Nebula Life Cycle

911 Words2 Pages
bulb-icon

Recommended: What is the theorized life cycle of a star

The Life Cycle of Our Star

Nebula
What is a nebula? A nebula is the birth of a new star. Cloud of gas and dust in space.
Mostly made up of Hydrogen and Helium. The cause of a nebula has come from a huge collapse of gas, also known as Interstellar Medium. A nebula’s lifecycle is less than 1 million years old before they burst into a supernova.

Because of gravity Nebula forms a star

Protostar
Giant clouds form around a star that creates pressure--nebula. Differences in temperature create a gravitational collapse which creates protostar

A protostar is formed when gravity causes the dust and gas of a nebula to clump together in a process called accretion

As gravity continues to pull ever more matter inward towards the core, its temperature, …show more content…

This is the beginning of a new star. It is a giant cloud of dust and gas that is mostly made up of hydrogen and helium. The creation of a Nebula is caused by a collapse of gas, also known as Interstellar Medium. A Nebula can live up to a million years old before they turn into a …show more content…

That’s older than my grandma,” said Ralphie.

“Excellent observation Ralphie,” said Ms. Frizzle. 3 page
PROTOSTAR

“Aside from Ralphie’s sidecomment, we are now moving on to the second stage of a star, the Protostar,” said Ms. Frizzle.

This is the protostar. A process called accretion occurs when a gravitational collapse causes dust and gas of a nebula to clump and then a protostar is formed. Say a star has an equivalent weight to our sun, that means that that star was a protostar for more than 10 million years. During the process of a protostar, gravity pulls more matter inward towards the core, which cause its pressure, density, and temperature to rise. Nuclear Fusion then begins once the high temperatures in the core of a protostar is reached, from then, a star is born.

4 page
STABLE STATE

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

Show More
Related

  • Hertzsprung-russell Diagram

    510 Words  | 2 Pages

    Another group of stars, which are rather small, is found near the bottom left of the H-R Diagram.

    Read More

  • Lagoon Nebula Essay

    886 Words  | 2 Pages

    The Lagoon Nebula featured as Nasa’s astronomy picture of the day was photographed by John Nemcik using various filters to capture the light emitted by the Hydrogen, Sulfur, and Oxygen. While photographed showing beautiful vibrant, eye-catching colors, the Nebula would appear naturally appear gray to human eye due to poor color sensitivity existing at low-light levels (spacetelescope.org). The Lagoon Nebula is home to the formation of new stars, as well as several other interesting phenomena such as Bok globules, and the hourglass nebula. It is these regions of the nebula that make it a continuous area of interest and study for astronomers.

    Read More

  • My Favorite APOD Nebulae Images

    906 Words  | 2 Pages

    There are numerous mysteries contained within the Cosmos that have yet to fully be analyzed and appreciated. The unique events that transpire within the Universe everyday are unbelievably remarkable and captivating. Hidden within the immense ocean of stars we see every night lays an even more incredible spectacle in the form of Nebulae. The paragraphs that ensue will delve into the creation of Nebulae, and the many intriguing aspects of the most visually appealing amongst these particular phenomena.

    Read More

  • Black Holes

    1549 Words  | 4 Pages

    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.

    Read More

  • The Importance Of God In 'The Star'

    977 Words  | 2 Pages

    Nebula away so that it can avoid certain things. In the short story, “The Star,” the priest stated,

    Read More

  • Solar Nebula Cause Planet Formation

    532 Words  | 2 Pages

    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.

    Read More

  • History Of The Orion Nebula

    1022 Words  | 3 Pages

    In 1610, two years after the invention of the telescope, the Orion Nebula, which looks like a star to the naked eye, was discovered by a scholar named Nicolas-Claude Fabri Peiresc. In 1656 Christan Huygens, the Dutch scholar and scientist, using his own greatly improved instruments, was the first to describe the inner region of the nebula, and to determine that its inner star is not single but a compact quadruple system.

