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By Cassidy Clare Dakota Auringer Ismael Syed Austin Sandel

Solar Flares. By Cassidy Clare Dakota Auringer Ismael Syed Austin Sandel. What is a S olar Flare?.

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By Cassidy Clare Dakota Auringer Ismael Syed Austin Sandel

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  1. Solar Flares By Cassidy Clare Dakota Auringer Ismael Syed Austin Sandel

  2. What is a Solar Flare? A flare is defined as a sudden, rapid, and intense variation in brightness. A solar flare occurs when magnetic energy that has built up in the solar atmosphereis suddenly released. Radiation is emitted across virtually the entire electromagnetic spectrum, from radio waves at the long wavelength end, through optical emission to x-rays and gamma rays at the short wavelength end.

  3. What Causes a Solar Flare • The energy from the sun comes from nuclear fusion inside of the suns core. The fusion process creates energy by converting nuclear matter into energy. The most common fusion process is the proton-proton chain. This process begins when nuclei of the simplest form of hydrogen are forced together one at a time, then 2 particles form, then 3, and finally 4. The Flares are caused by the rearrangement of the sun’s magnetic field causing the magnetic loops to decrease or increase in pressure.

  4. Magnetic Fields • The magnetic field is rearranged by the lines that are squeezed past a critical point where it shapes into an 8 then into two 0’s, then the pressure increases to a point of explosion above sun spots. The magnetic loops are the magnetic field lines concentrated around the suns equator in the corona. The magnetic field becomes highly concentrated and increases in strength up to 3000 times normal strength. The energy is then released causing solar flares.

  5. Types of Solar Flares Impulsive Gradual • In the impulsive flare the energy spectra 0.5-9 MeVnucleon 4He and ~0.5-20 MeVnucleon O, Ne-Si and Fe ions are accelerated in this flare. Normally O, Ne- Si, and Fe ions are accelerated up to energies of ~16 MeVnucleon-1,Si and Fe have higher ionization states in the impulsive flare. Fe is likely to accelerate to at least 16 MeVnucleon and in one case it accelerated to 20-28 MeVnucleon. Electrons and ions are accelerated in and above the ionized coronal region of a magnetic loop. The ions and electrons are in the plasma state meaning that they are highly sensitive to magnetism so when they stream up a magnetic loop they produce the waves in the spectrum. Impulsive Flares are more compact, and in the lower corona. Flares produce hard X-ray burst that are controlled by the amount of time the flare develops. The hard X-rays are due to the bremsstrahlung emission of accelerated electrons. There are two types of solar flares • In a gradual solar flare Energetic particles are normally accelerated by a CME-driven shock (Coronal Mass Ejection). CME’s follow the solar cycle and emit the whole spectrum due to their high temperatures (1 million Kelvin). A CME requires a filament of plasma to form in an area of closed magnetic fields and it then ejected. The sun’s magnetic field reverses every 22 years and solar flares occur every 11 years.

  6. Three Stages of a Solar Flare The first stage is the precursor stage this is where the release of magnetic energy is triggered. Soft X-rays are detected during this stage. The third stage is the Decay stage, this is where the soft X-rays decay. The second stage was the impulsive stage, protons and electrons are accelerated to energies exceeding 1 MeVnucleon. During this stage radio, hard x-rays, gamma rays are emitted.

  7. Sun Spots Effect on Solar Flares Sun spots occur because in some places the magnetic field cools and slows down the radiation forming a Sun Spot. Sunspots usually form in pairs of the reverse polarity. Sun spots are essential in the flare process because when sun spots of the reverse polarity collide the particles are accelerated and explode resulting in a solar Flare.

  8. How Solar Flares Affect Us Solar Flares emit harmful rays throughout the spectrum. Most of these rays are blocked by our magnetosphere but the radio waves break through. These rays can disrupt our communications and cause global blackouts.

  9. Bibliography • Answers.com. "Bremsstrahlung." Answers.com. Answers Corp 2010, 2010. Web. 22 Apr. 2010. <http://www.answers.com/topic/bremsstrahlung>. Dunbar, Brian, ed. "Sun." Nasa World Book. Nasa, 29 Nov. 2007. Web. 22 Apr. 2010. <http://www.nasa.gov/worldbook/sun_worldbook.html>. Infield, Margery. "The Carrington Event: Flare or CME? A Report." Climate.arm. Putney High School, 24 July 2009. Web. 22 Apr. 2010. <http://climate.arm.ac.uk/Carrington_Flare_Report.pdf>. Makhmutov, V S, et al. "Evaluation of the Energy Spectrum of Solar Protons According to the Balloon Measurement Data and Monte Carlo Simulation." Metapress.com. Bulletin of the Russian Acad. of Sciences, 2007. Web. 22 Apr. 2010. <http://resources.metapress.com/pdf-preview.axd?>. Manuel, O, and StigFriberg. "Composition Of The Solar Interior:Information From Isotope Ratios." Arvix.org. Local and Global Helioseismology, 2002. Web. 22 Apr. 2010. <http://arxiv.org/ftp/astro-ph/papers/0410/0410717.pdf>. Mazur, J E, G M Mason, and B Klecker. "Heavy Ion Acceleration beyond 10 MeV per Nucleon in Impulsive Flares." The Astrophysical Journal Letters. The American Astronomical Society, 1995. Web. 22 Apr. 2010. <http://iopscience.iop.org/1538-4357/448/1/L53/fulltext?ejredirect=migration>. Miller, James A. "Particle Acceleration in Impulsive Solar Flares." Owlnet.edu. The U of Alabama, 2006. Web. 22 Apr. 2010. <http://www.owlnet.rice.edu/~astr554/miller98.pdf>. Tarko, Vlad. "Solar Mayhem." Softpedia. Softpedia, 2001. Web. 22 Apr. 2010. <http://news.softpedia.com/news/Solar-Mayhem-16550.shtml>. TL, Garrard, and Stone EC. "Composition of energetic particles from solar flares." PubMed.gov. National Center for Biotechnology Information, 28 Oct. 2009. Web. 22 Apr. 2010. <http://www.ncbi.nlm.nih.gov/About/disclaimer.html>. Watanabe, Tetsuya. "Plasma Motions in the Flare 1982 June 6(X12)." Metapress.com. National Astronomical Observatory, Nov. 1989. Web. 22 Apr. 2010. <http://resources.metapress.com/ pdf-preview.axd?code=x83753778n0l7571&size=largest>.

  10. Vocabulary • Solar Atmosphere- The outermost gaseous layers of a planet, natural satellite, or star. • Corona-type of plasma “atmosphere" of the sun or other celestial body, extending millions of kilometers into space, most easily seen during a total solar eclipse. • MeVnucleon-1-1,000,000 electron volts. • Bremsstrahlung- emission of accelerated electrons, when electromagnetic radiation is produced by a change in the velocity of an electrically charged subatomic particle such as an electron, as when it collides with another object.

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