Plasmasphere Essay

Today I am here to inform you about the High Frequency Active Auroral Research Program (HAARP) and its intentions.

Training an artificial Neural Network involves choosing and allowing models for models which there are several associated algorithms.

Instead we use the original predictors to predict the response. The original dataset was split into a training set that consists of 75% of the total observations and a test set that consists of 25% of the total observations. Observations were chosen randomly. Supervised learning methods was conducted on the training set to obtain a model, then the model was used on the test set to assess the prediction performance. The values for “K” in KNN were tuned via cross-validation. Due to the volume of the data, the “cost” parameter in the SVM was chosen somewhat ad hoc and the “mtry” parameter in the random forest was chosen as default. The error rates are as

In the year 2065, climate change on Earth has spiraled out of control and nations are now fighting for new real estate in space to begin colonization. Mars had been a likely candidate for many years now and was becoming a massive fighting ground for numerous nations. However, it’s arid landscape and small size made it a questionable choice to some. More adventurous and risk-taking politicians urged their researchers to aim for Pluto or planets outside of our solar system. Feeling modern technology was not yet ready for such long distance travel, the United States has chosen to look toward the asteroid belt. As they are setting off, researchers will monitor sunspots to help forecast the behavior of the sun and predict coronal mass ejections (CMEs). Solar-powered sails will make use of solar wind for the early journey after leaving Earth. Radioisotope thermoelectric

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]

In 1945, Joseph Henry and Stephen Alexander, professors from Princeton University, discovered that sunspots emitted less radiation than surrounding areas of the sun. This is because the Sun’s outer shell, the photosphere, behaves as plasma, which is a very good conductor of electricity, and interacts with the magnetic fields of sunspots. The plasma slows down and cools to 1000 K less than the surrounding photosphere which makes it look darker than the surrounding areas. These areas were concentrated magnetic fields appear, are usually part of a loop, as sunspots generally present in pairs which line up parallel to the equator, showing a magnetic polarity. The sunspots in each hemisphere have the opposite polarity to the other. Over the 11 year cycle, the whole polarity reverses as the new set of sunspots form away from the Sun’s equator. Therefore, a complete 22 year cycle returns the polarity to its original

“All of them? I don’t know, but I would think so. What concerns me is the geomagnetic storms we’ve been having. The result of the solar wind gusts. We've got data from magnetometers—the elevated Kp Index. Jolts going off the charts. There's just no doubt any longer about a relationship between what we see happening on Earth and the solar wind. BUT then—you see—we also got solar wind coming from where our sun is most definitely NOT! You're the one who should be able to spot the source, Arnold. You're the whiz kid working with radiation emissions. Tell me what's going on here!”

Since the electrons are stripped from the atoms in a plasma, all that remains is the positively charged nucleus, which can be acted on by magnetic fields. In magnetic confinement reactors, so-called magnetic bottles are created with magnetic fields that confine the plasma. In experiments, however, plasmas can only be contained for a few seconds before their oscilations cause them to come into contact with the walls of the reactor. The biggest problem in controlling plasmas with magnetic confinement is their chaotic behaivior. With continuing research, longer containment times are being recorded.

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.

Possibly the most dramatic event that occurs within our solar system is the solar flare. Scientists have spent much time studying this solar phenomenon attempting to learn how to predict them. This in turn has caused a significant increase in understanding the anatomy of solar flares to include the phases of flares and what they emit. Bringing things closer to Earth, the emissions of solar flares can have a significant impact in today’s technological world. By far, the largest impact of solar flares to our technology is radio blackouts. The emissions of solar flares cause scintillation to occur in the ionosphere effectively blocking long distance transmissions. Solar flares are excessively bright and powerful and so deserve our attention not only from a scientific standpoint, but a societal standpoint as we rely more and more on our technology.

