Star Life Cycle Web Activity
... of a Star. Read the web page and the summary of a typical cycle of stars given here. Stars repeat a cycle of reaching equilibrium and then losing it after burning out one fuel source…then condensing (shrinking) because of gravity, making the core more dense and hotter…so hot that now a new element c ...
... of a Star. Read the web page and the summary of a typical cycle of stars given here. Stars repeat a cycle of reaching equilibrium and then losing it after burning out one fuel source…then condensing (shrinking) because of gravity, making the core more dense and hotter…so hot that now a new element c ...
The Stellar Cycle
... What holds the white dwarf from collapsing? • The resulting outward pressure which keeps the electrons apart is called electron degeneracy pressure – this is what balances the weight. • Only if more energy drives the electrons into higher energy states, can the density increase. • Adding mass can d ...
... What holds the white dwarf from collapsing? • The resulting outward pressure which keeps the electrons apart is called electron degeneracy pressure – this is what balances the weight. • Only if more energy drives the electrons into higher energy states, can the density increase. • Adding mass can d ...
The Sun (power point) by Ms. Kimball the_sun_pp
... • Our Sun is a second or third generation star. Second generation stars do not just burn hydrogen, they also burn heavier elements, like helium and metals, and were formed from supernova explosions. • supernova = an exploding star ...
... • Our Sun is a second or third generation star. Second generation stars do not just burn hydrogen, they also burn heavier elements, like helium and metals, and were formed from supernova explosions. • supernova = an exploding star ...
Introduction to Astrophysics, Lecture 10
... Many stars do form in the collapse of a single dust cloud. The collapse is very complex due to fragmentation. The stars interact frequently with each other after formation, through their gravitational attraction. The presence of stars can also induce new star formation. ...
... Many stars do form in the collapse of a single dust cloud. The collapse is very complex due to fragmentation. The stars interact frequently with each other after formation, through their gravitational attraction. The presence of stars can also induce new star formation. ...
Problem Set No. 5
... At R/R⊙ = 0.1, X=0.5572 and Y(He4)=0.4278, while at the surface, X=0.7583 and Y=0.2291. Thus the He/H ratio at the surface is 0.30 while it is 0.77 in the interior. This is because the proton-proton chain operating over 4.5 billion years has converted a lot of the hydrogen in the interior into heliu ...
... At R/R⊙ = 0.1, X=0.5572 and Y(He4)=0.4278, while at the surface, X=0.7583 and Y=0.2291. Thus the He/H ratio at the surface is 0.30 while it is 0.77 in the interior. This is because the proton-proton chain operating over 4.5 billion years has converted a lot of the hydrogen in the interior into heliu ...
Variation of Elements in Nature
... He/3He. When the helium-4 nuclei interact with interstellar hydrogen, part of it is converted into helium-3 (and also helium-2). The ratio of 3He/4He thus will increase with the amount of matter travelled. From the measurement of this ratio it has been estimated that cosmic ray nuclei have travelled ...
... He/3He. When the helium-4 nuclei interact with interstellar hydrogen, part of it is converted into helium-3 (and also helium-2). The ratio of 3He/4He thus will increase with the amount of matter travelled. From the measurement of this ratio it has been estimated that cosmic ray nuclei have travelled ...
Answers
... Hint: Consider the different stages these two stars will go through during their lifetime, and the properties of the final stages. Both stars will become supergiants after leaving the Main Sequence. When the core of the star collapses, both stars will explode as a Supernova. The 40 Msun star will re ...
... Hint: Consider the different stages these two stars will go through during their lifetime, and the properties of the final stages. Both stars will become supergiants after leaving the Main Sequence. When the core of the star collapses, both stars will explode as a Supernova. The 40 Msun star will re ...
Slides from the second lecture
... • Further atom building in solar-type stars is prohibited by the increasingly strong Coulomb barrier (Not enough T and density to get an alpha into a nucleus) – However, in more massive stars, the central temperature may be significantly higher, allowing further reactions to occur. – Iron is the mos ...
... • Further atom building in solar-type stars is prohibited by the increasingly strong Coulomb barrier (Not enough T and density to get an alpha into a nucleus) – However, in more massive stars, the central temperature may be significantly higher, allowing further reactions to occur. – Iron is the mos ...
poll_questions
... surface temperature as our Sun, and is about 1.33 pc from Earth. It has apparent magnitude zero, while our sun has apparent magnitude -27. • The luminosity of α Cen is larger than our Sun • The luminosity of α Cen is much less than our Sun • The flux from α Cen is about 1010 times less than our Sun ...
... surface temperature as our Sun, and is about 1.33 pc from Earth. It has apparent magnitude zero, while our sun has apparent magnitude -27. • The luminosity of α Cen is larger than our Sun • The luminosity of α Cen is much less than our Sun • The flux from α Cen is about 1010 times less than our Sun ...
ASTRONOMY 0089: EXAM 2 Class Meets M,W,F, 1:00 PM Mar 22
... a. are evolved low-mass stars burning He in their core. b. are stars of extremely low mass whose central temperature never gets high enough to initiate the fusion of H into He. c. are extremely young objects approaching the Main Sequence. d. are a form of pulsating star useful for determining stella ...
