Star luminosity info and HR diagram
... intrinsic brightness, how bright it really is. A star’s apparent magnitude – its brightness as it appears from Earth – is something different and depends on how far away we are from that star. ...
... intrinsic brightness, how bright it really is. A star’s apparent magnitude – its brightness as it appears from Earth – is something different and depends on how far away we are from that star. ...
RED DWARFS AND THE END OF THE MAIN SEQUENCE
... temperature cannot increase because of the sharply increasing opacity with increasing temperature, i.e., the photosphere encounters an opacity wall. As a result, the photospheric temperature remains (nearly) constant and the star ascends the red giant branch. For stars with photospheres that do not ...
... temperature cannot increase because of the sharply increasing opacity with increasing temperature, i.e., the photosphere encounters an opacity wall. As a result, the photospheric temperature remains (nearly) constant and the star ascends the red giant branch. For stars with photospheres that do not ...
AY 12 Homework #4 Solutions Winter 2016 Longer Problems 1. a
... c) Binary stellar massed x-ray sources are thought to be the result of a neutron star or black hole accreting mass from a companion star. If the x-ray emitting source can be shown to have a mass greater than 2 M , it must be a black hole, because there are no existing neutron stars above 2 M . 4. ...
... c) Binary stellar massed x-ray sources are thought to be the result of a neutron star or black hole accreting mass from a companion star. If the x-ray emitting source can be shown to have a mass greater than 2 M , it must be a black hole, because there are no existing neutron stars above 2 M . 4. ...
Spectral-Type Trends: Absorption
... the Chandra archive, arranged in order of decreasing surface temperature and mass-loss rate. As is evident from the data, the more luminous stars have stronger emission at short wavelengths. One possible explanation for this trend is that we are seeing the effects of absorption on the spectra. Since ...
... the Chandra archive, arranged in order of decreasing surface temperature and mass-loss rate. As is evident from the data, the more luminous stars have stronger emission at short wavelengths. One possible explanation for this trend is that we are seeing the effects of absorption on the spectra. Since ...
LIFE CYCLE OF A STAR
... NO LONGER CAN GENERATE __________ by fusing hydrogen atoms into _____ atoms. Can shine for _____________of years even after they die. ...
... NO LONGER CAN GENERATE __________ by fusing hydrogen atoms into _____ atoms. Can shine for _____________of years even after they die. ...
AST1100 Lecture Notes
... stars range from 0.08M⊙ for the least massive stars up to about 100M⊙ for the most massive stars. We will later discuss theoretical arguments explaining why there is a lower and an upper limit of star masses. We will now start to look at the evolution of stars, from birth to death. Stars start out a ...
... stars range from 0.08M⊙ for the least massive stars up to about 100M⊙ for the most massive stars. We will later discuss theoretical arguments explaining why there is a lower and an upper limit of star masses. We will now start to look at the evolution of stars, from birth to death. Stars start out a ...
Dead Stars They do exist! The white dwarf stars
... • Appendix 12 (nearest stars) lists 2 of them, so they must be very common ...
... • Appendix 12 (nearest stars) lists 2 of them, so they must be very common ...
Lecture 1
... 1. Equation of state (EOS) determines the pressure of the matter, P. 2. The neutron star matter is so dense that P is almost independent of the temperature T and is determined by the mass density and the composition of the matter; one usually writes P P( ). 3. The mass density is defined as ...
... 1. Equation of state (EOS) determines the pressure of the matter, P. 2. The neutron star matter is so dense that P is almost independent of the temperature T and is determined by the mass density and the composition of the matter; one usually writes P P( ). 3. The mass density is defined as ...
Stars & Galaxies
... © 2006, TESCCC The content of this multimedia presentation is intended for use by TESCCC subscribers for intra-district professional development ONLY; and may not be used for other purposes, in whole or part, without the expressed written permission of their ESC-TESCCC coordinator for the region han ...
... © 2006, TESCCC The content of this multimedia presentation is intended for use by TESCCC subscribers for intra-district professional development ONLY; and may not be used for other purposes, in whole or part, without the expressed written permission of their ESC-TESCCC coordinator for the region han ...
Geochemistry & Lab
... ▪ A star system = Star(s) + planets + satellites + meteorites + asteroids + comets +others ▪ Star + star + .. Galaxy < Galaxy group < Universe A star may be the elementary constituent of ...
... ▪ A star system = Star(s) + planets + satellites + meteorites + asteroids + comets +others ▪ Star + star + .. Galaxy < Galaxy group < Universe A star may be the elementary constituent of ...
astr study guide ex 3 s`16
... 2. Why don't we see hydrogen Balmer lines in the spectra of very cool stars? (like 3,000 K ...
... 2. Why don't we see hydrogen Balmer lines in the spectra of very cool stars? (like 3,000 K ...
Similarities Between Electric and Gravitational Forces • Coulomb’s force: q F
... • Distances calculated durectly (“trigonometric parallax”) • Giants, main-sequence and white dwarfs ...
... • Distances calculated durectly (“trigonometric parallax”) • Giants, main-sequence and white dwarfs ...
