinary star. It behaves exactly the way they would expect a star of its size to behave. The main difference between the Sun and other stars is that the Sun is much closer to Earth.

Most stars have masses similar to that of the Sun. The majority of stars� masses are between 0.3 to 3.0 times the mass of the Sun. Theoretical calculations indicate that in order to trigger nuclear reactions and to create its own energy - that is, to become a star - a body must have a mass greater than 7 percent of the mass of the Sun. Astronomical bodies that are less massive than this become planets or objects called brown dwarfs. The largest accurately determined stellar mass is of a star called V382 Cygni and is 27 times that of the Sun.

The range of brightness among stars is much larger than the range of mass. Astronomers measure the brightness of a star by measuring its magnitude and luminosity. Magnitude allows astronomers to rank how bright, comparatively, different stars appear to humans. Because of the way our eyes detect light, a lamp ten times more luminous than a second lamp will appear less than ten times brighter to human eyes. This discrepancy affects the magnitude scale, as does the tradition of giving brighter stars lower magnitudes. The lower a star�s magnitude, the brighter it is. Stars with negative magnitudes are the brightest of all.

Magnitude is given in terms of absolute and apparent values. Absolute magnitude is a measurement of how bright a star would appear if viewed from a set distance away. By convention, this distance is 10 parsecs, or 32.6 light-years. Apparent magnitude measures how bright a star appears from Earth. The Sun�s absolute magnitude is 4.8. The brightest known stars have absolute magnitudes of about -9 (lower magnitudes mean brighter stars), and the dimmest known stars have absolute magnitudes of about 20. The apparent magnitude of the Sun is -26.72. The apparent magnitude of the brightest star in Earth�s night sky, Sirius, is -1.46. The dimmest stars that can be seen from Earth with unaided eyes have apparent magnitudes of about 6.

Astronomers also measure a star�s brightness in terms of its luminosity. A star�s absolute luminosity or intrinsic brightness is the total amount of energy radiated by the star per second. Luminosity is often expressed in units of watts. The Sun�s absolute luminosity is 3.86 � 1026 watts. The absolute luminosity of stars ranges from one thousandth of the luminosity of the Sun to 10 million times that of the Sun.

Another way of measuring brightness is to measure the amount of light that reaches an observer. This measurement is called apparent brightness or apparent luminosity. Apparent luminosity depends on the absolute luminosity of a star and the distance from the star to the observer. Apparent luminosity becomes smaller as distance from the star to the observer becomes larger. From Earth, the apparent luminosity of the Sun is 10 billion times greater than the apparent luminosity of the next brightest star, Sirius, because the Sun is so much closer to Earth.

The radius of the Sun is about average among stars. The radii of most stars fall between 0.2 and 15 times the Sun�s radius, although some giant stars are hundreds of times larger than the Sun. Larger stars usually have larger absolute luminosities. We receive much more energy from the Sun than from other stars, because the Sun is so nearby. The Sun�s proximity also allows scientists to study its face in detail. A modest telescope can resolve solar structures that are 700 km (400 mi) across�about the distance from Boston, Massachusetts, to Washington, D.C. That level of detail is comparable to seeing the features on a coin from 1 km (0.6 mi) away. Other stars are so distant that the details on their surfaces remain unresolved with even the largest telescopes.

Composition of the Sun

The Sun is a second-generation star, meaning that some of its material came from former stars. Some stars in our galaxy are nearly as old as the expanding universe, which scientists believe originated in the big bang explosion about 15 billion years ago - Big Bang theory. In contrast, the Sun is only 4.6 billion years old.

The first stars were composed only of the hydrogen and helium produced in the early universe. These stars are called first-generation stars. Although hydrogen is also the main ingredient of the Sun, it contains heavier elements, such as carbon, nitrogen, and oxygen, as well. These elements formed inside first-generation stars that lived and died before the Sun was born. When these massive, short-lived stars used up their internal fuel, they exploded and ejected the heavier elements into interstellar space. The Sun formed from this material, making it a second-generation star.

The Sun�s Remote Past and Distant Future

The Sun and planets in our solar system formed when a rotating cloud of dust and gas in space collapsed, or condensed, due to the gravitational attraction between the particles in the cloud. A nearby supernova explosion may have triggered the collapse, or a random fluctuation in the density of the cloud may have started the process. The Sun formed at the center of the spinning cloud, while the debris that condensed into planets formed a flattened disk revolving around the Sun. When the Sun reached its present size about 4.6 billion years ago, it was hot enough inside to ignite the nuclear reactions that make it glow.

The Sun cannot shine forever, because it will eventually use up its present fuel. The nuclear fusion reactions that make the Sun glow (for more information, see the section entitled The Sun�s Energy in this article) depend on the element hydrogen, but the hydrogen in the Sun�s core will eventually run out. Nuclear reactions have converted about 37 percent of the hydrogen originally in the Sun�s core into helium. Astronomers estimate that the Sun�s core will run out of hydrogen in about 7 billion years.

The Sun will grow steadily brighter as time goes on and more helium accumulates in its core. Even as the supply of hydrogen dwindles, the Sun�s core must keep producing enough pressure to keep the Sun from collapsing in on itself. The only way it can do this is to increase its temperature. The increase in temperature raises the rate at which nuclear reactions occur and makes the Sun brighter. In 3 billion years, the Sun will be hot enough to boil Earth�s oceans away. Four billion years thereafter, the Sun will have used up all its hydrogen and will balloon into a giant star that engulfs the planet Mercury. At this point in its life, the Sun will be a red giant star. The Sun will then be 2,000 times brighter than it is now, and hot enough to melt Earth�s rocks. At this time the outer solar system will get warmer and more habitable. The icy moons of the giant planets may warm enough to be covered by water instead of ice.

