ppt - Astronomy & Physics
... Many stars (depends on their mass) end up here after they leave the main-sequence Their temperatures are not that high (2000— 6000K) but they are very luminous by Stefan-Boltzmann law they must be very large (big surface area) Outer parts of the Sun’s atmosphere will engulf Earth and Mars when it ...
... Many stars (depends on their mass) end up here after they leave the main-sequence Their temperatures are not that high (2000— 6000K) but they are very luminous by Stefan-Boltzmann law they must be very large (big surface area) Outer parts of the Sun’s atmosphere will engulf Earth and Mars when it ...
Sample Exam 2
... 10. Late in its evolution, the Sun will become a white dwarf with a radius about 100 times smaller than its current radius. The volume of the Sun today is approximately ______ times larger than its future volume. A. 100 B. 103 C. 104 D. 106 E. 108 11. What kind of celestial observation would be best ...
... 10. Late in its evolution, the Sun will become a white dwarf with a radius about 100 times smaller than its current radius. The volume of the Sun today is approximately ______ times larger than its future volume. A. 100 B. 103 C. 104 D. 106 E. 108 11. What kind of celestial observation would be best ...
Homologous Stellar Models and Polytropes Main Sequence Stars
... Main Sequence Star Characteristics – III • Main sequence star interiors are extremely hot (T > 106 K) and the fall-off to surface temperatures (T ∼ 104 K) takes place in a very thin region near the surface. • Nuclear energy generation is restricted to a very small M (r) near the centre of the star. ...
... Main Sequence Star Characteristics – III • Main sequence star interiors are extremely hot (T > 106 K) and the fall-off to surface temperatures (T ∼ 104 K) takes place in a very thin region near the surface. • Nuclear energy generation is restricted to a very small M (r) near the centre of the star. ...
PHYS 2410 General Astronomy Homework 7
... The energy emitted from the surface of a main sequence star is _____the energy generated in the core. a. ...
... The energy emitted from the surface of a main sequence star is _____the energy generated in the core. a. ...
PHYXXXX UNIVERSITY OF EXETER PHYSICS XXX/YYY 20XX
... Explain why a molecular cloud collapsing under gravity heats up. Unless this heat is removed, the pressure will increase to a point where collapse is no longer possible and a star will not form. Explain how heat is removed during the early phases of star formation. Explain why this no longer works w ...
... Explain why a molecular cloud collapsing under gravity heats up. Unless this heat is removed, the pressure will increase to a point where collapse is no longer possible and a star will not form. Explain how heat is removed during the early phases of star formation. Explain why this no longer works w ...
Integrative Studies 410 Our Place in the Universe
... Describe how variable stars, e.g. Cepheids, can be used as cosmic yardsticks • k: Cepheid stars oscillate between two states: In one of the states, the star is compact and large temperature and pressure gradients build up in the star. These large pressures cause the star to expand. When the star is ...
... Describe how variable stars, e.g. Cepheids, can be used as cosmic yardsticks • k: Cepheid stars oscillate between two states: In one of the states, the star is compact and large temperature and pressure gradients build up in the star. These large pressures cause the star to expand. When the star is ...
l max T = 0.002897755 m K
... 2) Which would look brighter, a star with m=10 or a star that has M=10 and is at 20 pc? Answer: m=10 Explain: A M=10 star would have m=10 at 10pc and be fainter than m=10 at 20pc ...
... 2) Which would look brighter, a star with m=10 or a star that has M=10 and is at 20 pc? Answer: m=10 Explain: A M=10 star would have m=10 at 10pc and be fainter than m=10 at 20pc ...
Stellar Evolution – Life of a Star
... • He is now the fuel source, but the temperature and energy needed to ignite He fusion is greater than H. Thus, the energy released by He fusion in the core is greater than needed to support the weight of the outer layer. The excess energy expands the outer layers beyond its previous radius and star ...
... • He is now the fuel source, but the temperature and energy needed to ignite He fusion is greater than H. Thus, the energy released by He fusion in the core is greater than needed to support the weight of the outer layer. The excess energy expands the outer layers beyond its previous radius and star ...
SNC1 Practice Astronomy Exam 1) If something were to happen to
... b) Measure the angles from a very short baseline (of known length) to the object at each end of the baseline. c) Measure the angle from a baseline to the object at one end of the baseline and the length of the baseline. b) Measure the angles from a very long baseline (of known length) to the object ...
... b) Measure the angles from a very short baseline (of known length) to the object at each end of the baseline. c) Measure the angle from a baseline to the object at one end of the baseline and the length of the baseline. b) Measure the angles from a very long baseline (of known length) to the object ...
Quiz 3 Feedback Electron Jumps in Atoms Emission and absorption
... (continuous) spectrum. If there are emission lines, those come from low-density hotter gas above the surface. “You get temperature from the mass.” •The mass of a star tells you where it will be on the Main Sequence, hence its luminosity and temperature. But this works only for Main Sequence stars, a ...
... (continuous) spectrum. If there are emission lines, those come from low-density hotter gas above the surface. “You get temperature from the mass.” •The mass of a star tells you where it will be on the Main Sequence, hence its luminosity and temperature. But this works only for Main Sequence stars, a ...
Star Systems and Galaxies
... Star systems that have two stars are called double stars or binary stars Those with three stars are called triple stars Often one star in a binary star is much brighter and more massive than the ...
... Star systems that have two stars are called double stars or binary stars Those with three stars are called triple stars Often one star in a binary star is much brighter and more massive than the ...
