MT 2 Answers Version C
... 11. Which sequence correctly lists the spectral classes of stars in order of decreasing temperature (from hottest to coolest)? (a) ...
... 11. Which sequence correctly lists the spectral classes of stars in order of decreasing temperature (from hottest to coolest)? (a) ...
MT 2 Answers Version D
... read through all the answers. Take your time. If a question is unclear, ask for clarification during the exam. Mark your answers on the scantron sheet and on your copy of the exam. Keep your copy of the exam and check your grade with the posted answers on the course website and the grade posted on D ...
... read through all the answers. Take your time. If a question is unclear, ask for clarification during the exam. Mark your answers on the scantron sheet and on your copy of the exam. Keep your copy of the exam and check your grade with the posted answers on the course website and the grade posted on D ...
EARTH SCIENCE KEY NOTES
... LEAD (low or medium mass compared to a high mass star). 1) Stars begin their lives as Molecular Clouds called Nebula (called stellar nurseries). 2) Protostar: forms when a nebula is dense and cool enough to begin contracting into a star (GRAVITY). 3) When hydrogen begins to fuse into helium the prot ...
... LEAD (low or medium mass compared to a high mass star). 1) Stars begin their lives as Molecular Clouds called Nebula (called stellar nurseries). 2) Protostar: forms when a nebula is dense and cool enough to begin contracting into a star (GRAVITY). 3) When hydrogen begins to fuse into helium the prot ...
DUPREE_SPLINTER
... Candidates for second parameter: age, environment (including free-floating planets); primordial He abundance; surface pollution (helium); CNO abundances; rotation; mass loss….. ...
... Candidates for second parameter: age, environment (including free-floating planets); primordial He abundance; surface pollution (helium); CNO abundances; rotation; mass loss….. ...
Stars
... – Very large, massive stars burn their fuel much faster than smaller stars – Main sequence may last only a few hundred thousand years – Smaller stars will live on for billions of years because they burn their fuel much more slowly ...
... – Very large, massive stars burn their fuel much faster than smaller stars – Main sequence may last only a few hundred thousand years – Smaller stars will live on for billions of years because they burn their fuel much more slowly ...
H-R Diagram - Faculty Website Listing
... Please read the section in textbook that talks about HR diagram. We have also discussed this in class with examples. It may be useful to have your class notes with you when you do the lab. You can also look them up on the class webpage. 1. Using Stellarium software to collect the information on abso ...
... Please read the section in textbook that talks about HR diagram. We have also discussed this in class with examples. It may be useful to have your class notes with you when you do the lab. You can also look them up on the class webpage. 1. Using Stellarium software to collect the information on abso ...
Sources of energy and the origin of the chemical elements
... When the triple-α process in a red-giant is complete, the star core starts contracting. For a main sequence mass of M < 4 M¤ there is not enough energy to ignite the carbon fusion process, thus the collapse keeps going until it is halted by the pressure arising from electron degeneracy. From the st ...
... When the triple-α process in a red-giant is complete, the star core starts contracting. For a main sequence mass of M < 4 M¤ there is not enough energy to ignite the carbon fusion process, thus the collapse keeps going until it is halted by the pressure arising from electron degeneracy. From the st ...
Origins Of The Universe
... expansion then the Universe will eventually stop expanding and begin contracting (which could be cyclic…) Constant expansion – if the mass is below the critical point then the Universe will expand forever ...
... expansion then the Universe will eventually stop expanding and begin contracting (which could be cyclic…) Constant expansion – if the mass is below the critical point then the Universe will expand forever ...
Astronomy 328 Midterm Exam - Department of Physics and Astronomy
... exert a greater degeneracy pressure. Explain why this is the case. Why then are the more massive stars (neutron stars) supported by neutron degeneracy pressure? (3 pts) ...
... exert a greater degeneracy pressure. Explain why this is the case. Why then are the more massive stars (neutron stars) supported by neutron degeneracy pressure? (3 pts) ...
Stellar Evolution after the Main Sequence
... You can see that the Silicon Iron stage takes place in a single day. It's here that there is A Serious Problem for our massive star. Iron occupies a rather special place for the elements. Iron is at the top of the "Binding Energy Curve". This means creating all of the elements by nuclear fusion ha ...
... You can see that the Silicon Iron stage takes place in a single day. It's here that there is A Serious Problem for our massive star. Iron occupies a rather special place for the elements. Iron is at the top of the "Binding Energy Curve". This means creating all of the elements by nuclear fusion ha ...
Final Exam Practice Part I
... 6. The inner planets of our solar system are rocky, while the outer planets are “gas giants.” Why are the inner and outer planets different? 7. What is Nuclear Fusion? 8. How does nuclear fusion produce energy? 9. Nuclear fusion can only occur in the center of the solar system. Why is that? 10. What ...
... 6. The inner planets of our solar system are rocky, while the outer planets are “gas giants.” Why are the inner and outer planets different? 7. What is Nuclear Fusion? 8. How does nuclear fusion produce energy? 9. Nuclear fusion can only occur in the center of the solar system. Why is that? 10. What ...