... a. are evolved low-mass stars burning He in their core. b. are stars of extremely low mass whose central temperature never gets high enough to initiate the fusion of H into He. c. are extremely young objects approaching the Main Sequence. d. are a form of pulsating star useful for determining stella ...
Lecture Slides – Stars
... End of core hydrogen burning core cools, pressure decreases Cores shrinks energy deposited in hydrogen burning shell (Kelvin-Helmholtz contraction; core temperature actually increases when fusion stops!) – CNO burning (thin) ...
... End of core hydrogen burning core cools, pressure decreases Cores shrinks energy deposited in hydrogen burning shell (Kelvin-Helmholtz contraction; core temperature actually increases when fusion stops!) – CNO burning (thin) ...
2017 Maryland Regional
... 22. __This object will eventually end it life in a white-dwarf merger to produce a Type Ia supernova. This is the first documented case of a supernova candidate through white-dwarf merger.__ 23. __ The star, Mira, is thermally pulsing every 10,000 years, with each causing it to increase in luminosit ...
... 22. __This object will eventually end it life in a white-dwarf merger to produce a Type Ia supernova. This is the first documented case of a supernova candidate through white-dwarf merger.__ 23. __ The star, Mira, is thermally pulsing every 10,000 years, with each causing it to increase in luminosit ...
and mass loss
... Collapse: basic questions • Can the collapse of the inner core induce the ejection of the remaining mass (core plus mantle)? • The key problem is how to transfer even a small amount of the energy liberated by the collapsing nucleus to the rest of the star. ...
... Collapse: basic questions • Can the collapse of the inner core induce the ejection of the remaining mass (core plus mantle)? • The key problem is how to transfer even a small amount of the energy liberated by the collapsing nucleus to the rest of the star. ...
Lives of stars HR
... of a pulsar, a rapidly rotating stellar remnant which can appear to blink hundreds or thousands of times per second. The most famous pulsar is in the Crab nebula ...
... of a pulsar, a rapidly rotating stellar remnant which can appear to blink hundreds or thousands of times per second. The most famous pulsar is in the Crab nebula ...
Supernovae
... Supernova’s characteristics are shaped by the progenitor star. Stars more massive than 8 M evolve to an onion-like configuration. A good example for how this happens is the life of one such star - Sanduleak −69◦ 202, the progenitor of the forementioned SN1987A. It all began about 11 million years a ...
... Supernova’s characteristics are shaped by the progenitor star. Stars more massive than 8 M evolve to an onion-like configuration. A good example for how this happens is the life of one such star - Sanduleak −69◦ 202, the progenitor of the forementioned SN1987A. It all began about 11 million years a ...
Stellar Metamorphosis
... evaporation causes loss of surface liquids by this process. There was more water on earth in earlier phases than now and the earth’s water constantly recirculates through its atmosphere via evaporation. During this cooling process life forming amino acid molecules are being produced in the cooling p ...
... evaporation causes loss of surface liquids by this process. There was more water on earth in earlier phases than now and the earth’s water constantly recirculates through its atmosphere via evaporation. During this cooling process life forming amino acid molecules are being produced in the cooling p ...
Star Wreck
... respective minimal values beyond which they are unstable. This leads to an explosion. The lifetime of a contaminated star is determined by the parameters of the underlying supersymmetric theory and can be in the Gyr range. The energy released from the cataclysmic death of a neutron star may be the o ...
... respective minimal values beyond which they are unstable. This leads to an explosion. The lifetime of a contaminated star is determined by the parameters of the underlying supersymmetric theory and can be in the Gyr range. The energy released from the cataclysmic death of a neutron star may be the o ...
Astronomy
... D) White dwarf (only) E) Main sequence and double shell burning 21. What event is responsible for the ultimate death of the Sun? A) All the hydrogen runs out B) All the helium runs out C) The outer layers of the Sun are blown away by strong winds D) The Sun burns all the way to iron, which cannot bu ...
... D) White dwarf (only) E) Main sequence and double shell burning 21. What event is responsible for the ultimate death of the Sun? A) All the hydrogen runs out B) All the helium runs out C) The outer layers of the Sun are blown away by strong winds D) The Sun burns all the way to iron, which cannot bu ...
Properties of stars during hydrogen burning
... is balanced by nuclear energy generation and there is no time dependence of any state variables. The generated heat will then exactly match the outgoing energy flow (luminosity) at any point in the star. Heat flows from hot to cold à temperature gradient is required to carry the luminosity outward: ...
... is balanced by nuclear energy generation and there is no time dependence of any state variables. The generated heat will then exactly match the outgoing energy flow (luminosity) at any point in the star. Heat flows from hot to cold à temperature gradient is required to carry the luminosity outward: ...
Article 8
... Big Bang - the birth of our universe. The universe we can observe is finite. It has a beginning in space and time, before which the concept of space and time has no meaning, because spacetime itself is a property of the universe. According to the Big Bang theory, the universe began about twelve to f ...
... Big Bang - the birth of our universe. The universe we can observe is finite. It has a beginning in space and time, before which the concept of space and time has no meaning, because spacetime itself is a property of the universe. According to the Big Bang theory, the universe began about twelve to f ...
P-nuclei
p-Nuclei (p stands for proton-rich) are certain proton-rich, naturally occurring isotopes of some elements between selenium and mercury which cannot be produced in either s- or r-process.