Lecture 7
... Once H in core virtually exhausted, core contracts due to drop in pressure, H burns in shell around He core. Burnt material (He) added to core, density increases. Eventually core becomes so dense contracts and heats up energy generation in shell accelerates, outer envelope expands, surface tempera ...
... Once H in core virtually exhausted, core contracts due to drop in pressure, H burns in shell around He core. Burnt material (He) added to core, density increases. Eventually core becomes so dense contracts and heats up energy generation in shell accelerates, outer envelope expands, surface tempera ...
The Sun and the Stars
... Once H in core virtually exhausted, core contracts due to drop in pressure, H burns in shell around He core. Burnt material (He) added to core, density increases. Eventually core becomes so dense contracts and heats up energy generation in shell accelerates, outer envelope expands, surface tempera ...
... Once H in core virtually exhausted, core contracts due to drop in pressure, H burns in shell around He core. Burnt material (He) added to core, density increases. Eventually core becomes so dense contracts and heats up energy generation in shell accelerates, outer envelope expands, surface tempera ...
Chapter 13 (Properties of Stars)
... A. Luminosity/brightness. B. Color/luminosity. C. Wavelength/temperature increasing to the right. D. Wavelength/temperature decreasing to the right. 15. Refer to the H-R diagram: for stars in general, a higher mass star may be found: A. at higher luminosity and lower temperature. B. at higher lumino ...
... A. Luminosity/brightness. B. Color/luminosity. C. Wavelength/temperature increasing to the right. D. Wavelength/temperature decreasing to the right. 15. Refer to the H-R diagram: for stars in general, a higher mass star may be found: A. at higher luminosity and lower temperature. B. at higher lumino ...
Student Paper (Klongcheongsan)
... fraction (X), helium (Y), and metal mass fraction (Z) in one or more zones of the star. Once the central values of temperature and mass density are picked, the program calculates the change in all physical variables for the next mass shell. These are then added to the previous values in an iterative ...
... fraction (X), helium (Y), and metal mass fraction (Z) in one or more zones of the star. Once the central values of temperature and mass density are picked, the program calculates the change in all physical variables for the next mass shell. These are then added to the previous values in an iterative ...
neutron star.
... The White Dwarf Limit • Quantum mechanics says that electrons must move faster as they are squeezed into a very small space. • As a white dwarf’s mass approaches 1.4MSun, its electrons must move at nearly the speed of light. • Because nothing can move faster than light, a white dwarf cannot be more ...
... The White Dwarf Limit • Quantum mechanics says that electrons must move faster as they are squeezed into a very small space. • As a white dwarf’s mass approaches 1.4MSun, its electrons must move at nearly the speed of light. • Because nothing can move faster than light, a white dwarf cannot be more ...
Lecture 12
... requires measuring the entire EM spectrum of a source, which is impossible with a single type detector. • Bolometric fluxes have to be inferred by knowledge of the physics producing the luminous source for which you have partial information, or pieced together from observations at all parts of the E ...
... requires measuring the entire EM spectrum of a source, which is impossible with a single type detector. • Bolometric fluxes have to be inferred by knowledge of the physics producing the luminous source for which you have partial information, or pieced together from observations at all parts of the E ...
ON STARS, THEIR EVOLUTION AND THEIR STABILITY
... The paradox posed by Eddington was reformulated in clearer physical terms by R. H. Fowler.4 His formulation was the following: The stellar material, in the white-dwarf state, will have radiated so much energy that it has less energy than the same matter in normal atoms expanded at the absolute zero ...
... The paradox posed by Eddington was reformulated in clearer physical terms by R. H. Fowler.4 His formulation was the following: The stellar material, in the white-dwarf state, will have radiated so much energy that it has less energy than the same matter in normal atoms expanded at the absolute zero ...
Read the information on Hertzsprung
... radiates in one second, but you can think of it as how bright or how dim the star appears. The luminosity scale is a "ratio scale" in which stars are compared to each other based upon a reference (our sun). The horizontal axis represents the star’s surface temperature (not the star’s core temperatur ...
