Coronal Mass Ejection Essay

The foremost differentiation between solar flares and coronal mass ejections (CMEs) is the scale on which they transpire. Solar flares are rather little and local, occuring in the low solar atmosphere, near sunspots, where magnetic field lines are concentrated. CMEs on the other hand are huge. They can even be bigger than the sun itself!

Sunspots are generated by strong and dense magnetic fields, and these magnetic fields are caused by flowing plasma that gets tangled and moves through the photosphere. [1] However, it is not actually sunspot activity that effects the Earth’s power grid and satellite communications, [2] but rather the solar flares and coronal mass ejections (CMEs) that can be caused by sunspots that cause problems. [3]

Solar wind is a continuous stream of charged particles – protons and electrons – with some atomic nuclei. It is produced by the hydrogen fusion reactions at the Sun’s core with

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At the center of the sun, the temperature is 27 million degrees Fahrenheit (15 million degrees Celsius). As the temperature on its surface rises and falls, the sun boils and bubbles. Particles escape from the star from the sunspot regions on the surface, hurtling particles of plasma, known as solar wind, into space. It takes these winds around 40 hours to reach Earth. When they do, they can cause the dramatic displays known as the aurora borealis. [Infographics: How the Northern Lights Work & Anatomy of Sun Storms & Solar

As the plasma rotates with the sun’s convection zone, consolidation of the magnetic flux tubes occurs such that their field strength is stronger. As the outer layers of the sun rotate faster near the equator than they do near the poles (“differential rotation”), as much as 1.3 times more than the rotation at 30° latitude (see figure 4, part 2, not to scale), the magnetic field becomes distorted forming lines of concentrated magnetic intensity (see figure 4, part 3). This activity causes enough turbulence to ‘buckle’ the magnetic field such that it bends out forming a loop above the photosphere, and as these regions rise through the solar atmosphere, the convective flow of energy is partially blocked, cooling the region and thus reducing its brightness, causing the darkness associated with sunspots (see figure 4, part

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The outer solar atmosphere, the corona, is created by magnetic fields. When the fields close, the confined solar atmosphere can suddenly violently release bubbles of gas and magnetic fields. A coronal mass ejection can contain a billion tons of matter that can move at millions of miles per hour (Solar). Solar energetic particles are released by shocks at the front of Coronal mass ejections and solar flares. When a coronal mass ejection flows through the solar wind, high velocity solar energetic particles are produced. They are charged so they follow the magnetic lines between the Sun and Earth (Solar).

Solar flares are high energy explosions that radiate through space. They are sometimes called CME’s, which stands for coronal mass ejection. Solar flares are measured by the maximum flux of their X-rays. The scale consists of grade A, B, C, M, X flares. A is the weakest level and X is the strongest. This scale is similar to the Richter scale for measuring earthquakes. The most recent solar flare that was considered X-rated occurred in 2011, according to (Science Daily.)

Solar flares release 10 million times more energy than a volcano and during times, there are over 20 solar flares a day. They are about as hot as the Sun’s core. A Solar flare/Solar storm is a brief outburst of intense high-energy radiation from the sun’s surface associated with sunspots and causing electromagnetic disturbances on the Earth, as with radio frequency communications and power line transmissions. Solar flares are caused by the sudden release of magnetic energy. The largest ones can release as much as a billion one - megaton nuclear bombs. Solar flares/Solar storms occur anywhere on the sun, the most violent events on the surface of the sun. We are well protected from the effects of the solar flares.

The first is the precursor stage where magnetic energy is released. In the second stage, known as the impulsive stage, protons and electrons energies are accelerated. During this stage radio waves, hard x-rays, and gamma rays are emitted. In the third stage, called the decay stage, is the buildup of soft x-rays and then the decay of the soft x-rays. The duration of the precursor, impulsive, and decay stages can take anywhere from a few seconds up to one hour. Solar flares form in a layer of the sun called the corona, the outermost layer, where the gases can reach a few million degrees Kelvin(“Solar Flares”). Solar flares normally erupt from sunspots. Typically, these sunspots are temporarily cooler, darker, and the local magnetic field is relatively

The solar wind containing these hot gases races toward the edges of the solar system, and smash in to the magnetosphere. The magnetosphere protects the earth by deflecting most of the solar wind around the planet. Trillions of these charged particles mange to get through and project from the North and South poles. Energy released in this fashion excites atoms of nitrogen and oxygen, which in turn emit pulses of colored light. These formations are called an aurora. The aurora borealis, which are visible in Alaska, are a result of this sort of space storm.

In short terms, explosions on the sun releases charged particles called plasma into the solar system (Goodrich). Some of these particles hit Earth, which then reacts with our planet’s magnetic field and atmosphere. Then, the atoms and molecules in the atmosphere light up due to the electrons moving up to higher-energy orbits and back down to the lower-energy orbit (Imster).

     Have you ever heard of a solar flare? A solar flare exists after a sunspot has existed for a long time and the magnetic lines of force usually become jumbled. As a result of this jumbling, magnetic energy is stored in the Corona (region of atmosphere above the chromosphere). The energy may be released in a spectacular discharge, which is a solar flare. A solar flare can be as wide as 367,000 miles and as high 500,000 miles out into space. A solar flare is nothing more than helium erupting from the sun like a volcano.

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