More stellar evolution…bloated stars and compact cores
... swell up and cool --> red giant (not obvious) ...
... swell up and cool --> red giant (not obvious) ...
Lifetimes of stars
... • The Sun has a main-sequence lifetime of 10 billion years. What about the other stars? (1) The fuel for stars is mass (2) The fuel consumption rate is ...
... • The Sun has a main-sequence lifetime of 10 billion years. What about the other stars? (1) The fuel for stars is mass (2) The fuel consumption rate is ...
Day-6
... The protostar’s energy source is gravitational energy. Temperature rises in the core. Hydrogen fusion begins in the core, and the star begins its life on the main sequence. Very low-mass stars (< 0.08 M) never start hydrogen fusion. These are called brown dwarfs. ...
... The protostar’s energy source is gravitational energy. Temperature rises in the core. Hydrogen fusion begins in the core, and the star begins its life on the main sequence. Very low-mass stars (< 0.08 M) never start hydrogen fusion. These are called brown dwarfs. ...
AnwerkeyTypes-of-stars-and-HR-diagram
... White dwarf compares to red giants? __________________Higher______ 3. What is color of stars with highest Surface Temperature? ____________blue____________ 4. What is color of stars with lowest Surface Temperature? _______________Red_________ 5. List the colors from hottest to Coldest: __Blue, white ...
... White dwarf compares to red giants? __________________Higher______ 3. What is color of stars with highest Surface Temperature? ____________blue____________ 4. What is color of stars with lowest Surface Temperature? _______________Red_________ 5. List the colors from hottest to Coldest: __Blue, white ...
Stars from Afar
... Brightness/Magnitude – The amount of light a star gives off depends on its size and temperature. ...
... Brightness/Magnitude – The amount of light a star gives off depends on its size and temperature. ...
ph607-15-test2ans
... Where, or whether, such layers occur in a particular star depends on the mass of the star, as shown in the figure. (c) m/M is the the fraction of mass, m(r), within r ( as a logarithmic function of stellar mass, M). (d) In stars with masses below about 1.3M, the surface layers are cool enough to be ...
... Where, or whether, such layers occur in a particular star depends on the mass of the star, as shown in the figure. (c) m/M is the the fraction of mass, m(r), within r ( as a logarithmic function of stellar mass, M). (d) In stars with masses below about 1.3M, the surface layers are cool enough to be ...
Stellar life after the Main Sequence (cont.)
... As cores contract, the density goes to “astronomical” levels, matter acts in funny ways • Gas in this room, the “perfect gas law” PV=nRT. Pressure depends on both density and temperature • Extremely dense, “degenerate” gas PV=Kn. Pressure depends only on density • Demo ...
... As cores contract, the density goes to “astronomical” levels, matter acts in funny ways • Gas in this room, the “perfect gas law” PV=nRT. Pressure depends on both density and temperature • Extremely dense, “degenerate” gas PV=Kn. Pressure depends only on density • Demo ...
Stars after the Main Sequence. Example: Betelgeuse (Alpha Orionis
... These compact cores exist….the white dwarf stars ...
... These compact cores exist….the white dwarf stars ...
Friday, November 7 - Otterbein University
... • Density and temperature increase towards center • Very hot & dense core produces all the energy by hydrogen nuclear fusion • Energy is released in the form of EM radiation and particles (neutrinos) • Energy transport well understood in physics ...
... • Density and temperature increase towards center • Very hot & dense core produces all the energy by hydrogen nuclear fusion • Energy is released in the form of EM radiation and particles (neutrinos) • Energy transport well understood in physics ...
Introduction to Astronomy
... Cecilia Payne at Harvard, 1924 In the sun, only one H atom in a million is in level 2, ready to absorb visible light! ...
... Cecilia Payne at Harvard, 1924 In the sun, only one H atom in a million is in level 2, ready to absorb visible light! ...
protostars and pre-main-sequence evolution.key
... iterate until match with outer boundary conditions. ...
... iterate until match with outer boundary conditions. ...
The Hertzsprung – Russell Diagram Star Data Table
... Danish astronomer Ejnar Hertzsprung and American astronomer Henry Russell discovered a relationship between the brightness of a star and the surface temperature of a star. The graph of a star’s absolute magnitude versus its temperature is called an ...
... Danish astronomer Ejnar Hertzsprung and American astronomer Henry Russell discovered a relationship between the brightness of a star and the surface temperature of a star. The graph of a star’s absolute magnitude versus its temperature is called an ...
Astronomy Galaxies & The Universe
... Life Cycle of Stars Average to small stars collapse again after C fuel is used up → white dwarf (Earth size) Large stars (at least 7 times our sun) when fusion (of carbon) stops, a central iron core is left, intense gravitational energy causes further collapse, creates heavier elements → explosion ...
... Life Cycle of Stars Average to small stars collapse again after C fuel is used up → white dwarf (Earth size) Large stars (at least 7 times our sun) when fusion (of carbon) stops, a central iron core is left, intense gravitational energy causes further collapse, creates heavier elements → explosion ...
