PH109 Exploring the Universe, Test 3, Fall 2001 Please indicate the
... c) Gravity is inversely proportional to radius., d) Gravity is stronger the faster you go. 18. Sunspots appear dark because a) they are cooler regions, b) they are concentrations of carbon, c) their spectrum has been Doppler shifted, d) impurities in the Sun 19. The magnetic field in the Sun gets tw ...
... c) Gravity is inversely proportional to radius., d) Gravity is stronger the faster you go. 18. Sunspots appear dark because a) they are cooler regions, b) they are concentrations of carbon, c) their spectrum has been Doppler shifted, d) impurities in the Sun 19. The magnetic field in the Sun gets tw ...
OUR UNIVERSE Problem Set 7 Solutions Question A1 Question A2
... The early universe consisted of mainly hydrogen, a little helium, hence there was no iron, and stars made out of these materials and went through their evolution where very large stars can fuse elements up to Fe in their cores, releasing energy with each fusion reaction [1]. However, the fusion of i ...
... The early universe consisted of mainly hydrogen, a little helium, hence there was no iron, and stars made out of these materials and went through their evolution where very large stars can fuse elements up to Fe in their cores, releasing energy with each fusion reaction [1]. However, the fusion of i ...
Astronomy 103 Final review session - Home | UW
... • Moving from lower right to upper left, stars increase in radius • Moving from upper right to lower left, stars decrease in mass ...
... • Moving from lower right to upper left, stars increase in radius • Moving from upper right to lower left, stars decrease in mass ...
The Life Cycle of Stars Webquest
... Task #4: Types of Stars Continue to read on to the section “Types of Stars” on the same webpage http://www.seasky.org/cosmic/sky7a01.html and answer the following questions: 1. What does the main ...
... Task #4: Types of Stars Continue to read on to the section “Types of Stars” on the same webpage http://www.seasky.org/cosmic/sky7a01.html and answer the following questions: 1. What does the main ...
The Life Cycle of Stars Webquest
... Task #4: Types of Stars Continue to read on to the section “Types of Stars” on the same webpage http://www.seasky.org/cosmic/sky7a01.html and answer the following questions: 1. What does the main ...
... Task #4: Types of Stars Continue to read on to the section “Types of Stars” on the same webpage http://www.seasky.org/cosmic/sky7a01.html and answer the following questions: 1. What does the main ...
Characteristics of Stars
... amount of light given off by a star • Apparent magnitude – a measure of the amount of light received on Earth (a dim star can appear bright if its close to Earth; a bright star can appear dim if its far away) ...
... amount of light given off by a star • Apparent magnitude – a measure of the amount of light received on Earth (a dim star can appear bright if its close to Earth; a bright star can appear dim if its far away) ...
Stellar Evolution: The Live and Death of a Star
... The rest of the core is unbalanced & fusing at an increased rate ...
... The rest of the core is unbalanced & fusing at an increased rate ...
Unit 12 Guide: Concepts of Earth Science Stars, Galaxies, and the
... 4. Compare and contrast the apparent and actual motion of stars. How can scientists know if a star or galaxy is moving toward or away from Earth? 5. What is the difference between absolute and apparent magnitude? What is luminosity? 6. What are the three types of spectra? How can scientists use abso ...
... 4. Compare and contrast the apparent and actual motion of stars. How can scientists know if a star or galaxy is moving toward or away from Earth? 5. What is the difference between absolute and apparent magnitude? What is luminosity? 6. What are the three types of spectra? How can scientists use abso ...
COSMOLOGY 1 An Introduction to the Universe
... nebula of expelled gas. Radiation from this hot core will ionize the nebula, producing a striking "planetary nebula", much like the nebulae seen around the remnants of other stars. The carbon core will eventually cool and become a white dwarf, the dense dim remnant of a once bright star. ...
... nebula of expelled gas. Radiation from this hot core will ionize the nebula, producing a striking "planetary nebula", much like the nebulae seen around the remnants of other stars. The carbon core will eventually cool and become a white dwarf, the dense dim remnant of a once bright star. ...
Lec 25.2- STELLAR EVOLUTION SUMMARY
... How long a star remains a main-sequence, or hydrogen-burning, star, like our Sun and most others visible in the heavens, depends largely upon its mass. Our Sun has a main sequence lifetime of about ten billion years, of which approximately five billion have already passed. Larger stars burn faster a ...
... How long a star remains a main-sequence, or hydrogen-burning, star, like our Sun and most others visible in the heavens, depends largely upon its mass. Our Sun has a main sequence lifetime of about ten billion years, of which approximately five billion have already passed. Larger stars burn faster a ...
Star Life Cycles Stellar Nebula
... Stars begin life as cloud of gas + dust Cloud condenses and becomes more massive Nuclear fission begins (the power ...
... Stars begin life as cloud of gas + dust Cloud condenses and becomes more massive Nuclear fission begins (the power ...
Stars and the Sun
... – Big enough to swallow first 3 planets – Uses He other elements for about 10 million years ...
... – Big enough to swallow first 3 planets – Uses He other elements for about 10 million years ...
Stellar Evolution II
... Have a Different Story • Fusion in the core continues through many more stages than for low mass stars • Heavier elements are produced: – carbon, – oxygen, – neon, – silicon, – and so on up to iron ...
... Have a Different Story • Fusion in the core continues through many more stages than for low mass stars • Heavier elements are produced: – carbon, – oxygen, – neon, – silicon, – and so on up to iron ...
Monday, Oct. 20
... to about ½ AU, and it will become more than 100 times more luminous than it is now. Life will not be pleasant on Earth. The core of the Sun will be mostly helium, and will continue to contract and heat up. When the temperature in the core reaches about 108 K (about 1 million years after the Sun leav ...
... to about ½ AU, and it will become more than 100 times more luminous than it is now. Life will not be pleasant on Earth. The core of the Sun will be mostly helium, and will continue to contract and heat up. When the temperature in the core reaches about 108 K (about 1 million years after the Sun leav ...
Can We Make A Star?
... • They are made of cosmic dust, mostly hydrogen and helium • They are very unstable • The are very violent • They give off an extremely large amount of energy ...
... • They are made of cosmic dust, mostly hydrogen and helium • They are very unstable • The are very violent • They give off an extremely large amount of energy ...
Life2
... original matter from Big Bang into clumps called protostars. Hysdrostatic equilibrium is established where outward radiation pressure balances gravity. A Star is born! Early stars had very little metallicity (i.e. no heavy elements). Stellar evolution - (main sequence) – Life cycle of a star depends ...
... original matter from Big Bang into clumps called protostars. Hysdrostatic equilibrium is established where outward radiation pressure balances gravity. A Star is born! Early stars had very little metallicity (i.e. no heavy elements). Stellar evolution - (main sequence) – Life cycle of a star depends ...
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.