01 - Awtrey Middle School
... 1. What keeps a star from breaking apart? a. gravity b. energy c. mass d. density 2. During which stage of the life cycle is a star a ball of gas and dust? a. first stage b. second stage c. third stage d. last stage 3. What gas does hydrogen change into as a star becomes hotter? a. uranium b. helium ...
... 1. What keeps a star from breaking apart? a. gravity b. energy c. mass d. density 2. During which stage of the life cycle is a star a ball of gas and dust? a. first stage b. second stage c. third stage d. last stage 3. What gas does hydrogen change into as a star becomes hotter? a. uranium b. helium ...
Stellar Evolution (Formation)
... Example: in the dense core of a typical giant molecular cloud: T~ 10 K; ~ 3 x 10-17 kg/m3; ~ 2 for pure H2 gas (X= 1, Y = Z = 0) Thus MJ ~ 2 Msun The characteristic mass of these dense cores is ~ 10 Msun so they are unstable to gravitational collapse - consistent with them being sites of star fo ...
... Example: in the dense core of a typical giant molecular cloud: T~ 10 K; ~ 3 x 10-17 kg/m3; ~ 2 for pure H2 gas (X= 1, Y = Z = 0) Thus MJ ~ 2 Msun The characteristic mass of these dense cores is ~ 10 Msun so they are unstable to gravitational collapse - consistent with them being sites of star fo ...
Scientists classify stars by
... 2. If the remaining mass of the star is about 1.4 times that of our Sun, it will collapse further to become a neutron star. 3. If the remaining mass of the star is more than about three times that of the Sun, it will collapse and what is left behind is an intense region of gravity called a black hol ...
... 2. If the remaining mass of the star is about 1.4 times that of our Sun, it will collapse further to become a neutron star. 3. If the remaining mass of the star is more than about three times that of the Sun, it will collapse and what is left behind is an intense region of gravity called a black hol ...
Report Sheet
... 17. What is the minimum temperature a Protostar must achieve to begin hydrogen fusion? ____________F 18. Define hydrogen fusion- ____________________________________________________________________ 19. If our Sun is blowing up like a bomb, why does it not just blast itself into space? _____________ ...
... 17. What is the minimum temperature a Protostar must achieve to begin hydrogen fusion? ____________F 18. Define hydrogen fusion- ____________________________________________________________________ 19. If our Sun is blowing up like a bomb, why does it not just blast itself into space? _____________ ...
Stars
... it becomes a black hole and nothing can escape from it, not even light. • Black holes are not like giant vacuums. It has an event horizon, a region inside of which nothing can escape. Anything that crosses the event horizon will be sucked into it. ...
... it becomes a black hole and nothing can escape from it, not even light. • Black holes are not like giant vacuums. It has an event horizon, a region inside of which nothing can escape. Anything that crosses the event horizon will be sucked into it. ...
Slide 1
... HOW DO STARS DIE ? •Most stars take millions of years to die. When a star like the Sun has burned all of its hydrogen fuel, it expands to become a red giant while the rest of the stars become white dwarfs then cools down and becomes invisible. ...
... HOW DO STARS DIE ? •Most stars take millions of years to die. When a star like the Sun has burned all of its hydrogen fuel, it expands to become a red giant while the rest of the stars become white dwarfs then cools down and becomes invisible. ...
Document
... Medium Mass Stars • The main life of a medium mass stars is known as “main sequence stars” • There are different types of main sequence stars depending on the size/mass/ temperature/ ...
... Medium Mass Stars • The main life of a medium mass stars is known as “main sequence stars” • There are different types of main sequence stars depending on the size/mass/ temperature/ ...
astr study guide ex 3 s`16
... 2. Why don't we see hydrogen Balmer lines in the spectra of very cool stars? (like 3,000 K ...
... 2. Why don't we see hydrogen Balmer lines in the spectra of very cool stars? (like 3,000 K ...
Lesson 2 | The Sun and Other Stars
... Directions: On the line before each definition, write the letter of the term that matches it correctly. Each term is used only once. ...
... Directions: On the line before each definition, write the letter of the term that matches it correctly. Each term is used only once. ...
Final Review Questions. 1. Compare the atmospheric scale height of
... 18. Why is it that at T ∼ 107 K, the proton-proton chain and the CNO cycle produce roughly the same amount of energy, even though the CNO cycle requires much higher Gamov energies (and thus has much lower quantum tunneling probabilities)? 19. Why does the central temperature of the Sun increase slig ...
... 18. Why is it that at T ∼ 107 K, the proton-proton chain and the CNO cycle produce roughly the same amount of energy, even though the CNO cycle requires much higher Gamov energies (and thus has much lower quantum tunneling probabilities)? 19. Why does the central temperature of the Sun increase slig ...
