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Blank Jeopardy
Blank Jeopardy

... What is the coolest star color ? ...
Chapter 30 Section 2 Handout
Chapter 30 Section 2 Handout

... What does increased temperature from contraction in the core cause the helium core to do? ...
neutron star - Adams State University
neutron star - Adams State University

... Most importantly, it runs MUCH faster than the proton-proton chain, allowing these larger stars to burn through their available fuel much more quickly. ...
15.3 The Lives of Stars
15.3 The Lives of Stars

Lifecycle of the stars.
Lifecycle of the stars.

...  Small proto star-a brown dwarf that was too small to generate enough heat to start fusion. ...
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E5 stellar processes and stellar evolution (HL only)
E5 stellar processes and stellar evolution (HL only)

... its life (it “burns” out quicker) A star with a mass 10x greater than the sun will have a life time a factor 10-3 (1/1000) less than the sun ...
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PPT

... its current level—too hot for life on Earth ...
supernova!
supernova!

life and death of a high mass star 2
life and death of a high mass star 2

...  AFTER THAT, THEY LOSE THEIR MASS AND HEAT AND BEGIN TO DIE.  THIS PROCESS TAKES BILLIONS AND BILLIONS OF YEARS. ...
ASTR100 Homework #5 Solutions Chapter 11 #29, 31 Due
ASTR100 Homework #5 Solutions Chapter 11 #29, 31 Due

... Hydrogen into Helium via the Proton-Proton Chain. During this process the Sun will lose mass and radiate it away as energy. When the sun was born the percentages were about 94% hydrogen and 4% Helium, but now we can expect the percent of Hydrogen still available for fusion is closer to 60%. Don’t wo ...
Midterm II Jeopardy
Midterm II Jeopardy

Life Cycle of Star EDpuzzle worksheet
Life Cycle of Star EDpuzzle worksheet

Earth Science
Earth Science

... maintains a stable size as long as it has an ample supply of hydrogen to fuse into _____. ...
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Physical Science 1 Quiz 10 1 ID # or name:

Stellar Properties and Stellar Evolution Study Guide Name Why
Stellar Properties and Stellar Evolution Study Guide Name Why

... 5. A shock wave may be the stimulus that causes a nebula to start condensing to form new ...
less than 1 million years
less than 1 million years

... 1. Today, scientists have _________ about how stars evolve, what makes them different from one another, and how they _____. 2. When __________ fuel is depleted , a star loses its _________ ___________ status. (2 words) 3. This (depletion of star’s hydrogen) can take less than 1 million years for the ...
3. Stellar Formation and Evolution
3. Stellar Formation and Evolution

... patches of nebulosity known as Herbig-Haro objects. • These jets, in combination with radiation from nearby massive stars, may help to drive away the surrounding cloud in which the star was formed. ...
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File - Morgan, Kristen

Section 3-3(rev04) 2
Section 3-3(rev04) 2

... • Small stars can live for about 200 billion years. • Medium stars live for about 10 billion years. • Large stars live for about 10 million years. ...
Astronomy Homework - Life
Astronomy Homework - Life

STARS
STARS

Chapter 30 Study Notes
Chapter 30 Study Notes

... A star with the sun’s mass would stay on the main sequence of the H-R diagram for about _____ 10 billion years. ...
Stellar Evolution
Stellar Evolution

... For stars bigger than the sun a slightly different path is taken.  They form about the same way, only hydrogen is used up faster, because they are so bright.  These massive stars become red giants many times, each time it uses up a new layer of gases by fusing different elements together. ...
ASTR/STELL=Star
ASTR/STELL=Star

... ...
< 1 ... 401 402 403 404 405 406 407 408 409 >

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.
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