Answer ALL questions from SECTION A and TWO questions from
... 4. List the physical processes that give rise to the continuous opacity in stars. ...
... 4. List the physical processes that give rise to the continuous opacity in stars. ...
PS 224, Fall 2014 HW 4
... False. How bright a star appears depends on the luminosity of a stars and its distance away from us. d. Some of the stars on the main sequence of the H-R diagram are not converting hydrogen into helium. False. The main-seuqence is defined as the phase of a star’s life when it burns hydrogen into hel ...
... False. How bright a star appears depends on the luminosity of a stars and its distance away from us. d. Some of the stars on the main sequence of the H-R diagram are not converting hydrogen into helium. False. The main-seuqence is defined as the phase of a star’s life when it burns hydrogen into hel ...
Astronomy 112: Physics of Stars Problem set 2: Due April 29 1. Time
... 7. Polytropes: A neutron star is roughly describable as a polytrope of index 1. The radius of a typical neutron star of mass 1.4 solar masses is 10 km. What is its central density? The density of the atomic nucleus is 2.4 x 10**14 g cm−3 . Compare the value you computed to this number. Neutron stars ...
... 7. Polytropes: A neutron star is roughly describable as a polytrope of index 1. The radius of a typical neutron star of mass 1.4 solar masses is 10 km. What is its central density? The density of the atomic nucleus is 2.4 x 10**14 g cm−3 . Compare the value you computed to this number. Neutron stars ...
Sun, Stars, HR Diagram
... white dwarf B) to shrink to a white dwarf then eventually expand to a red giant C) become hotter and expand into a blue supergiant D) to become a black hole 17. By using a spectroscope an astronomer can A) B) C) D) ...
... white dwarf B) to shrink to a white dwarf then eventually expand to a red giant C) become hotter and expand into a blue supergiant D) to become a black hole 17. By using a spectroscope an astronomer can A) B) C) D) ...
Chapter 40
... – Older stars had only hydrogen and helium – Elements heavier than hydrogen and helium came from the core of stars – When stars die, they spew material out – Newer stars are composed of heavier elements – We are made of star dust! ...
... – Older stars had only hydrogen and helium – Elements heavier than hydrogen and helium came from the core of stars – When stars die, they spew material out – Newer stars are composed of heavier elements – We are made of star dust! ...
Stellar Evolution - Hays High Indians
... – Small low mass stars can take billions of years to form – More massive stars can completely form in a few hundred thousand years ...
... – Small low mass stars can take billions of years to form – More massive stars can completely form in a few hundred thousand years ...
Theoretical Problem 3
... The stars are spheres of hot gas. Most of them shine because they are fusing hydrogen into helium in their central parts. In this problem we use concepts of both classical and quantum mechanics, as well as of electrostatics and thermodynamics, to understand why stars have to be big enough to achieve ...
... The stars are spheres of hot gas. Most of them shine because they are fusing hydrogen into helium in their central parts. In this problem we use concepts of both classical and quantum mechanics, as well as of electrostatics and thermodynamics, to understand why stars have to be big enough to achieve ...
For instance, two hydrogen atoms may fuse together to form one
... 1. Why might stars of one color be much more abundant than stars of another color? 2. Which type(s) of stars should we consider when looking for stars that might have lifesupporting worlds around them? Why? 3. Which Term(s) in the Drake Equation would be affected by the evidence provided in the ...
... 1. Why might stars of one color be much more abundant than stars of another color? 2. Which type(s) of stars should we consider when looking for stars that might have lifesupporting worlds around them? Why? 3. Which Term(s) in the Drake Equation would be affected by the evidence provided in the ...
Astronomy Webquest _2 STARS
... outwards into its atmosphere and burn the hydrogen that’s in a shell surrounding the core. As a result, the outside of the star starts to expand and cool, turning much redder. Over time, the star will change into a ___________________________ and grow to more than 400 times its original size. As the ...
... outwards into its atmosphere and burn the hydrogen that’s in a shell surrounding the core. As a result, the outside of the star starts to expand and cool, turning much redder. Over time, the star will change into a ___________________________ and grow to more than 400 times its original size. As the ...
The Life of a Star
... throws its outer layers into space, forming a planetary nebula – This leaves behind the hot dense core of the red giant. – The remaining core is called a white dwarf. Over time, the white dwarf cools off and becomes a black dwarf. Planetary Nebula: A collection of gas and dust that was formed during ...
... throws its outer layers into space, forming a planetary nebula – This leaves behind the hot dense core of the red giant. – The remaining core is called a white dwarf. Over time, the white dwarf cools off and becomes a black dwarf. Planetary Nebula: A collection of gas and dust that was formed during ...
Stars and Galaxies
... explode into a supernova leaving behind a core that is even more dense than a neutron star? Such gravitational forces would be so great that not even light could escape We call these black holes ...
... explode into a supernova leaving behind a core that is even more dense than a neutron star? Such gravitational forces would be so great that not even light could escape We call these black holes ...
The Family of Stars
... The Deaths of Massive Stars: Supernovae Final stages of fusion in high-mass stars (> 8 Msun), leading to the formation of an iron core, happen extremely rapidly: Si burning lasts only for ~ 1 day. Iron core ultimately collapses, triggering an explosion that destroys the star: ...
... The Deaths of Massive Stars: Supernovae Final stages of fusion in high-mass stars (> 8 Msun), leading to the formation of an iron core, happen extremely rapidly: Si burning lasts only for ~ 1 day. Iron core ultimately collapses, triggering an explosion that destroys the star: ...