When the giant Sun uses up its fuel, it will no longer be able to support the weight of its inner layers, and they will begin to collapse toward the core, eventually producing a small, dense, cool star called a white dwarf. The Sun will then have about the same radius as Earth has, but it will be much denser and more massive than Earth. The Sun will become a white dwarf star about 8 billion years from now. After it becomes a white dwarf, it will cool slowly for billions of years, eventually becoming so cool that it will no longer emit light.


Sunspot snapshot reveals mystery filaments Nivember 2002 - New Scientist

Simultaneous solar flares intrigue scientists November 2002 - MSNBC
Scientists say they have made the unprecedented discovery of solar flares erupting almost simultaneously on opposite sides of the sun.

Prophecy - May 2002

Harmless halo around the sun transformed many South Floridians into instant astronomers. May 17, 2002

Hopi Prophecy:

Now we enter the time of testing that only the Great Creator can confirm. The alignment of the planets, we were so kindly informed of by the star watchers has been awaited by the Hopi. As the time nears, the predicted behavior of the people accurately describes the behavior of people in the 1990's. When the end is near, we will see a halo of mist around the heavenly bodies. Four times it will appear around the sun as a warning that we must reform.

Harmonics - May 2002 - Cosmi Universe

Giant Star Plays Bass Notes

About 30 years ago, astronomers realised that the Sun resonates like a giant musical instrument with well-defined periods (frequencies). It forms a sort of large, spherical organ pipe. The energy that excites these sound waves comes from the turbulent region just below the Sun's visible surface.

Sunspots and the Rise and Fall of Civilizations

There appears to be a correlation between the rise and fall of civilizations with the rise and fall of radiation from the sun.

The graph shows a long-term envelope of sunspot activity derived from the center graph of Carbon 14.

More carbon 14 is absorbed in the growth rings of tress udring the sunspot minima.



Solar flares are intense, temporary releases of energy. They are seen at ground-based observatories as bright areas on the Sun in optical wavelengths and as bursts of noise at radio wavelengths; they can last from minutes to hours. Flares are our solar system's largest explosive events, equivalent to approximately 40 billion Hiroshima-size atomic bombs. The primary energy source for flares appears to be the tearing and reconnection of strong magnetic fields. They radiate throughout the electromagnetic spectrum, from gamma rays to x-rays, through visible light out to kilometer-long radio waves. -


The outer solar atmosphere, the corona, is structured by strong magnetic fields. Where these fields are closed, often above sunspot groups, the confined solar atmosphere can suddenly and violently release bubbles or tongues of gas and magnetic fields called coronal mass ejections. A large CME can contain 10.0E16 grams (a billion tons) of matter that can be accelerated to several million miles per hour in a spectacular explosion. Solar material streaks out through the interplanetary medium, impacting any planets or spacecraft in its path. CMEs are sometimes associated with flares but usually occur independently.

After only 8 minutes ....

X-ray and ultraviolet light given off by solar flares arrives at the Earth. These types of light are responsible for the formation of the ionosphere under normal circumstances. But now the intensities of these types of light have increased dramatically. All over the dayside hemisphere, the ionosphere is increased in density particularly at low altitudes in the D and E regions. This is called a sudden ionospheric disturbance (SID) and lasts usually for between 10 and 60 minutes. Short wave radio signals experience increased absorption when ionization is produced at these low altitudes. Loss of signal at this time is called a short wave fadeout.

Enhanced levels of solar radiation can also cause heating and expansion of the neutral atmosphere and increase the amount of atmospheric drag that a satellite experiences in an unpredictable manner.


Minutes to Hours Later .....

Solar protons are accelerated to very high velocities in the explosive release of energy associated with a solar flare. These particles first make their way out of the corona. Then they cannot take a straight line path to the Earth but must travel along the Sun's extended magnetic field lines (called the interplanetary magnetic field or IMF). These field lines have a structure resembling the spiral traced out by a spinning lawn sprinkler, which is referred to as a Parker spiral.


Hours to Days Later... Disturbances in the solar wind arrive at the Earth within hours to days after a violent event on the Sun. The largest space weather disturbances at Earth are produced by coronal mass ejections and fast solar wind streams emanating from coronal holes. Coronal holes are the main source of recurrent solar activity.

Coronal mass ejections (CMEs) violently expell billions of tons of solar material into interplanetary space. They normally drive shocks ahead of them as they plow into the slower-moving solar wind streams. Vast quantities of high speed particles are born in these shock structures and speed ahead of the coronal mass ejection to impact the Earth before the CME itself makes an appearance. It is now believed that a large fraction of the solar energetic particles arriving at Earth were produced in these shocks rather than at flare sites on the Sun.

CMEs are difficult to detect and, in fact, were not observed until coronographs were build and flow in space. Many of the CMEs that are blown toward the Earth never actually directly hit us. They just pass us by.


After 27 days ....

Coronal holes are eaily seen as dark regions in xray images of the sun. The unique feature of coronal holes compared to surrounding regions is that magnetic field lines within the coronal hole extend outward into the interplanetary medium. This allows solar wind plasma to freely flow out into interplanetary space. In surrounding regions, the magnetic field lines resemble arches with both feet connected to the solar disk. The outward flow of plasma in this region is impeded by these closed field lines.

Polar coronal holes almost always exist. However, the fast streams that are associated with the polar coronal holes never reach the Earth. During some intervals, coronal holes are formed at lower solar latitudes. In this location, the coronal holes spray the Earth with high speed plasma streams, like a powerful garden sprinkler, and are responsible for generating space weather storms that recur in intervals of 27 days as the coronal hole rotates back over the limb of the Sun. These recurrent storms tend to be weaker than storms produced by coronal mass ejections and to be most frequent during the years just following solar maximum.