Stefan-Boltzmann Law
... temperature? (This is meant to be obvious.) Which lettered example(s) above supports your answer? 4. If you use two hot plates of different sizes, can you assume that the one that boils water first is at a higher temperature? Which lettered example(s) above supports your answer? 5. Two students are ...
... temperature? (This is meant to be obvious.) Which lettered example(s) above supports your answer? 4. If you use two hot plates of different sizes, can you assume that the one that boils water first is at a higher temperature? Which lettered example(s) above supports your answer? 5. Two students are ...
2008 - UCL
... name the corresponding carrier particle for each of them, as well as the particles they act upon. ...
... name the corresponding carrier particle for each of them, as well as the particles they act upon. ...
Star Factories: Nuclear Fusion and the Creation of the Elements
... elements up to and including iron in their cores. But iron is the heaviest element they can make. Fusion of iron does not create energy, and without an energy supply, the star will soon die. ...
... elements up to and including iron in their cores. But iron is the heaviest element they can make. Fusion of iron does not create energy, and without an energy supply, the star will soon die. ...
Star Life Cycle Web Activity
... II. Go to http://sunshine.chpc.utah.edu/labs/star_life/starlife_main.html This page will give more details on each of these stages. Read the content of this first page. 1) Using the human life cycle analogy, what star phase is the birth of a star and what is the usual end stage (death) of the star? ...
... II. Go to http://sunshine.chpc.utah.edu/labs/star_life/starlife_main.html This page will give more details on each of these stages. Read the content of this first page. 1) Using the human life cycle analogy, what star phase is the birth of a star and what is the usual end stage (death) of the star? ...
giant molecular clouds
... Energy generated in the star’s center must be transported to the surface. Inner layers: ...
... Energy generated in the star’s center must be transported to the surface. Inner layers: ...
ph507lecnote06
... Most stars have properties within the shaded region known as the main sequence. The points plotted here are for stars lying within about 5 pc of the Sun. The diagonal lines correspond to constant stellar radius, so that stellar size can be represented on the same diagram as luminosity and temperatur ...
... Most stars have properties within the shaded region known as the main sequence. The points plotted here are for stars lying within about 5 pc of the Sun. The diagonal lines correspond to constant stellar radius, so that stellar size can be represented on the same diagram as luminosity and temperatur ...
The Formation of Stars Chapter 11 Guidepost Guidepost
... forming stars exposed by the ionizing radiation from nearby massive stars ...
... forming stars exposed by the ionizing radiation from nearby massive stars ...
Student Exploration Sheet: Growing Plants
... 5. Predict: Consider any relationships you see between a star’s luminosity, radius, and mass. A. As the radius of a star increases, how do you think its luminosity might change? ___________________________________________________________________ B. As the mass of a star increases, how do you think i ...
... 5. Predict: Consider any relationships you see between a star’s luminosity, radius, and mass. A. As the radius of a star increases, how do you think its luminosity might change? ___________________________________________________________________ B. As the mass of a star increases, how do you think i ...
Solutions to test #2 taken on Monday
... 2. (13) Millions, Billions or One. This is an “order of magnitude” question. Pick the number (the order of magnitude) that is closest for each. a) ___one_____ Average distance (in parsecs) between stars. b) ____billions____ Current age of the Sun in years. c) ___millions_____ Length of time a star l ...
... 2. (13) Millions, Billions or One. This is an “order of magnitude” question. Pick the number (the order of magnitude) that is closest for each. a) ___one_____ Average distance (in parsecs) between stars. b) ____billions____ Current age of the Sun in years. c) ___millions_____ Length of time a star l ...
Stellar Evolution (Formation)
... Sun has enough H in its core to produce energy for about 1010 yrs. (It is about halfway through its life now.) When the core’s H is exhausted, there will be no more nuclear energy to heat the gas. Gravity will win over gas pressure and the core will collapse. Gravitational potential energy of th ...
... Sun has enough H in its core to produce energy for about 1010 yrs. (It is about halfway through its life now.) When the core’s H is exhausted, there will be no more nuclear energy to heat the gas. Gravity will win over gas pressure and the core will collapse. Gravitational potential energy of th ...
H-RDiagramSE
... diagram and become giants or supergiants. Giants and supergiants form when the center of a star collapses and its outer parts expand outwards. What are the characteristics of giants and supergiants? _____________________________ ...
... diagram and become giants or supergiants. Giants and supergiants form when the center of a star collapses and its outer parts expand outwards. What are the characteristics of giants and supergiants? _____________________________ ...
evolution of low
... . central temperature determined by characteristic nuclear-burning temperature (hydrogen fusion: Tc ∼ 107 K; helium fusion: Tc ∼ 108 K) . from (3) ⇒ R ∝ M (in reality R ∝ M0.6−0.8 ) ...
... . central temperature determined by characteristic nuclear-burning temperature (hydrogen fusion: Tc ∼ 107 K; helium fusion: Tc ∼ 108 K) . from (3) ⇒ R ∝ M (in reality R ∝ M0.6−0.8 ) ...