Understand The Effect Of Solar Plasma On Earth's Magnetosphere

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!

However, this has not happened and it’s starting to make secular scientist themselves admit that our sun is special and unique in design, because it does not emit these monster super flares like the ones produced by Proxima Centauri. The question is, could our sun send out such a flare powerful enough to even melt the ice on Jupiter’s moon’s, destroy earth’s ozone layer and even obliterate all our satellites? Well the answer is yes. Scientist have studied other sun like stars in our galaxy and discovered that they produce these super flares about once a century. But, they have no explanations as to why our sun does not produce such solar

Despite the amounts of incoming radiation, very little actually reaches the Earth’s surface. One layer of protection the Earth provides is in the form of a magnetic field that deflects charged particles from reaching the Earth’s surface. This magnetic field is generated by a combination of the liquids within the Earth’s core and the interplanetary magnetic field generated by the Sun. This field reaches out thousands of miles from Earth, so when solar wind travels through space and encounters Earth’s

The sun is an enormous bright yellow circle object visible in the sky daytime. Astronomers believe that it is one of the many stars which the earth orbits in our galaxy. The sun is thought to be the midpoint of the solar system based on the assertion that it is the only star in the solar system that is the source of energy for all the other planets. According to geometry facts, the sun acts as the hub of the solar system since all the other components of the solar system go around it on all sides (Haugen, 2002). The sun is vital to the solar system since it used as the center of research, study, and forecasting not only in space travel but also on earth.

The number of sunspots is controlled by the amount of distortion of the Sun's magnetic field. The magnetic field becomes distorted because the Sun's equator and core rotate more quickly than its other parts. As a result, sunspot activity varies over an average 11-year cycle. Over approximately 11 years, the Sun goes from a solar minimum (fewer spots) to a solar maximum (more spots) and back to a minimum

We now that the Earth has layers in the atmosphere to protect us from the Suns light and heat. It may not be technically a “layer” of the atmosphere, but the magnetosphere also plays a role in our protection. The Sun produces something called solar wind which is basically “the flow of” “charged particles from the Sun”, writes authors Timothy Slater and Roger Freedman. (Slater) Solar wind can travel at supersonic speeds and we probably wouldn’t be here have this discussion. Fortunately for us, the magnetosphere and Earth’s magnetic field can deflect these winds.

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]

To start on how the sun produces heat, the sun consists mostly of hydrogen, especially at its core. The core is only one fourth of its size but this is where all of the reactions happen and where all the heat of the sun is actually produced. In the core of a star, it is so pressurized and so hot that nuclear fusion occurs every 9.2×1037 times a second. The hydrogen molecules are forced together to make helium molecules. When this reaction occurs, it releases 0.7% of the mass in the form of energy. The conversion rate of mass into energy is 4.26 million metric tons a second. This type of reaction is what occurred in a hydrogen bomb. So just like the bomb, that explosion is what happens in the sun but not exactly. Because the sun is so dense with hydrogen and helium, the explosion is contained. The outer mantle of the sun, which makes up three fourths of the sun and consists of all of the energy that is created by the core, contains this explosion. Plus the inward gravitation pull on itself also keeps the explosions contained.

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.

The Sun, a star, is hot ball of glowing gases at the center of our solar system (nasa.gov/sun). It’s heat and energy sustain the life we have on Earth. Without it, we would not be able to survive. The Sun warms the entire planet, reaching the Earth’s surface, oceans, and atmosphere. The heat and energy from the Sun is what essentially drives the weather and climates (windows2universe.org). The orientation of the Earth to the Sun is what creates the Earth’s seasons. Depending on what hemisphere you reside in, the season and weather patterns vary. If the hemisphere you live in is pointed towards the Sun, it is summer. If it is directed away from the Sun, it is winter. This is due to the tilt of Earth’s axis.

Cosmic-rays are modulated as they traverse into the heliosphere. Measurements have shown that cosmic-ray intensity varies on different time scales. On a longer time scale, the cosmic-ray intensity variations in anti-phase with solar activity having ≈ 11-year cyclicity is well known and studied extensively (e.g., see Venkatesan and Badruddin, 1990; Storini et al., 1995; Usoskin et al., 1998; Mavromichalaki et al., 1998; Kane, 2003; Sabbah and Rybansky, 2006; Ma et al., 2009; Chaudhary et al., 2011; Kudela, 2012). In addition, the ≈ 22-year modulation cycle in cosmic-ray flux due to solar magnetic field polarity reversals is observed and modeled (e.g., Jokipii and Thomas, 1981; Potgieter and Moraal, 1985; Webber and Lockwood, 1988; Potgieter, 1995; Cliver and Ling, 2001; Laurenza et al., 2012). However, in order to understand these phenomena, it is important to understand how cosmic-ray transport and propagation vary with the solar activity and solar magnetic polarity (Heber, 2013).

Observations made in the space environment consistently show plasma particles with velocity distributions that have non-thermal tails, and frequently with anisotropies. (-- removed HTML --) (-- removed HTML --) 1–6 (-- removed HTML --) (-- removed HTML --) Characteristically, observed solar wind electrons are modeled by a combination of the Maxwellian core population (with energy in the range of tens of eV) and a tenuous but energetic (-- removed HTML --) halo (-- removed HTML --) distribution that contains a power-law velocity distribution in the suprathermal range (∼10 (-- removed HTML --) 2 (-- removed HTML --) –10 (-- removed HTML --) 3 (-- removed HTML --) eV). For energy range even higher than that of the halo population, that

elerated a wave of energetic particles… this wash of quick-moving particles would have been dangerous to anyone outside Earth’s protective magnetic

In the present paper, we considered the dynamical evolution of protons and electrons in response to parallel electron firehose instability excitation. Even though the free energy source for the instability is provided by excessive electron temperature anisotropy, because of the fact that unstable modes operate in low frequency range, the protons respond to the instability excitation as well. Kinetic instabilities driven by electron and proton temperature anisotropies, of which the present electron firehose instability is a part, are known to play significant roles in regulating the temperature anisotropy upper bound as the solar wind expands out into the interplanetary space from its solar source. In the present paper, we employed

What starts a geomagnetic storm is an event called solar flares or an extremely large cloud of solar material called a coronal mass ejection (CME). When these charged particles get near the earth’s magnetic field, due to the increased magnitudes in solar wind, the magnetic field accelerates towards the geomagnetic poles, therefore causing the phenomena called aurora borealis or northern lights. The other effect of a magnetic storm causes the geomagnetic field to become highly unstable due to the change and distribution of density, as a result, the ions in the earth’s ionosphere become agitated, resulting in disorder; a massive disruption in our technical systems [Wisconsin State Journal P.A2].