Ch. 20
... As the blue-giant star entered its red-giant phase, it expanded to the point where mass ...
... As the blue-giant star entered its red-giant phase, it expanded to the point where mass ...
The Evolution of the Universe and the formation of Black Holes
... which lasts for billions of years. During that time, it begins to cool and condense into socalled dark matter. The smallest particles of mass, thions and tachyons, which due do its high energy potential and their speed which is faster than the speed of light chaotically move around the entire univer ...
... which lasts for billions of years. During that time, it begins to cool and condense into socalled dark matter. The smallest particles of mass, thions and tachyons, which due do its high energy potential and their speed which is faster than the speed of light chaotically move around the entire univer ...
Universe 19
... How far away are the stars? What evidence do astronomers have that the Sun is a typical star? 3. What is meant by a “first-magnitude” or “secondmagnitude” star? 4. Why are some stars red and others blue? 5. What are the stars made of? 6. As stars go, is our Sun especially large or small? 7. What are ...
... How far away are the stars? What evidence do astronomers have that the Sun is a typical star? 3. What is meant by a “first-magnitude” or “secondmagnitude” star? 4. Why are some stars red and others blue? 5. What are the stars made of? 6. As stars go, is our Sun especially large or small? 7. What are ...
Chapter 12
... it becomes a protostar surrounded by a spinning disk of gas. —The protostar may also fire jets of matter ...
... it becomes a protostar surrounded by a spinning disk of gas. —The protostar may also fire jets of matter ...
eneb_form
... the light coming from the Sun. The tail has to always point away from the Sun, regardless of how the comet moving. ...
... the light coming from the Sun. The tail has to always point away from the Sun, regardless of how the comet moving. ...
Star Stuff
... The Hertzsprung-Russell Diagram (H-R Diagram) Properties of stars on the Main-Sequence • fusing H He in their cores • the length of time fusion can last depends on how much “fuel” is there for fusion and the rate at which fusion occurs • amount of fuel = star’s MASS • rate of fusion = star’s LUMI ...
... The Hertzsprung-Russell Diagram (H-R Diagram) Properties of stars on the Main-Sequence • fusing H He in their cores • the length of time fusion can last depends on how much “fuel” is there for fusion and the rate at which fusion occurs • amount of fuel = star’s MASS • rate of fusion = star’s LUMI ...
A Star is
... • Scientists have learned that all stars are made up of the same elements which compose Earth. • The most common elements in stars are hydrogen and helium, in that order. • Small quantities of carbon, oxygen, and nitrogen are also found in stars, but stars are primarily composed of…. • HYDROGEN and ...
... • Scientists have learned that all stars are made up of the same elements which compose Earth. • The most common elements in stars are hydrogen and helium, in that order. • Small quantities of carbon, oxygen, and nitrogen are also found in stars, but stars are primarily composed of…. • HYDROGEN and ...
HR Diagrams
... Do you think that taller students tend to weigh more or less than shorter students? You could examine this by plotting the students in your class on a graph, with height on one axis and weight on the other. Each student would be plotted as a point on the graph. What do you think that graph would loo ...
... Do you think that taller students tend to weigh more or less than shorter students? You could examine this by plotting the students in your class on a graph, with height on one axis and weight on the other. Each student would be plotted as a point on the graph. What do you think that graph would loo ...
Death - Wayne State University Physics and Astronomy
... • After the nova burst, gas from the regular star begins to build up again on the white dwarf's surface • A binary system can have repeating nova bursts • If enough mass accumulates on the white dwarf to push it over the 1.4 solar mass limit, the degenerate electrons will not be able to stop gravity ...
... • After the nova burst, gas from the regular star begins to build up again on the white dwarf's surface • A binary system can have repeating nova bursts • If enough mass accumulates on the white dwarf to push it over the 1.4 solar mass limit, the degenerate electrons will not be able to stop gravity ...
Take Home #2 Complete the following on your own paper. Do not
... 11) Which two factors combine together to cause an object to remain in a stable orbit? A. gravity and inertia D. heat and electricity B. mass and magnetism E. temperature and luminosity C. fusion and fission 12) Why does a comet's ion tail always point away from the sun? A. galactic gravity pulls it ...
... 11) Which two factors combine together to cause an object to remain in a stable orbit? A. gravity and inertia D. heat and electricity B. mass and magnetism E. temperature and luminosity C. fusion and fission 12) Why does a comet's ion tail always point away from the sun? A. galactic gravity pulls it ...
The Daily Sun 1st Sept
... To start with, he talked about the famous Einstein-Tagore discussion of 1926 (at Einstein’s home in Berlin) where they exchanged their own respected ideas about universe and harmony of nature. Professor Mofiz Uddin Ahmed continued: “A star is born from a proto-star and evolved to a red giant. And f ...
... To start with, he talked about the famous Einstein-Tagore discussion of 1926 (at Einstein’s home in Berlin) where they exchanged their own respected ideas about universe and harmony of nature. Professor Mofiz Uddin Ahmed continued: “A star is born from a proto-star and evolved to a red giant. And f ...