Lecture 10 - Concord University
... Do we have all this right? How do we check all this out? (1) Star clusters are perfect because they contain stars in many of the evolutionary phases. Can test timescale, surface temperature and luminosity predictions. After 30 years of testing, it looks like we understand the basic evolution o ...
... Do we have all this right? How do we check all this out? (1) Star clusters are perfect because they contain stars in many of the evolutionary phases. Can test timescale, surface temperature and luminosity predictions. After 30 years of testing, it looks like we understand the basic evolution o ...
Teacher Subject Title Concept Context Tek/SE Verb
... What do you see when you look up at the sky? Does the sky look the same during the day as it does at night? Other than the Moon, what do we see in the night sky? What do you know about stars? Misconceptions: students may think that all of the stars in a constellation are near each other. Students ma ...
... What do you see when you look up at the sky? Does the sky look the same during the day as it does at night? Other than the Moon, what do we see in the night sky? What do you know about stars? Misconceptions: students may think that all of the stars in a constellation are near each other. Students ma ...
Stars
... Did you know that stars die and can turn into different things after they're dead? Well all of that is true! A star starts to die when their core runs out of hydrogen and then helium. The dead star could become a black hole, a neutron star or a black dwarf depending on how big or small it is. Bigger ...
... Did you know that stars die and can turn into different things after they're dead? Well all of that is true! A star starts to die when their core runs out of hydrogen and then helium. The dead star could become a black hole, a neutron star or a black dwarf depending on how big or small it is. Bigger ...
Astronomy 103 Exam 2 Review
... A. They are the most massive stars and have more hydrogen fuel B. Their core pressure and temperature are low so the rate of hydrogen fusion is low C. They are fully convecLve D. B and C ...
... A. They are the most massive stars and have more hydrogen fuel B. Their core pressure and temperature are low so the rate of hydrogen fusion is low C. They are fully convecLve D. B and C ...
the lives of stars
... sky. People named these patterns, called constellations and told stories about them. This picture shows one of the most easily recognized constellations. The ancient Greeks thought this group of stars looked like a hunter from one of their myths, so they named it Orion after a great hunter. The patt ...
... sky. People named these patterns, called constellations and told stories about them. This picture shows one of the most easily recognized constellations. The ancient Greeks thought this group of stars looked like a hunter from one of their myths, so they named it Orion after a great hunter. The patt ...
The Sun, Stars, and Beyond
... • Irregularly shaped galaxies also exist, though fewer in number. • A galaxy’s shape is determined by its rate of spin, and if it has been subject to any collisions or mergers. • These all contain 100 billion stars or more, and there are 100 billion galaxies out there! ...
... • Irregularly shaped galaxies also exist, though fewer in number. • A galaxy’s shape is determined by its rate of spin, and if it has been subject to any collisions or mergers. • These all contain 100 billion stars or more, and there are 100 billion galaxies out there! ...
Characteristics of Main Sequence Stars
... temperature slightly.) The relation also flattens significantly at the very faint end of the luminosity function. This is due to the increasing important of convection for stellar structure. • Main sequence stars obey a mass-radius relation. However, the relation displays a significant break around ...
... temperature slightly.) The relation also flattens significantly at the very faint end of the luminosity function. This is due to the increasing important of convection for stellar structure. • Main sequence stars obey a mass-radius relation. However, the relation displays a significant break around ...
Star
A star is a luminous sphere of plasma held together by its own gravity. The nearest star to Earth is the Sun. Other stars are visible from Earth during the night, appearing as a multitude of fixed luminous points in the sky due to their immense distance from Earth. Historically, the most prominent stars were grouped into constellations and asterisms, and the brightest stars gained proper names. Extensive catalogues of stars have been assembled by astronomers, which provide standardized star designations.For at least a portion of its life, a star shines due to thermonuclear fusion of hydrogen into helium in its core, releasing energy that traverses the star's interior and then radiates into outer space. Once the hydrogen in the core of a star is nearly exhausted, almost all naturally occurring elements heavier than helium are created by stellar nucleosynthesis during the star's lifetime and, for some stars, by supernova nucleosynthesis when it explodes. Near the end of its life, a star can also contain degenerate matter. Astronomers can determine the mass, age, metallicity (chemical composition), and many other properties of a star by observing its motion through space, luminosity, and spectrum respectively. The total mass of a star is the principal determinant of its evolution and eventual fate. Other characteristics of a star, including diameter and temperature, change over its life, while the star's environment affects its rotation and movement. A plot of the temperature of many stars against their luminosities, known as a Hertzsprung–Russell diagram (H–R diagram), allows the age and evolutionary state of a star to be determined.A star's life begins with the gravitational collapse of a gaseous nebula of material composed primarily of hydrogen, along with helium and trace amounts of heavier elements. Once the stellar core is sufficiently dense, hydrogen becomes steadily converted into helium through nuclear fusion, releasing energy in the process. The remainder of the star's interior carries energy away from the core through a combination of radiative and convective processes. The star's internal pressure prevents it from collapsing further under its own gravity. Once the hydrogen fuel at the core is exhausted, a star with at least 0.4 times the mass of the Sun expands to become a red giant, in some cases fusing heavier elements at the core or in shells around the core. The star then evolves into a degenerate form, recycling a portion of its matter into the interstellar environment, where it will contribute to the formation of a new generation of stars with a higher proportion of heavy elements. Meanwhile, the core becomes a stellar remnant: a white dwarf, a neutron star, or (if it is sufficiently massive) a black hole.Binary and multi-star systems consist of two or more stars that are gravitationally bound, and generally move around each other in stable orbits. When two such stars have a relatively close orbit, their gravitational interaction can have a significant impact on their evolution. Stars can form part of a much larger gravitationally bound structure, such as a star cluster or a galaxy.