The sun is a massive object comprised of intensely hot, ionized gases called plasma. Hot objects, like the sun, have a tendency to expand, however the sun’s size and density give it a very strong gravitational pull which balances out the would-be expansion; the combination of these forces can cause the sun's surface to change in dramatic and sometimes violent ways which I will now explain.
The sun’s enormous magnetic field drives its gases to flow in currents which carry electrons, too superheated to hold on to their atoms, throughout the photosphere, corona and solar interior. These currents cause lines in the magnetic field to twist preventing hotter gases from the sun's core from rising to the surface; which in turn creates darker, cooler areas than the rest of the sun's surface, known as Sunspots. The hot gases trapped below these sunspots exert pressure on the obstructions winding the magnetic field lines into tighter and tighter coils. Sometimes, the magnetic field lines will uncoil without incident; the sunspot fades and the hotter gases rise to the surface as normal, but ot...
In “The Warmth of Other Suns” by Isabel Wilkerson, the three main characters that the story follows face a great deal of inequality and racial prejudice in both the Jim Crow south that they left and the north that they fled to. Through their stories, as well as the excerpts from Wilkerson that serve to dispel some of the common myths and to explain some of the inequalities that others faced, one is able to make many connections between the problems that Ida Mae, George Starling, and Richard Foster, among many others, faced in their time and the obstacles to equality that our society still to this day struggles to overcome. A large reason as to why these obstacles still exist is that many have preconceived ideas about African Americans and African American Communities. However, numerous obstacles still survive to this day as a result of certain racist ideas.
The very symbol of life – the elemental force of the Sun – is rendered
Stars are born and reborn from an explosion of a previous star. The particles and helium are brought together the same way the last star was born. Throughout the life of a star, it manages to avoid collapsing. The gravitational pull from the core of the star has to equal the gravitational pull of the gasses, which form a type of orbit. When this equality is broken, the star can go into several different stages. Some stars that are at least thirty times larger than our sun can form black holes and other kinds of stars.
Solar nebula is a rotating flattened disk of gas and dust in which the outer part of the disk became planets while the center bulge part became the sun. Its inner part is hot, which is heated by a young sun and due to the impact of the gas falling on the disk during its collapse. However, the outer part is cold and far below the freezing point of water. In the solar nebula, the process of condensation occurs after enough cooling of solar nebula and results in the formation into a disk. Condensation is a process of cooling the gas and its molecules stick together to form liquid or solid particles. Therefore, condensation is the change from gas to liquid. In this process, the gas must cool below a critical temperature. Accretion is the process in which the tiny condensed particles from the nebula begin to stick together to form bigger pieces. Solar nebular theory explains the formation of the solar system. In the solar nebula, tiny grains stuck together and created bigger grains that grew into clumps, possibly held together by electrical forces similar to those that make lint stick to your clothes. Subsequent collisions, if not too violent, allowed these smaller particles to grow into objects ranging in size from millimeters to kilometers. These larger objects are called planetesimals. As planetesimals moved within the disk and collide with one another, planets formed. Because astronomers have no direct way to observe how the Solar System formed, they rely heavily on computer simulations to study that remote time. Computer simulations try to solve Newton’s laws of motion for the complex mix of dust and gas that we believe made up the solar nebula. Merging of the planetesimals increased their mass and thus their gravitational attraction. That, in turn, helped them grow even more massive by drawing planetesimals into clumps or rings around the sun. The process of planets building undergoes consumption of most of the planetesimals. Some survived planetesimals form small moons, asteroids, and comets. The leftover Rocky planetesimals that remained between Jupiter and Mars were stirred by Jupiter’s gravitational force. Therefore, these Rocky planetesimals are unable to assemble into a planet. These planetesimals are known as asteroids. Formation of solar system is explained by solar nebular theory. A rotating flat disk with center bulge is the solar nebula. The outer part of the disk becomes planets and the center bulge becomes the sun.
absorb the energy from the sun, but it does absorb some of the heat energy
The sun became the king of the universe and he was very bright so he could be seen from far and wide. The stars feared him and so again began to behave in an appropriate fashion. He also was very hot and warmed the once cold universe so that life would be possible.