... radiates in one second, but you can think of it as how bright or how dim the star appears. The luminosity scale is a "ratio scale" in which stars are compared to each other based upon a reference (our sun). The horizontal axis represents the star’s surface temperature (not the star’s core temperatur ...
CHP 13
... 1. The lowest-mass stars cannot become giants because a. they do not contain helium. b. they rotate too slowly. c. they cannot heat their centers hot enough. d. they contain strong magnetic fields. e. they never use up their hydrogen. 2. A planetary nebula is a. the expelled outer envelope of a medi ...
... 1. The lowest-mass stars cannot become giants because a. they do not contain helium. b. they rotate too slowly. c. they cannot heat their centers hot enough. d. they contain strong magnetic fields. e. they never use up their hydrogen. 2. A planetary nebula is a. the expelled outer envelope of a medi ...
The Death of Stars
... 1. The lowest-mass stars cannot become giants because a. they do not contain helium. b. they rotate too slowly. c. they cannot heat their centers hot enough. d. they contain strong magnetic fields. e. they never use up their hydrogen. 2. A planetary nebula is a. the expelled outer envelope of a medi ...
... 1. The lowest-mass stars cannot become giants because a. they do not contain helium. b. they rotate too slowly. c. they cannot heat their centers hot enough. d. they contain strong magnetic fields. e. they never use up their hydrogen. 2. A planetary nebula is a. the expelled outer envelope of a medi ...
All_Stars
... • Medium-mass stars burn H He in their cores while on the main sequence and He C and O while on the horizontal branch • They are not massive enough to ignite C-burning once their He is gone. Their cores contract and heat up until the contraction is stopped by electron degeneracy pressure • At th ...
... • Medium-mass stars burn H He in their cores while on the main sequence and He C and O while on the horizontal branch • They are not massive enough to ignite C-burning once their He is gone. Their cores contract and heat up until the contraction is stopped by electron degeneracy pressure • At th ...
Canis Majoris
... Canis Majoris is the largest star that has so far been discovered. When viewed from earth it’s very tiny, which means it has a very small apparent magnitude. Canis Majoris is so large that you could fit about seven quadrillion earths inside of it. To put this into perspective, if earth were the size ...
... Canis Majoris is the largest star that has so far been discovered. When viewed from earth it’s very tiny, which means it has a very small apparent magnitude. Canis Majoris is so large that you could fit about seven quadrillion earths inside of it. To put this into perspective, if earth were the size ...
Stellar Winds and Mass Loss
... on the order of 10-6M/yr Most notable is Hα Also, Paschen and Brackett lines of He II Wolf-Rayet stars are dominated by lines that form in high density winds ...
... on the order of 10-6M/yr Most notable is Hα Also, Paschen and Brackett lines of He II Wolf-Rayet stars are dominated by lines that form in high density winds ...
parallax
... The measurements that you made above are quite similar to those made by astronomers in order to measure the distances to nearby stars. The big difference is that even the nearest stars are quite far away compared to the diameter of the Earth’s orbit around the Sun. Because the stars are so far away, ...
... The measurements that you made above are quite similar to those made by astronomers in order to measure the distances to nearby stars. The big difference is that even the nearest stars are quite far away compared to the diameter of the Earth’s orbit around the Sun. Because the stars are so far away, ...
Project 3. Colour in Astronomy
... M50, but most of the dimmer, red stars do not. M50 lies about 3000 light‐years from Earth and is about 20 light years across. Magnitude is a number that measures the brightness of a star or galaxy. In magnitude, higher numbers correspond to fainter objects, lower numbers to ...
... M50, but most of the dimmer, red stars do not. M50 lies about 3000 light‐years from Earth and is about 20 light years across. Magnitude is a number that measures the brightness of a star or galaxy. In magnitude, higher numbers correspond to fainter objects, lower numbers to ...
