HW #9 Answers (Due 10/28)
... 3) What causes a lower mass star to lose its outer envelope as a planetary nebula and thus expose the core which is a white dwarf? It is the sporadic helium shell burning which occurs during the asymptotic giant branch phase. See question #1 for description of this. ...
... 3) What causes a lower mass star to lose its outer envelope as a planetary nebula and thus expose the core which is a white dwarf? It is the sporadic helium shell burning which occurs during the asymptotic giant branch phase. See question #1 for description of this. ...
Test 3, February 7, 2007 - Brock physics
... (a) Protostar, main-sequence, yellow giant, red giant, neutron star or a black hole. (b) Protostar, main-sequence, red giant, yellow giant, red giant, white dwarf. 31. Which is the heaviest element that can be obtained through nuclear fusion of the lighter ones with a release of energy? (a) Gold. (b ...
... (a) Protostar, main-sequence, yellow giant, red giant, neutron star or a black hole. (b) Protostar, main-sequence, red giant, yellow giant, red giant, white dwarf. 31. Which is the heaviest element that can be obtained through nuclear fusion of the lighter ones with a release of energy? (a) Gold. (b ...
STAR TYPES
... Hertzsprung - Russell Diagram The Hertzsprung -Russell (H-R) Diagram is a graph that plots stars color (spectral type or surface temperature) vs. its luminosity (intrinsic brightness or absolute magnitude). On it, astronomers plot stars' color, temperature, luminosity, spectral type, and evolutionar ...
... Hertzsprung - Russell Diagram The Hertzsprung -Russell (H-R) Diagram is a graph that plots stars color (spectral type or surface temperature) vs. its luminosity (intrinsic brightness or absolute magnitude). On it, astronomers plot stars' color, temperature, luminosity, spectral type, and evolutionar ...
Low Mass
... • As stars burn H to He, He builds up in the core. • Stars begin to “die” when they run out of hydrogen in their core. • No hydrogen fusion in core • Core collapses because there is no longer balance between gravity and outward pressure (no more hydrostatic equilibrium) ...
... • As stars burn H to He, He builds up in the core. • Stars begin to “die” when they run out of hydrogen in their core. • No hydrogen fusion in core • Core collapses because there is no longer balance between gravity and outward pressure (no more hydrostatic equilibrium) ...
Volcanoes and Igneous Activity Earth - Chapter 4
... the use of instructors in teaching their courses and assessing student learning. Dissemination or sale of any part of this work (including on the World Wide Web) will destroy the integrity of the work and is not permitted. The work and materials from it should never be made available to students exc ...
... the use of instructors in teaching their courses and assessing student learning. Dissemination or sale of any part of this work (including on the World Wide Web) will destroy the integrity of the work and is not permitted. The work and materials from it should never be made available to students exc ...
Black Hole
... It is likely that very massive black holes exist at the centers of most galaxies. Black holes of a few solar masses are believed to form when massive stars undergo core collapse if the collapsed core exceeds the maximum of ~ 3 M permitted for neutron stars. The best evidence for such black holes co ...
... It is likely that very massive black holes exist at the centers of most galaxies. Black holes of a few solar masses are believed to form when massive stars undergo core collapse if the collapsed core exceeds the maximum of ~ 3 M permitted for neutron stars. The best evidence for such black holes co ...
B - Department of Physics and Astronomy
... 17. In some binary star systems, such as Algol, the less massive star is a red giant and the more massive star is on the main sequence. This is evidence that A. *mass transfer has occurred from one star to another B. the more massive star formed later, from a disk of gas surrounding the less massive ...
... 17. In some binary star systems, such as Algol, the less massive star is a red giant and the more massive star is on the main sequence. This is evidence that A. *mass transfer has occurred from one star to another B. the more massive star formed later, from a disk of gas surrounding the less massive ...
STEM for TY Teachers
... ! Supergiant: A supergiant star is the largest known type of star; some are almost as large as our entire solar system. Betelgeuse and Rigel are supergiants. These stars are rare. When supergiants die they explode as a supernova and may produce black holes. ...
... ! Supergiant: A supergiant star is the largest known type of star; some are almost as large as our entire solar system. Betelgeuse and Rigel are supergiants. These stars are rare. When supergiants die they explode as a supernova and may produce black holes. ...
Masses are much harder than distance, luminosity, or temperature
... • Range of different mass stars! ...
... • Range of different mass stars! ...
Binary Star - Armagh Observatory
... Supergiant: A supergiant star is the largest known type of star; some are almost as large as our entire solar system. Betelgeuse and Rigel are supergiants. These stars are rare. When supergiants die they explode as a supernova and may produce black holes. ...
... Supergiant: A supergiant star is the largest known type of star; some are almost as large as our entire solar system. Betelgeuse and Rigel are supergiants. These stars are rare. When supergiants die they explode as a supernova and may produce black holes. ...
The Sun: Example of Radiation Laws
... Low-mass stars (M < 8M⊙ ) evolve into a red giant phase in which their surfaces expand enormously and also cool, but their interiors shrink and heat. This occurs when the H fuel in the star’s core is depleted. A red giant burns He into C and O. When the He fuel is eventually exhausted, the outer ste ...
... Low-mass stars (M < 8M⊙ ) evolve into a red giant phase in which their surfaces expand enormously and also cool, but their interiors shrink and heat. This occurs when the H fuel in the star’s core is depleted. A red giant burns He into C and O. When the He fuel is eventually exhausted, the outer ste ...
charts_set_8
... light emitted just outside event horizon may appear red to distant observer. 3) Time dilation. Clock just outside event horizon appears to run slow to a ...
... light emitted just outside event horizon may appear red to distant observer. 3) Time dilation. Clock just outside event horizon appears to run slow to a ...
File
... Formation of the Elements • Stars’ processes are responsible for creating much of the world in which we live. • We currently know of 118 different elements. • The 81 stable elements found on Earth make up the bulk of matter in the universe. • 10 radioactive elements also occur naturally on our plan ...
... Formation of the Elements • Stars’ processes are responsible for creating much of the world in which we live. • We currently know of 118 different elements. • The 81 stable elements found on Earth make up the bulk of matter in the universe. • 10 radioactive elements also occur naturally on our plan ...
Powerpoint Presentation (large file)
... 1. What kinds of nuclear reactions occur within a star like the Sun as it ages? 2. Where did the carbon atoms in our bodies come from? 3. What is a planetary nebula, and what does it have to do ...
... 1. What kinds of nuclear reactions occur within a star like the Sun as it ages? 2. Where did the carbon atoms in our bodies come from? 3. What is a planetary nebula, and what does it have to do ...
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.