PPT - Mr.E Science
... Nebula – a huge gas cloud made up mainly of Hydrogen that collapse down on itself and compresses the gas down into a Protostar Star is “born” when the protostar has contracting tight enough for Hydrogen to fuse into Helium, this releases the light and energy we normally associate with a “normal” sta ...
... Nebula – a huge gas cloud made up mainly of Hydrogen that collapse down on itself and compresses the gas down into a Protostar Star is “born” when the protostar has contracting tight enough for Hydrogen to fuse into Helium, this releases the light and energy we normally associate with a “normal” sta ...
Stars - Mike Brotherton
... The Deaths of Massive Stars: Supernovae Final stages of fusion in high-mass stars (> 8 Msun), leading to the formation of an iron ...
... The Deaths of Massive Stars: Supernovae Final stages of fusion in high-mass stars (> 8 Msun), leading to the formation of an iron ...
This link is in pdf format for ease of reading
... Eventually, all stars run out of fuel in their cores. They lose their equilibrium as the force of gravity comes to dominate. Different-mass stars end their lives differently. Low-mass stars die quietly as their nuclear fires dwindle. The core in a Sun-like star collapses rapidly into an Earth-size w ...
... Eventually, all stars run out of fuel in their cores. They lose their equilibrium as the force of gravity comes to dominate. Different-mass stars end their lives differently. Low-mass stars die quietly as their nuclear fires dwindle. The core in a Sun-like star collapses rapidly into an Earth-size w ...
![Dust [12.1]](http://s1.studyres.com/store/data/008843506_1-c0b3bc1292042697e2dbc020b2f06e1c-300x300.png)
Dust [12.1]
... • Globular clusters (12-15 Gyr) • Halo field stars • Bulge??? ….but includes metal rich stars. ...
... • Globular clusters (12-15 Gyr) • Halo field stars • Bulge??? ….but includes metal rich stars. ...
Last time we left off at hydrogen and helium, because that`s all that
... generating energy, so that’s the end of the road. For most stars, actually, they never get to that stage, and simply burn hydrogen and (for stars other than the least massive) then helium. In principle, then, plenty of carbon and other heavier nuclei are produced in stars. However, stars are too hot ...
... generating energy, so that’s the end of the road. For most stars, actually, they never get to that stage, and simply burn hydrogen and (for stars other than the least massive) then helium. In principle, then, plenty of carbon and other heavier nuclei are produced in stars. However, stars are too hot ...
Unit 11: Stellar Evolution
... compressed, its rotation speed increases, keeping the angular momentum constant. The rapid rotation has very important consequences for the formation of planets, which we will discuss in a later reading on our solar system. A second consequence of gravitational collapse is that the particles of the ...
... compressed, its rotation speed increases, keeping the angular momentum constant. The rapid rotation has very important consequences for the formation of planets, which we will discuss in a later reading on our solar system. A second consequence of gravitational collapse is that the particles of the ...
Stars - Quia
... What is a star? - body of gasses that give off “tons of” energy (light & heat) - clusters = those little specks in the sky that we see may really be more than one star…. ...
... What is a star? - body of gasses that give off “tons of” energy (light & heat) - clusters = those little specks in the sky that we see may really be more than one star…. ...
White dwarfs that crossed the Chandrasekhar limit
... Thus, our Sun is destined to eject out a planetary nebula and end up as a white dwarf. Chandrasekhar estimated that, as long as the end stage of a less massive star resulting from a planetary nebula is less than 1.44 times the mass of the Sun [M], it survives as a faintly visible white dwarf (Box 1 ...
... Thus, our Sun is destined to eject out a planetary nebula and end up as a white dwarf. Chandrasekhar estimated that, as long as the end stage of a less massive star resulting from a planetary nebula is less than 1.44 times the mass of the Sun [M], it survives as a faintly visible white dwarf (Box 1 ...
7a Properties of Stars.pptx
... • Pulsate in brightness because of the expansion and contrac7on of their outer layers • Cepheid stars – get brighter and fainter in a regular pa?ern ...
... • Pulsate in brightness because of the expansion and contrac7on of their outer layers • Cepheid stars – get brighter and fainter in a regular pa?ern ...
Observational Astronomy - Spring 2014 Homework 7
... • Spacecraft take hundreds to thousands of watts of power, so it would take really large solar cells to power a spacecraft at Neptune, too large to be practical. For this reason, deep-space missions are nuclear powered. 3. What process powers the stars? What element does the Sun consume for fuel and ...
... • Spacecraft take hundreds to thousands of watts of power, so it would take really large solar cells to power a spacecraft at Neptune, too large to be practical. For this reason, deep-space missions are nuclear powered. 3. What process powers the stars? What element does the Sun consume for fuel and ...
Document
... The more massive the protostar, the more rapidly it evolves • Greater mass, contracts and heats more rapidly, and hydrogen fusion begins earlier • Greater mass, greater pressure and temperature in the core • If protostar less than 0.08 Msun, it can never develop the temperature and pressure to star ...
... The more massive the protostar, the more rapidly it evolves • Greater mass, contracts and heats more rapidly, and hydrogen fusion begins earlier • Greater mass, greater pressure and temperature in the core • If protostar less than 0.08 Msun, it can never develop the temperature and pressure to star ...
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.