The Life Cycle of a star
... White dwarfs • Gravity causes the last of the star’s matter to collapse inward and compact, this is the white dwarf stage. • At this stage the star’s matter is extremely dense. • White dwarfs shine with a white hot light. • The star has now reached the black dwarf phase in which it will forever rem ...
... White dwarfs • Gravity causes the last of the star’s matter to collapse inward and compact, this is the white dwarf stage. • At this stage the star’s matter is extremely dense. • White dwarfs shine with a white hot light. • The star has now reached the black dwarf phase in which it will forever rem ...
Deep Space and Solar System
... line toward its normal wavelength If the source is moving toward the observer, there is a blue shift toward shorter wavelengths • Why do we think the universe is expanding? Light reaching us from distant galaxies has a lower frequency then expected Therefore, the universe is expanding ...
... line toward its normal wavelength If the source is moving toward the observer, there is a blue shift toward shorter wavelengths • Why do we think the universe is expanding? Light reaching us from distant galaxies has a lower frequency then expected Therefore, the universe is expanding ...
Study Guide_galaxies, Tools, and Stars Test
... and send it back to Earth where the data can be interrupted by scientists. 14. ________ _________ are sent on missions outside of Earth’s orbit into deep space where it could be dangerous for astronauts to travel. 15. Diagram the Milky Way and our place in it. 16. What tool do astronomers use to ide ...
... and send it back to Earth where the data can be interrupted by scientists. 14. ________ _________ are sent on missions outside of Earth’s orbit into deep space where it could be dangerous for astronauts to travel. 15. Diagram the Milky Way and our place in it. 16. What tool do astronomers use to ide ...
Other Objects in Space
... Any fragments from space that land on Earth Page 455 Figure 18 Important clues from space Made of metal and rock Hundreds fall to Earth each year! ...
... Any fragments from space that land on Earth Page 455 Figure 18 Important clues from space Made of metal and rock Hundreds fall to Earth each year! ...
Stellar Evolution and the Herzsprung-Russell Diagram
... • The ashes of each reaction are the fuel for the next inner shell. • Each reaction is less efficient than the previous: they buy very little time • Iron accumulates because energy cannot be gained by making heavier elements (it has the most stable nucleus) • The iron core is supported by degeneracy ...
... • The ashes of each reaction are the fuel for the next inner shell. • Each reaction is less efficient than the previous: they buy very little time • Iron accumulates because energy cannot be gained by making heavier elements (it has the most stable nucleus) • The iron core is supported by degeneracy ...
Electromagnetic Radiation from the Sun
... atomic number elements. This is the case because of the Big Bang, when temperatures were so high that only energy could exist. As the universe expanded, it cooled and some of the energy converted into matter in the form of electrons, protons and neutrons. As the universe continued to expand and cool ...
... atomic number elements. This is the case because of the Big Bang, when temperatures were so high that only energy could exist. As the universe expanded, it cooled and some of the energy converted into matter in the form of electrons, protons and neutrons. As the universe continued to expand and cool ...
Stellar Evolution Test Answers
... 21. The most common type star in the universe is the a) brown dwarf b) white dwarf c) yellow dwarf d) red dwarf 22. A star hotter than the sun would tend to be more _________in color. a) yellow b) red c) blue 23. That which drives the life history of a star is its mass. a) true b) false 24. More mas ...
... 21. The most common type star in the universe is the a) brown dwarf b) white dwarf c) yellow dwarf d) red dwarf 22. A star hotter than the sun would tend to be more _________in color. a) yellow b) red c) blue 23. That which drives the life history of a star is its mass. a) true b) false 24. More mas ...
Astronomy 360 Physics/Geology 360
... nearest star clusters to Earth and is the cluster most obvious to the naked eye in the night sky. Pleiades has several meanings in different cultures and traditions. The cluster is dominated by hot blue and extremely luminous stars that have formed within the last 100 million years. Dust that forms ...
... nearest star clusters to Earth and is the cluster most obvious to the naked eye in the night sky. Pleiades has several meanings in different cultures and traditions. The cluster is dominated by hot blue and extremely luminous stars that have formed within the last 100 million years. Dust that forms ...
Astronomy Universe2
... wavelengths stretch into longer wavelengths Blue shift = source is moving closer so wavelengths squeeze into shorter ...
... wavelengths stretch into longer wavelengths Blue shift = source is moving closer so wavelengths squeeze into shorter ...
1 Star Formation and Main Sequence Evolution Condensation
... Protostars and Protoplanety disks are seen inside interstellar clouds! ...
... Protostars and Protoplanety disks are seen inside interstellar clouds! ...
