Nuclear Interactions in Supernovae .
... Chandrasekhar Limit • The white dwarf will continue to accrete mass, the pressure and density of the dwarf rises and the temperature increases from this increase in weight bearing down on the dead core. • Eventually (at around 1.38 solar masses) the temperature is increased so much, carbon starts f ...
... Chandrasekhar Limit • The white dwarf will continue to accrete mass, the pressure and density of the dwarf rises and the temperature increases from this increase in weight bearing down on the dead core. • Eventually (at around 1.38 solar masses) the temperature is increased so much, carbon starts f ...
14-1 Reading Questions: Neutron Stars
... density is so high that physicists calculate that this material is stable only as a ___________________________. Theory predicts that such an object would spin _____________ times per second, have a surface temperature nearly as hot as the ___________ interior, and possess a magnetic field a _______ ...
... density is so high that physicists calculate that this material is stable only as a ___________________________. Theory predicts that such an object would spin _____________ times per second, have a surface temperature nearly as hot as the ___________ interior, and possess a magnetic field a _______ ...
Nebula - NICADD
... • Any source of light in the night sky that was not a point was called a nebula. ...
... • Any source of light in the night sky that was not a point was called a nebula. ...
AST 301 Introduction to Astronomy
... To understand nuclear fusion, we need to know about the interactions between the particles in an atomic nucleus. We already know something about gravity and electrical forces. There are two more forces that matter. The strong, or nuclear, force is an attraction between the particles in a nucleus (pr ...
... To understand nuclear fusion, we need to know about the interactions between the particles in an atomic nucleus. We already know something about gravity and electrical forces. There are two more forces that matter. The strong, or nuclear, force is an attraction between the particles in a nucleus (pr ...
So why are more massive stars more luminous?
... A star becomes a red giant after the fusion of hydrogen into helium in its core has come to an end. As the red giant’s core shrinks and heats up, a new cycle of reactions can occur that create the even heavier elements carbon and oxygen. ...
... A star becomes a red giant after the fusion of hydrogen into helium in its core has come to an end. As the red giant’s core shrinks and heats up, a new cycle of reactions can occur that create the even heavier elements carbon and oxygen. ...
Lecture21 - UCSB Physics
... A star becomes a red giant after the fusion of hydrogen into helium in its core has come to an end. As the red giant’s core shrinks and heats up, a new cycle of reactions can occur that create the even heavier elements carbon and oxygen. ...
... A star becomes a red giant after the fusion of hydrogen into helium in its core has come to an end. As the red giant’s core shrinks and heats up, a new cycle of reactions can occur that create the even heavier elements carbon and oxygen. ...
Outline - March 16, 2010 Interstellar Medium (ISM) Why should you
... The energy is gravitational. Half the gravitational energy goes into heating the collapsing clout, the other half escapes as light. The central object is called a “protostar”, and they are very bright! (Because they have very large radii.) ...
... The energy is gravitational. Half the gravitational energy goes into heating the collapsing clout, the other half escapes as light. The central object is called a “protostar”, and they are very bright! (Because they have very large radii.) ...
Stellar Evolution
... the first distance determinations that worked out to distances beyond our Milky Way! Cepheids are up to ~ 40,000 times more luminous than our sun => can be identified in other galaxies. ...
... the first distance determinations that worked out to distances beyond our Milky Way! Cepheids are up to ~ 40,000 times more luminous than our sun => can be identified in other galaxies. ...
name - New York Science Teacher
... Continue to read on to the section: A Nuclear Fireplace about NUCLEAR FUSION in the Stars: Lights in the Sky paper. The picture there shows how stars take hydrogen and changes it to helium to make energy in the star. Your task is to design a 3-D model of this nuclear reaction with clay. Place these ...
... Continue to read on to the section: A Nuclear Fireplace about NUCLEAR FUSION in the Stars: Lights in the Sky paper. The picture there shows how stars take hydrogen and changes it to helium to make energy in the star. Your task is to design a 3-D model of this nuclear reaction with clay. Place these ...
Branches of Earth Science
... o Globular Cluster more common ______________ , densely packed stars 100,000 to 1,000,000 ______________ stars ...
... o Globular Cluster more common ______________ , densely packed stars 100,000 to 1,000,000 ______________ stars ...
Name
... 6. The brightest, hottest, and most massive stars are the brilliant blue stars designated as spectral class O. If a class O star with a mass of 3.38 X1031 kg has a kinetic energy of 1.10 X1042 J, what is its speed? Express your answer in km/s (a typical unit for describing the speed of stars). ...