    Read More

  • Stars Lifecycle

    891 Words  | 2 Pages

    In this state the outward force of the fusion balances inward force of gravity thus balancing out the star for about 90% of its lifetime. The life of a star depends on how massive the star is. Larger stars have hotter centers and will burn through the hydrogen core faster. The largest know stars last only a couple of millions of years. Smaller stars, like our own Sun, have cooler cores and burn the fuel at a slower rate and will last for billions of years. The smallest stars or dwarf stars burn so slowly that they could potentially last 100 billion years in their adult stage. For comparisons sake think of large stars as an F-150 and a smaller star as a Prius, although the F-150 has a larger tank it will burn through the fuel faster than the Prius with the smaller tank will. After a star’s fuel core is exhausted it will experience a

    Read More

  • Stellar Evolution

    2295 Words  | 5 Pages

    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...

    Read More

  • Cosmic Life and Death of a Star

    1612 Words  | 4 Pages

    If the nebula is dense enough, certain regions of it will begin to gravitationally collapse after being disturbed. As it collapses the particles begin to move more rapidly, which on a molecular level is actually heat, and photons are emitted that drive off the remaining dust and gas. Once the cloud has collapsed enough to cause the core temperature to reach ten-million degrees Celsius, nuclear fusion starts in its core and this ball of gas and dust is now a star. It begins its life as a main sequence star and little does it know its entire life has already been predetermined.

    Read More

  • Solar System Formation

    1864 Words  | 4 Pages

    Our solar system, as we see it today, originally formed from the collapse of a very cold and low-density cloud of gas. The mass of this cloud was composed of 98% hydrogen and helium, 1.4% hydrogen compounds, .4% rock, and .2% metal. The nebula was thought to be a few light years across and was roughly spherical in shape. The cloud was in a state of balance, it was neither contracting or expanding, until a cataclysmic event, most likely a supernova, created a shock wave through the nebula, resulting in an area of higher mass. Once this area became more massive than the rest of the nebula it begin to collapse with the area of hig...

    Read More

  • Essay On Galaxies

    668 Words  | 2 Pages

    A galaxy is a system of millions or billions, maybe even trillions of stars that are composed with gas and dust, which is held together by gravitational attraction. Galaxies have been categorized throughout history according to their shape, size and brightness.

    Read More

  • Stellar Evolution

    1854 Words  | 4 Pages

    It is not understood well, but in some supernovae the gravity is so intense within the red supergiant that the electrons are forced into the atomic nuclei where they combine with protons to form neutrons. The electromagnetic forces keeping apart the seperate nuclei are gone and the entire core becomes a dense ball of neutrons or an atomic nucleus about the size of Manhatten called a Neutron Star. If the mass is great enough though, when the star turns into a red supergiant it will collapse under its on gravity into a radius smaller than the Schwarzchild Radius and turn into a Black Hole.

    Read More

  • Galaxies in Our Universe

    757 Words  | 2 Pages

    The Universe is a collection of millions of galaxies and extends beyond human imagination. After the big bang, the universe was found to be composed of radiation and subatomic particles. Information following big bang is arguable on how galaxies formed, that is whether small particles merged to form clusters and eventually galaxies or whether the universe systematized as immense clumps of matter that later fragmented into galaxies (Nasa World book, 2013). A galaxy is a massive area of empty space full of dust, gases (mainly 75% Hydrogen and 25%Helium), atoms, about 100-200 billion stars, interstellar clouds and planets, attracted to the center by gravitational force of attraction. Based on recent research, 170 billion galaxies have been estimated to exist, with only tens of thousands been discovered (Deutsch, 2011).

    Read More

  • Solar System Essay

    932 Words  | 2 Pages

    Solar System:The solar system has a collection of nebulas along with multiple planets,moons, stars,comets, meteoroids and asteroids. There are eight main planets in our solar system with a moon or many moons orbiting it. There are other planets in the solar system that are smaller and they’re called dwarf planets, they also have moons in their orbit. They’re stars being formed by nebulas everyday in this solar system along with comets, meteoroids and asteroids charging around, blasting into planets at high speeds.

    Read More

More about Nebula Life Cycle

Open Document