The Mass-Radius Relation for Polytropes The mass within any point
... −ξ n+1 MT1−n Rn−3 K −n = 4π dξ ξ1 G ...
... −ξ n+1 MT1−n Rn−3 K −n = 4π dξ ξ1 G ...
Worksheet: Stars and the HR Diagram
... Background: The Hertzsprung-Russell diagram is actually a graph that illustrates the relationship that exists between the average surface temperature of stars and their absolute magnitude, which is how bright they would appear to be if they were al the same distance away. Rather than speak of the br ...
... Background: The Hertzsprung-Russell diagram is actually a graph that illustrates the relationship that exists between the average surface temperature of stars and their absolute magnitude, which is how bright they would appear to be if they were al the same distance away. Rather than speak of the br ...
ASTR2050 Spring 2005 • In this class we will cover: Brief review
... Greek letter (in order of brightness) then constellation e.g. α-Orionis is brightest star in Orion (aka Betelgeuse) δ-Cephei is fourth brightest star in Cepheus Variable stars Listed in order of discovery, starting with “R”, then “S” and on through “Z”, then “RR..RZ...SS...SZ...ZZ”, and then “AA...A ...
... Greek letter (in order of brightness) then constellation e.g. α-Orionis is brightest star in Orion (aka Betelgeuse) δ-Cephei is fourth brightest star in Cepheus Variable stars Listed in order of discovery, starting with “R”, then “S” and on through “Z”, then “RR..RZ...SS...SZ...ZZ”, and then “AA...A ...
08 October: Stellar life after the Main Sequence
... When you look at a Main Sequence star, the appearance of it exterior tells you what it is like inside ...
... When you look at a Main Sequence star, the appearance of it exterior tells you what it is like inside ...
The Fates of Stars Mass-Luminosity Relation: Lifetime Relation:
... be perfectly accurate; just show the general trend.) Remember that the temp. axis goes backwards. 2. Calculate the mass and total lifetime of one of these stars and fill this entries in the table. Make sure to translate the lifetime to years. (You may do the other stars if you have extra time.) 3. U ...
... be perfectly accurate; just show the general trend.) Remember that the temp. axis goes backwards. 2. Calculate the mass and total lifetime of one of these stars and fill this entries in the table. Make sure to translate the lifetime to years. (You may do the other stars if you have extra time.) 3. U ...
source
... be perfectly accurate; just show the general trend.) Remember that the temp. axis goes backwards. 2. Calculate the mass and total lifetime of one of these stars and fill this entries in the table. Make sure to translate the lifetime to years. (You may do the other stars if you have extra time.) 3. U ...
... be perfectly accurate; just show the general trend.) Remember that the temp. axis goes backwards. 2. Calculate the mass and total lifetime of one of these stars and fill this entries in the table. Make sure to translate the lifetime to years. (You may do the other stars if you have extra time.) 3. U ...
H-R diagram worksheet
... Mark each of the following on the H-R diagram and label it as indicated. You may use page 15 of your ESRT to help you. 6. Draw and label a long diagonal line showing the approximate location of the main sequence. 7. A large circle indicating the area where you find the biggest diameter stars, labele ...
... Mark each of the following on the H-R diagram and label it as indicated. You may use page 15 of your ESRT to help you. 6. Draw and label a long diagonal line showing the approximate location of the main sequence. 7. A large circle indicating the area where you find the biggest diameter stars, labele ...
PS #1 Solutions - Stars and Stellar Explosions 1. Opacity sources
... to Thompson scattering. We will carry out many related estimates during this course so it is important to become familiar with this process. Consider a star in hydrostatic equilibrium in which energy transport is by radiative diffusion. The star is composed of ionized hydrogen and is supported prima ...
... to Thompson scattering. We will carry out many related estimates during this course so it is important to become familiar with this process. Consider a star in hydrostatic equilibrium in which energy transport is by radiative diffusion. The star is composed of ionized hydrogen and is supported prima ...
here
... and nitrogen. Later, after the star has expelled its gaseous envelope in form of massive stellar winds and a planetary nebula, these cores are found as white dwarfs. A typical white dwarf is half as massive as the Sun, yet only slightly bigger than Earth, with a mean density of ∼ 109 kg/m3 . This fo ...
... and nitrogen. Later, after the star has expelled its gaseous envelope in form of massive stellar winds and a planetary nebula, these cores are found as white dwarfs. A typical white dwarf is half as massive as the Sun, yet only slightly bigger than Earth, with a mean density of ∼ 109 kg/m3 . This fo ...
Great Migrations & other natural history tales
... form in large numbers, and are mostly dispersed throughout the Galaxy afterwards. Sometimes, they are found as orbital companions to stars (not frequently, hence the term “brown dwarf desert” by comparison with the large numbers of planetary companions to stars.) And there is even one BD with it’s o ...
... form in large numbers, and are mostly dispersed throughout the Galaxy afterwards. Sometimes, they are found as orbital companions to stars (not frequently, hence the term “brown dwarf desert” by comparison with the large numbers of planetary companions to stars.) And there is even one BD with it’s o ...