... 6. The brightest, hottest, and most massive stars are the brilliant blue stars designated as spectral class O. If a class O star with a mass of 3.38 X1031 kg has a kinetic energy of 1.10 X1042 J, what is its speed? Express your answer in km/s (a typical unit for describing the speed of stars). ...
PH507 - University of Kent
... 3. Taking Deneb to have a surface temperature of 8,500K and a radius of 200 solar radii, determine the present spectral class and luminosity class of Deneb. Investigate and state the stages through which Deneb is expected to progress. State the name of the pre-main-sequence track that Deneb would ha ...
... 3. Taking Deneb to have a surface temperature of 8,500K and a radius of 200 solar radii, determine the present spectral class and luminosity class of Deneb. Investigate and state the stages through which Deneb is expected to progress. State the name of the pre-main-sequence track that Deneb would ha ...
The Life of a Star
... begins in the core (secondary fusion). Once all fusion reactions stop, the 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 bl ...
... begins in the core (secondary fusion). Once all fusion reactions stop, the 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 bl ...
Hertzsprung-Russell (H-R) Diagram Hertzsprung-Russell Diagram March 16 −
... Which is the hottest star? Which is the smallest star? Which is the biggest star? If stars A-D replaced the sun, would people be able to live in Michigan? a. b. c. d. e. ...
... Which is the hottest star? Which is the smallest star? Which is the biggest star? If stars A-D replaced the sun, would people be able to live in Michigan? a. b. c. d. e. ...
Locating Objects in Space
... Supernova: referred to as Type II supernova for paths 2 and 3 Black Hole: density so high that escape velocity of star becomes equal to the speed of light, so ...
... Supernova: referred to as Type II supernova for paths 2 and 3 Black Hole: density so high that escape velocity of star becomes equal to the speed of light, so ...
Study Guide
... Giant - helium is being fused into carbon and the star is now brighter but cooler Supernova - violent explosion of a massive star when the core collapses causing the outer layers to blow away main sequence star - as soon as fusion starts, the star is in this stage fusing hydrogen into helium Protost ...
... Giant - helium is being fused into carbon and the star is now brighter but cooler Supernova - violent explosion of a massive star when the core collapses causing the outer layers to blow away main sequence star - as soon as fusion starts, the star is in this stage fusing hydrogen into helium Protost ...
pps
... the local energy generation rate and the local density of the material This, in turn, is connected to the nuclear reactions occurring in that material. Before we can get to nuclear reaction physics, however, we require one more stellar structure equation. It is clear that the energy generation rate ...
... the local energy generation rate and the local density of the material This, in turn, is connected to the nuclear reactions occurring in that material. Before we can get to nuclear reaction physics, however, we require one more stellar structure equation. It is clear that the energy generation rate ...
Simon P. Balm Astronomy 5, Test #1, Sample Questions
... A) time it takes for light to travel from the nearest star to the Earth B) distance light travels in one year C) average distance between the Earth and the nearest star D) time it take light to travel from the Sun to the Earth ...
... A) time it takes for light to travel from the nearest star to the Earth B) distance light travels in one year C) average distance between the Earth and the nearest star D) time it take light to travel from the Sun to the Earth ...
Today`s Powerpoint
... For light, separate white light into its colors using a glass prism or "diffraction grating". For radiation in general, spread out the radiation by wavelength (e.g car radio, satellite TV receiver). How we know these things: - Physical states of stars, gas clouds, e.g. temperature, density, pressure ...
... For light, separate white light into its colors using a glass prism or "diffraction grating". For radiation in general, spread out the radiation by wavelength (e.g car radio, satellite TV receiver). How we know these things: - Physical states of stars, gas clouds, e.g. temperature, density, pressure ...
Homework 3 available
... c. (10 points) Only the central 10% of the mass of the Sun is close enough to the core, i.e., hot and dense enough, for thermonuclear fusion to take place. With this in mind (and remembering that only 75% of the mass of the Sun is hydrogen) calculate how long the Sun can shine with its current lumin ...
... c. (10 points) Only the central 10% of the mass of the Sun is close enough to the core, i.e., hot and dense enough, for thermonuclear fusion to take place. With this in mind (and remembering that only 75% of the mass of the Sun is hydrogen) calculate how long the Sun can shine with its current lumin ...
Lecture 10 - Concord University
... Fusing light elements together results in more nuclear binding energy and less mass per nucleon. When the mass disappears, it is converted to energy so light-element fusion produces energy. But, when fusing any element to Fe, you now need to PROVIDE some energy to be converted into mass and Natu ...
... Fusing light elements together results in more nuclear binding energy and less mass per nucleon. When the mass disappears, it is converted to energy so light-element fusion produces energy. But, when fusing any element to Fe, you now need to PROVIDE some energy to be converted into mass and Natu ...