The Life Cycles of Stars MEDIUM STARS MASSIVE STARS
... A star's life cycle is determined by its mass. The larger the mass, the shorter the life cycle. A star's mass is determined by the amount of matter that is available in its nebula, the giant cloud of gas and dust in which it is born. Over time, gravity pulls the hydrogen gas in the nebula together a ...
... A star's life cycle is determined by its mass. The larger the mass, the shorter the life cycle. A star's mass is determined by the amount of matter that is available in its nebula, the giant cloud of gas and dust in which it is born. Over time, gravity pulls the hydrogen gas in the nebula together a ...
H R Diagram Online Activity
... 2. “The position of each dot on the diagram tells us two things about each star: its _____________________ (or absolute magnitude) and its _____________________________” 3. “The vertical axis represents the star’s ________________________ or absolute magnitude. Luminosity is technically the amount o ...
... 2. “The position of each dot on the diagram tells us two things about each star: its _____________________ (or absolute magnitude) and its _____________________________” 3. “The vertical axis represents the star’s ________________________ or absolute magnitude. Luminosity is technically the amount o ...
Astronomy 15 - Homework 3 - Due Wed. April 24 1) As we`ll see
... Teff is called the ‘effective temperature’ – it’s the temperature of a blackbody which emits the same power per unit area as the star. Different levels in a star’s atmosphere have different temperatures, and the effective temperature is a useful average of these. We can learn a lot from this simple ...
... Teff is called the ‘effective temperature’ – it’s the temperature of a blackbody which emits the same power per unit area as the star. Different levels in a star’s atmosphere have different temperatures, and the effective temperature is a useful average of these. We can learn a lot from this simple ...
Lecture 13 Hydrogen Burning on the Main Sequence and Homology
... is specified, R is undetermined, though L may be. 3. Stars will get hotter in their centers when they use up a given fuel – unless they become degenerate 4. More massive stars will arrive at a given temperature (e.g. ignition) at a lower central density ...
... is specified, R is undetermined, though L may be. 3. Stars will get hotter in their centers when they use up a given fuel – unless they become degenerate 4. More massive stars will arrive at a given temperature (e.g. ignition) at a lower central density ...
Stellar Evolution
... • As the helium core grows, it compresses. Helium doesn’t fuse to heavier elements for two reasons. (1) with 2 p+ per nucleus, the electric repulsion force is higher than was the case for H-fusion. This means that helium fusion requires a higher temperature than hydrogen fusion -- 100 million K (2) ...
... • As the helium core grows, it compresses. Helium doesn’t fuse to heavier elements for two reasons. (1) with 2 p+ per nucleus, the electric repulsion force is higher than was the case for H-fusion. This means that helium fusion requires a higher temperature than hydrogen fusion -- 100 million K (2) ...
How Bright is that star?
... The luminosity/meter² (l), is determined by the temperature (T) of that area ) l = σT⁴ (σ is a constant which if T is in °K, “l “ comes out in Watts) Surface area is determined by radius(R): A = 4πR² So the total Luminosity of star becomes L = 4πR²σT⁴ Thus luminosity depends entirely on Radius and t ...
... The luminosity/meter² (l), is determined by the temperature (T) of that area ) l = σT⁴ (σ is a constant which if T is in °K, “l “ comes out in Watts) Surface area is determined by radius(R): A = 4πR² So the total Luminosity of star becomes L = 4πR²σT⁴ Thus luminosity depends entirely on Radius and t ...
Red giants aren`t just big, they`re turbulent
... Since astronomers can neither zoom in on more distant stars nor peek under the cover of even the nearest one, how do they learn what drives these stellar furnaces? If they are Paul Woodward and David Porter, they create their own. These astrophysicists, nearly as well known for setting computing rec ...
... Since astronomers can neither zoom in on more distant stars nor peek under the cover of even the nearest one, how do they learn what drives these stellar furnaces? If they are Paul Woodward and David Porter, they create their own. These astrophysicists, nearly as well known for setting computing rec ...
A105 Stars and Galaxies
... During hydrogen burning, basic physics forces a star to lie on the main sequence. A star’s position on the MS depends on its mass. ...
... During hydrogen burning, basic physics forces a star to lie on the main sequence. A star’s position on the MS depends on its mass. ...
Can`t tell –depends on how much hotter the small one is relative to
... Imagine you are comparing the abilities of electric hot plates of different sizes and temperatures to cook fully two identical large pots of spaghetti. Note that the pots are all as large as the largest hot plate. When a hot plate is at one of the temperature settings (low, med, high), the hot plate ...
... Imagine you are comparing the abilities of electric hot plates of different sizes and temperatures to cook fully two identical large pots of spaghetti. Note that the pots are all as large as the largest hot plate. When a hot plate is at one of the temperature settings (low, med, high), the hot plate ...
9.1 Introduction 9.2 Static Models
... by replacing the differential equations with difference equations and approximating the internal structure of a star by a series of concentric shells separated by a small, but finite, radial distance δr. For example, if the pressure in shell i is Pi , the pressure in the next shell is Pi+1 = Pi +(∆P ...
... by replacing the differential equations with difference equations and approximating the internal structure of a star by a series of concentric shells separated by a small, but finite, radial distance δr. For example, if the pressure in shell i is Pi , the pressure in the next shell is Pi+1 = Pi +(∆P ...
Chapter 19 Star Formation
... Star formation happens when part of a dust cloud begins to contract under its own gravitational force; as it collapses, the center becomes hotter and hotter until nuclear fusion begins in the core. ...
... Star formation happens when part of a dust cloud begins to contract under its own gravitational force; as it collapses, the center becomes hotter and hotter until nuclear fusion begins in the core. ...
Chapter11
... 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: ...