Stellar Evolution
... around a sun-like star that is dying. -White dwarfs – As the planetary nebula disperses, gravity causes the remaining matter to collapse inward…what is left is hot & dense…it is called a white dwarf. -When a white dwarf no longer gives off light, it forms a ...
... around a sun-like star that is dying. -White dwarfs – As the planetary nebula disperses, gravity causes the remaining matter to collapse inward…what is left is hot & dense…it is called a white dwarf. -When a white dwarf no longer gives off light, it forms a ...
Document
... 1. It has been determined that all stars have the same general composition (90% H, 9% He, trace amounts of heavy elements). If this is the case, explain why stars of different temperatures show different spectral line patterns. ...
... 1. It has been determined that all stars have the same general composition (90% H, 9% He, trace amounts of heavy elements). If this is the case, explain why stars of different temperatures show different spectral line patterns. ...
S1E4 Extreme Stars
... mass, and eventually becomes hot enough (100 million Kelvin) for helium to begin to fuse into carbon Carbon ash is deposited in core and eventually a helium-burning shell develops. This shell is itself surrounded by a shell of hydrogen undergoing nuclear fusion. For a star with M< 1 Msun, the carbon ...
... mass, and eventually becomes hot enough (100 million Kelvin) for helium to begin to fuse into carbon Carbon ash is deposited in core and eventually a helium-burning shell develops. This shell is itself surrounded by a shell of hydrogen undergoing nuclear fusion. For a star with M< 1 Msun, the carbon ...
File - Physical Science
... centers of atoms) combine together to make a larger one (which is a different element). The result of this process is the release of a lot of energy. Stars are powered by nuclear fusion in their cores, mostly converting hydrogen into helium. The production of new elements via nuclear reactions is ca ...
... centers of atoms) combine together to make a larger one (which is a different element). The result of this process is the release of a lot of energy. Stars are powered by nuclear fusion in their cores, mostly converting hydrogen into helium. The production of new elements via nuclear reactions is ca ...
Forging the elements
... At the end of the planetary nebula stage the star is left with an extremely hot, dense core (a million times denser than the earth). ...
... At the end of the planetary nebula stage the star is left with an extremely hot, dense core (a million times denser than the earth). ...
White Dwarfs
... on the main sequence on the HertzsprungRussell diagram? A: Stars that have reached the main sequence have ceased nuclear "burning" and are simply cooling down by emitting ...
... on the main sequence on the HertzsprungRussell diagram? A: Stars that have reached the main sequence have ceased nuclear "burning" and are simply cooling down by emitting ...
Slide 1
... emit high energy photons that are absorbed by the gas. The heated gases produce an emission spectrum and the particular wavelength of the red light of the nebula is 656nm. The exact wavelength of Hydrogen. ...
... emit high energy photons that are absorbed by the gas. The heated gases produce an emission spectrum and the particular wavelength of the red light of the nebula is 656nm. The exact wavelength of Hydrogen. ...
Stellar evolution
Stellar evolution is the process by which a star changes during its lifetime. Depending on the mass of the star, this lifetime ranges from a few million years for the most massive to trillions of years for the least massive, which is considerably longer than the age of the universe. The table shows the lifetimes of stars as a function of their masses. All stars are born from collapsing clouds of gas and dust, often called nebulae or molecular clouds. Over the course of millions of years, these protostars settle down into a state of equilibrium, becoming what is known as a main-sequence star.Nuclear fusion powers a star for most of its life. Initially the energy is generated by the fusion of hydrogen atoms at the core of the main-sequence star. Later, as the preponderance of atoms at the core becomes helium, stars like the Sun begin to fuse hydrogen along a spherical shell surrounding the core. This process causes the star to gradually grow in size, passing through the subgiant stage until it reaches the red giant phase. Stars with at least half the mass of the Sun can also begin to generate energy through the fusion of helium at their core, whereas more-massive stars can fuse heavier elements along a series of concentric shells. Once a star like the Sun has exhausted its nuclear fuel, its core collapses into a dense white dwarf and the outer layers are expelled as a planetary nebula. Stars with around ten or more times the mass of the Sun can explode in a supernova as their inert iron cores collapse into an extremely dense neutron star or black hole. Although the universe is not old enough for any of the smallest red dwarfs to have reached the end of their lives, stellar models suggest they will slowly become brighter and hotter before running out of hydrogen fuel and becoming low-mass white dwarfs.Stellar evolution is not studied by observing the life of a single star, as most stellar changes occur too slowly to be detected, even over many centuries. Instead, astrophysicists come to understand how stars evolve by observing numerous stars at various points in their lifetime, and by simulating stellar structure using computer models.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.