Long ago, the goddess of life and death, Erius, watched over the humans and gave them light. She shined her light for centuries, but the humans were not grateful. She grew tired, and knew the humans were taking her for granted. So one day, she created the Sun, which shone light upon the world. The humans liked the Sun, but they wondered why the Sun was moving. They watched the sun set over the horizon, and as the sun set, it grew dark.
At last, we have reached the most relaxed area of a star. This area is called the Stable State. Our star, the sun is currently at its stable state and will be for another 3-5 billion years. The stable state is the longest period of the life of a star. When a star is at it’s stable state, it is constantly burning its fuel out. Once all the fuel burns out of the star, it means that the star has reached the red giant
A star begins as nothing more than a very light distribution of interstellar gases and dust particles over a distance of a few dozen lightyears. Although there is extremely low pressure existing between stars, this distribution of gas exists instead of a true vacuum. If the density of gas becomes larger than .1 particles per cubic centimeter, the interstellar gas grows unstable. Any small deviation in density, and because it is impossible to have a perfectly even distribution in these clouds this is something that will naturally occur, and the area begins to contract. This happens because between about .1 and 1 particles per cubic centimeter, pressure gains an inverse relationship with density. This causes internal pressure to decrease with increasing density, which because of the higher external pressure, causes the density to continue to increase. This causes the gas in the interstellar medium to spontaneously collect into denser clouds. The denser clouds will contain molecular hydrogen (H2) and interstellar dust particles including carbon compounds, silicates, and small impure ice crystals. Also, within these clouds, there are 2 types of zones. There are H I zones, which contain neutral hydrogen and often have a temperature around 100 Kelvin (K), and there are H II zones, which contain ionized hydrogen and have a temperature around 10,000 K. The ionized hydrogen absorbs ultraviolet light from it’s environment and retransmits it as visible and infrared light. These clouds, visible to the human eye, have been named nebulae. The density in these nebulae is usually about 10 atoms per cubic centimeter. In brighter nebulae, there exists densities of up to several thousand atoms per cubic centimete...
Smil, Vaclav. "The Long Slow Rise of Solar and Wind." Scientific American 310.1 (2014): 52. MasterFILE Complete. Web. 30 Mar. 2014.
Smil, Vaclav. "The Long Slow Rise Of Solar And Wind." Scientific American 310.1 (2014): 52-57. Academic Search Complete. Web. 16 May 2014.
Light is a very important factor in the rate of photosynthesis, in my project I am going to test that plants do need light in order to photosynthesise. It will be very interesting to see how light will influence the rate of photosynthesis in plants and what will happen if they do not get the required light in order to produce starch .
Looking up at the sky on a vibrant night, the vision is naturally lit one with millions of vivacious, glistening stars. The tenacity of this essay is to explore the lifecycle of a star, thence, signify its manifestation in the universe. A fundamental part of our universe is stars. Hence, these miniature luminous forms are essentially very immense in magnitude and it is merely due to their substantial distance from Earth that they appear so trivial. Scientifically, a star is a ball of hydrogen and helium with sufficient mass that it can endure nuclear mixture at its core. A huge, shining ball of plasma, whose lustre is an outcome of thermonuclear fusion are all properties of a star. In addition, they are held together by gravity. By far the star nearest to earth is probably known by all humans as the Sun. A bright star on Orion’s top-left section named as Betelgeuse is so massive that if it was placed where the sun is, it would swallow up Earth, Mars and Jupiter!2 Furthermore, a teaspoon full of Neutron star would weigh about “112 million tonnes” . Particular stars are known to be 600,000 times brighter than the sun ; thus a stars’ lifespan varies between 1 billion to 10 billion years 2.This essay will discuss a star’s journey from as little as a protostar (foetus) till the final stage as a black hole or a white dwarf (old age- death).
Our sun is the central pivot point to which or entire planet and solar system is built around. With out it all life on our planet would cease to exist. Within this paper we will explore how our Sun and solar system formed and came to resemble what we see today.