Shop Windows to the Universe

Warnings: The True Story of How Science Tamed the Weather by Mike Smith tells the story of our storm warning system. See our online store book collection.
Sequence of the main phases of formation of a star: very slowly rotating cloud of gas, gravitational collapse, star formation by slow contraction and accretion with generation of intense stellar wind, collimation of the stellar wind into bipolar flow.
Click on image for full size
Image courtesy of the University of Oregon, Department of Physics, the Electronic Universe Project

The life cycle of the stars

A gas cloud, if massive enough, starts to shrink under its own gravitational force. This shrinkage causes the density and temperature to increase. When the density and temperature are high enough, nuclear fusion reactions among ions become more frequent, and Hydrogen is converted into Helium. Eventually, the outward pressure generated by the fusion reactions balances the gravitational force, the shrinkage stops, and the gas cloud becomes a star. This is the present state of our Sun.

After billions of years, most of the Hydrogen fuel has been "burned", and there's no longer enough pressure to balance gravity and the star begins to shrink again. This causes the core temperature to rise to the point where the fusion of Helium can occur. A new equilibrium is reached where the star is now much larger, because the outer layers have expanded and cooled. In these conditions the star is called a red giant (referring to the color of its outer atmosphere). Our Sun is supposed to reach this state in about five billion years, and its radius will reach the orbit of Mars. A red giant will keep on burning until it its nuclear fuel is exhausted, then a new contraction will take place. If there is enough mass left in the star this contraction will heat the core enough to trigger fusion reactions of heavier elements at higher and higher temperatures until the fusion reactions produce Iron.

Beyond Iron the nuclear fusion process cannot release anymore energy, and a red giant start reaches the end of its life. The fusion reactions that powered the star have reduced its mass to the point that gravity is not strong enough to hold the outermost layers; this gaseous envelope is ejected to form a planetary nebula. The core of the star collapses to the point that repulsion between electrons balances the gravitational force and a white dwarf is formed. This is an extremely dense star the size of a planet. Finally, when the white dwarf has radiated all its energy away, it stops shining and becomes a "black dwarf", a dead star. This is expected to be the final state of our Sun.

For stars with higher masses than the Sun (up to about 40 times greater), gravitational collapse will be much faster, lasting a period of time estimated in the order of few seconds. An enormous shock wave is produced that pushes the outer layers of the star away and heats them. The star becomes extremely bright and large, comparable to the brightness of a galaxy. This is a supernova. In the final gravitational collapse of the supernova core, gravity overwhelms electron pressure and electrons and protons are brought close enough together to be converted into neutrons. The star collapses down to a radius of few tens of kilometers: this is what is called a "neutron star".
For stars larger than 40 solar masses the collapse following the supernova explosion is so fast that even the pressure from the neutrons formed in the core is not enough to stop the contraction. The density increases to the point that the velocity needed to escape from the gravitational field is larger than the velocity of light. Light itself is then trapped inside and the object has become invisible: this is a "black hole".


Last modified January 24, 2005 by Randy Russell.

Shop Windows to the Universe Science Store!

Cool It! is the new card game from the Union of Concerned Scientists that teaches kids about the choices we have when it comes to climate change—and how policy and technology decisions made today will matter. Cool It! is available in our online store.

Windows to the Universe Community

News

Opportunities

You might also be interested in:

Fusion Reactions

Nuclear fusion is a process where two or more nuclei combine to form an element with a higher atomic number (more protons in the nucleus). Fusion is the reverse process of nuclear fission. Fusion of light...more

The Hydrogen Fusion Process

The basic Hydrogen fusion cycle involves four Hydrogen nuclei (protons) and two electrons and yields a Helium nucleus, two neutrinos and six photons. This process occurs in three steps: the first one is...more

The Supernova

A Supernova is a very massive star that explodes at the end of its life cycle. The supernova is the furnace where the heavy elements (heavier than iron) are formed by neutron capture. ...more

Fusion Inside the Stars

Fusion in the core of the stars is achieved when the density and temperature arising from the gravitational pressure are high enough. There are different fusion cycles that occur in different phases of...more

Diagnostics for the Solar Interior

The Sun, as well as other stars, releases energy in the form of radiation and particles. The processes that produce this energy are taking place in the interior of the Sun, where direct observations are...more

The Neutron Capture Process

Neutron capture can occur when a neutron approaches a nucleus close enough for nuclear forces to be effective. The neutron is captured and forms a heavier isotope of the capturing element. When the new...more

IMF

IMF stands for Interplanetary Magnetic Field. It is another name for the Sun's magnetic field. The Sun's magnetic field is enormous and is carried by the solar wind. The solar wind and magnetic field are...more

The Cherenkov Effect

The theory of relativity states that no particle can travel at the speed of light in a vacuum. However, light travels at lower speeds in dense media, like water. A particle traveling in water must have...more

Windows to the Universe, a project of the National Earth Science Teachers Association, is sponsored in part by the National Science Foundation and NASA, our Founding Partners (the American Geophysical Union and American Geosciences Institute) as well as through Institutional, Contributing, and Affiliate Partners, individual memberships and generous donors. Thank you for your support! NASA AGU AGI NSF