Types of Planets and Stars
... are main sequence stars that have very little mass and are cooler than stars like Earth’s sun. Because of this, they use hydrogen more slowly, which allows them to burn longer than most stars. Its lifetime, 80-100 billion years, is older than the universe. Super Giants -- because of their size, th ...
... are main sequence stars that have very little mass and are cooler than stars like Earth’s sun. Because of this, they use hydrogen more slowly, which allows them to burn longer than most stars. Its lifetime, 80-100 billion years, is older than the universe. Super Giants -- because of their size, th ...
Stellar Lifetime - Madison Public Schools
... down to almost 1 solar radius • Its central temperature reaches 10,000,000 K • Fusion of Hydrogen begins • It is still not on the main sequence ...
... down to almost 1 solar radius • Its central temperature reaches 10,000,000 K • Fusion of Hydrogen begins • It is still not on the main sequence ...
SISTERS OF THE SUN
... 8. The super hot gas in the Sun’s interior pushes ____________________ while its ______________________ pulls it ____________________. 9. At present, the Sun fuses hydrogen. In a future phase, it will fuse ______________________________. 10. The Sun will eventually devour The Sun’s final state will ...
... 8. The super hot gas in the Sun’s interior pushes ____________________ while its ______________________ pulls it ____________________. 9. At present, the Sun fuses hydrogen. In a future phase, it will fuse ______________________________. 10. The Sun will eventually devour The Sun’s final state will ...
Stars and the Sun
... • In these conditions - Stars convert hydrogen to helium • As stars age, the run out of hydrogen and begin making carbon, oxygen, nitrogen… • Older stars can produce elements as heavy as lead ...
... • In these conditions - Stars convert hydrogen to helium • As stars age, the run out of hydrogen and begin making carbon, oxygen, nitrogen… • Older stars can produce elements as heavy as lead ...
CO 2 Cycle
... • Evolution of High-Mass Stars – What’s the nuclear fusion process during the MS stage? – What’s the inside looks like when it’s a giant? – Why does fusion stop? – Why does fusion stop? – How do they end their life? – What becomes of high-mass stars after they die? ...
... • Evolution of High-Mass Stars – What’s the nuclear fusion process during the MS stage? – What’s the inside looks like when it’s a giant? – Why does fusion stop? – Why does fusion stop? – How do they end their life? – What becomes of high-mass stars after they die? ...
Lives of stars HR
... The tool we use to study stars is called the Hertzsprung-Russell diagram. It plots two observable quantities: the absolute brightness of a star and the temperature of a star. Combined with some laws of physics, the HR diagram provides a way to understand how stars evolve with time. ...
... The tool we use to study stars is called the Hertzsprung-Russell diagram. It plots two observable quantities: the absolute brightness of a star and the temperature of a star. Combined with some laws of physics, the HR diagram provides a way to understand how stars evolve with time. ...
Space
... 3. To magnify the image produced by the eyepiece 4. To produce an image that is magnified by the eyepiece 5. To split light from stars into different colours. ...
... 3. To magnify the image produced by the eyepiece 4. To produce an image that is magnified by the eyepiece 5. To split light from stars into different colours. ...
STAR LIGHT, STAR BRIGHT
... Activity 2: Exploring Characteristics of Stars COLOR AND TEMPERATURE (Text Page 127) 5. What does the color of a star indicate about the star? ___________________________________ 6. Identify the temperature associated with each color, and include an example of a star that would appear each color. Te ...
... Activity 2: Exploring Characteristics of Stars COLOR AND TEMPERATURE (Text Page 127) 5. What does the color of a star indicate about the star? ___________________________________ 6. Identify the temperature associated with each color, and include an example of a star that would appear each color. Te ...
xam2ans
... to the most energetic electrons. In that case, the total energy of the system decreases if the quoted reaction makes some electrons disappear. (e) Nuclear reactions never become significant in the lowest-mass “stars.” Explain why. Answer: Low-mass stars have high densities. If the density is high en ...
... to the most energetic electrons. In that case, the total energy of the system decreases if the quoted reaction makes some electrons disappear. (e) Nuclear reactions never become significant in the lowest-mass “stars.” Explain why. Answer: Low-mass stars have high densities. If the density is high en ...
Energy Levels in Atoms
... The spectra from two different atoms are observed. A spectral line in the first atom has exactly one-half the wavelength of a spectral line in the second atom. Which of the below is TRUE? • The spacing between 2 levels in the first atom must be twice the spacing between 2 levels in the second atom. ...
... The spectra from two different atoms are observed. A spectral line in the first atom has exactly one-half the wavelength of a spectral line in the second atom. Which of the below is TRUE? • The spacing between 2 levels in the first atom must be twice the spacing between 2 levels in the second atom. ...
PHYSICS 1500 ASTRONOMY Sample Exam Solutions Section B
... (a) As a roughly spherical cloud core contracts under the action of gravity, it spins up because of conservation of angular momentum. This effect is greatest for the gas farthest from the rotation axis, which spins up sufficiently to resist farther contraction it orbits the centre instead. Material ...
... (a) As a roughly spherical cloud core contracts under the action of gravity, it spins up because of conservation of angular momentum. This effect is greatest for the gas farthest from the rotation axis, which spins up sufficiently to resist farther contraction it orbits the centre instead. Material ...
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.