The sun is a vital piece to our planet – it provides us with energy, warmth, food and auroras! The sun is an average star in size and is currently in the main sequence stage of its life. There are many parts to our sun, which begins at the core. The core is where the sun’s energy derives from, fusing hydrogen to helium. The outer regions of the core is where the energy travels outward through radiation, then convection, and finally out through the solar atmosphere. The solar atmosphere consists of three classified parts, a photosphere, chromosphere, and corona. The drama that unfolds on the chromosphere and corona play a major role in auroras. Particularly, a massive solar flare classified as a coronal mass ejection. A coronal mass ejection is a type of solar flare that “occur when magnetic fields pointing in opposite directions release energy by interacting with and destroying each other… their magnetic

In the heliosphere, the large-scale structure of the solar wind is dominated by two types of interplanetary disturbances: transient and corotating disturbances. Corotating disturbances, associated with spatial variability and solar rotation, occur in response to the interaction of fast and slow solar winds. Transient disturbances, due to episodic solar eruptions, expand outward from the Sun into interplanetary space (Gosling, 1996).

In the next paragraphs, this thesis paper discussed various factors of 3 mentioned MDSS like main motivation for the implementation of new MDSS, different data mining (DM) algorithms used, techniques used to improve the

First, MARS-K found that at certain levels of the normalized ratio of plasma pressure to magnetic field strength ( (-- removed HTML --) β (-- removed HTML --) N (-- removed HTML --) (-- removed HTML --) ), ITER could be stabilized at low rotation, but that alpha particles did not strongly affect stability. (-- removed HTML --) (-- removed HTML --) 13 (-- removed HTML --) (-- removed HTML --) It was also noted that the perturbative formulation was more stable than the self-consistent approach, (-- removed HTML --) (-- removed HTML --) 13 (-- removed HTML --) (-- removed HTML --) although in that case very large rational surface contributions were not removed in the MARS-K calculations of perturbed potential energy as was done in the benchmarking exercise in Ref. (-- removed HTML --) 2 (-- removed HTML --) . Subsequently, both MISK and HAGIS found that the kinetic effects of thermal particles alone may not be sufficient for ITER stability. (-- removed HTML --) (-- removed HTML --) 7,15 (-- removed HTML --) (-- removed HTML --) The HAGIS study also found stronger stabilizing effects from thermal particles at lower (precession) rotation. (-- removed HTML --) (-- removed HTML --) 15 (-- removed HTML --) (-- removed HTML --) Both HAGIS and MARS-K included energetic ions from neutral beam injection or ion cyclotron resonance heating in addition to alpha particles, emphasizing the importance of finite orbit

(-- removed HTML --) (-- removed HTML --) (-- removed HTML --) 5 (-- removed HTML --) (-- removed HTML --) studied the nonlinear propagation of EA waves in an unmagnetized plasma with hot Maxwellian electrons and fluid cold and beam electrons and ions and compared their results with the spiky structures of the broadband electrostatic noise due to nonlinear EA waves observed in the aurora1 region of the Earth's magnetosphere. Schriver and Ashour-Abdalla (-- removed HTML --) (-- removed HTML --) 6 (-- removed HTML --) (-- removed HTML --) showed that the electron acoustic instability and electron ion instability can be combined to form a broadbanded wave spectrum that rapidly destroys the electron beam. Pottelett (-- removed HTML --) et al. (-- removed HTML --) (-- removed HTML --) (-- removed HTML --) 7 (-- removed HTML --) (-- removed HTML --) observed large amplitude solitary waves at edges of the AKR source region, characterized by the presence of two electron populations with a dominant hot component and a minority cold component. Dubouloz (-- removed HTML --) et al. (-- removed HTML --) (-- removed HTML --) (-- removed HTML --) 8 (-- removed HTML --) (-- removed HTML --) presented that the great number of bursts of broadband electrostatic noise recorded during crossings of the dayside auroral zone by the Viking satellite enables their statistical study. The characteristics of the electrostatic turbulence produced by a gas of electron