Astronomy 115 Homework Set #1 – Due: Thursday, Feb
... 2. How many hydrogen atoms are converted to helium each second in order to power the Sun’s luminosity? To arrive at the solution, answer the following: (a) What is the mass of 4 hydrogen atoms? (b) What is the mass of 1 helium atom? (c) How much more mass is there in the 4 hydrogen atoms than in the ...
... 2. How many hydrogen atoms are converted to helium each second in order to power the Sun’s luminosity? To arrive at the solution, answer the following: (a) What is the mass of 4 hydrogen atoms? (b) What is the mass of 1 helium atom? (c) How much more mass is there in the 4 hydrogen atoms than in the ...
Slide 1 - Beverley High School
... • At the top left of the main sequence the stars have very large radius and high surface temperatures. This is what makes them highly luminous. • They are using up their hydrogen fuel tremendously quickly. So they are extremely short lived (c10 000 000 years) • These high mass stars finish their liv ...
... • At the top left of the main sequence the stars have very large radius and high surface temperatures. This is what makes them highly luminous. • They are using up their hydrogen fuel tremendously quickly. So they are extremely short lived (c10 000 000 years) • These high mass stars finish their liv ...
Star- large ball of gas held together by large ball of gas held
... For stars that are about the size of our sun, after main sequence they become giants, white dwarfs, and then black dwarfs. For stars larger than our sun, after main sequence and giant stage, they explode in supernovas, then become either black holes or neutron stars. ...
... For stars that are about the size of our sun, after main sequence they become giants, white dwarfs, and then black dwarfs. For stars larger than our sun, after main sequence and giant stage, they explode in supernovas, then become either black holes or neutron stars. ...
Astronomy Chapter 13 Name
... L. A star whose luminosity changes in time M. The region in the H-R diagram in which most stars are located N. A dense star whose radius is approximately equal to Earth’s but whose mass is comparable to the Sun’s O. Two stars in orbit around each other, held together by their mutual gravity P. A pai ...
... L. A star whose luminosity changes in time M. The region in the H-R diagram in which most stars are located N. A dense star whose radius is approximately equal to Earth’s but whose mass is comparable to the Sun’s O. Two stars in orbit around each other, held together by their mutual gravity P. A pai ...
Measuring Distances Beyond the Solar System The Characteristics
... Light travelling from the Sun distance 0.000016 ly away, takes approximately 8 minutes to reach Earth Light travelling from Vega distance 25 ly takes approximately 25 years to reach Earth. ...
... Light travelling from the Sun distance 0.000016 ly away, takes approximately 8 minutes to reach Earth Light travelling from Vega distance 25 ly takes approximately 25 years to reach Earth. ...
Document
... f. Which star’s spectrum most resembles the Sun’s? Centauri g. Which star is the closest (find m-M)? Centauri (m-M = -4.37) h. Which star has the smallest parallax angle? Canopus (m-M = 4.91) i. Which star can’t be seen without the use of a telescope? GL 725A j. How is it possible that Canopus i ...
... f. Which star’s spectrum most resembles the Sun’s? Centauri g. Which star is the closest (find m-M)? Centauri (m-M = -4.37) h. Which star has the smallest parallax angle? Canopus (m-M = 4.91) i. Which star can’t be seen without the use of a telescope? GL 725A j. How is it possible that Canopus i ...
ppt
... Therefore stars have an extremely large gravitational attraction that keeps their plasma held together. As gravity acts equally in all directions the plasma that forms the star is moulded into a sphere. But there must be some force keeping the star from collapsing in on itself. Because stars are so ...
... Therefore stars have an extremely large gravitational attraction that keeps their plasma held together. As gravity acts equally in all directions the plasma that forms the star is moulded into a sphere. But there must be some force keeping the star from collapsing in on itself. Because stars are so ...
Stellar types - schoolphysics
... diameters between 10 and 200 times that of the Sun. In spite of their relatively low surface temperature their enormous surface area means that they have luminosities between 100 and 10000 times that of the Sun. Aurigae (diameter about one hundred times that of the Sun) is an example of such a sta ...
... diameters between 10 and 200 times that of the Sun. In spite of their relatively low surface temperature their enormous surface area means that they have luminosities between 100 and 10000 times that of the Sun. Aurigae (diameter about one hundred times that of the Sun) is an example of such a sta ...
The Hot-plate Model of a Star Model of Stars— 3 Oct
... hot-plate get to my hand? What are two ways to make a hot plate produce more energy per second? (The same question applies to a star: What are two ways to make a star brighter or more luminous?) What can I do to make the same hot-plate at the same setting burn my hand and not burn my hand? ...
... hot-plate get to my hand? What are two ways to make a hot plate produce more energy per second? (The same question applies to a star: What are two ways to make a star brighter or more luminous?) What can I do to make the same hot-plate at the same setting burn my hand and not burn my hand? ...
Life Cycle of Stars
... lower right when plotted according to luminosity and surface temperature on the Hertzsprung-Russell diagram ...
... lower right when plotted according to luminosity and surface temperature on the Hertzsprung-Russell diagram ...
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.