PhD Qualifying Exam (2010) --
... (b) The equation of state for non-relativistic degeneracy gas can be written as P K 5 3 . Estimate the mass-radius relation of this degenerate star. (3 points) (c) As the mass increase, the electrons gradually become ultra-relativistic and the equation of state becomes P K 4 3 . Show that t ...
... (b) The equation of state for non-relativistic degeneracy gas can be written as P K 5 3 . Estimate the mass-radius relation of this degenerate star. (3 points) (c) As the mass increase, the electrons gradually become ultra-relativistic and the equation of state becomes P K 4 3 . Show that t ...
Stellar Evolution: The Lives of Stars
... Stellar Evolution: The Lives of Stars Stars are not static (unchanging); they evolve, or change over time. They are “born” from giant spinning masses of primarily H & He evolve through common stages and “die” various deaths based on their mass. It is the crushing force of gravity on such great mass ...
... Stellar Evolution: The Lives of Stars Stars are not static (unchanging); they evolve, or change over time. They are “born” from giant spinning masses of primarily H & He evolve through common stages and “die” various deaths based on their mass. It is the crushing force of gravity on such great mass ...
Document
... Binary Star Evolution • Half of all stars are in binary systems - stellar evolution in binaries is important • Roche Lobe: 3-D boundary where the gravity of 2 stars is equal; if a star expands beyond this boundary some of its matter accretes onto the other star • Matter that transfers from one star ...
... Binary Star Evolution • Half of all stars are in binary systems - stellar evolution in binaries is important • Roche Lobe: 3-D boundary where the gravity of 2 stars is equal; if a star expands beyond this boundary some of its matter accretes onto the other star • Matter that transfers from one star ...
Ch_16-18_Example_Exam
... a. The luminosity would increase because the star would become a nova. b. The luminosity would increase because the star’s central pressure would rise and the rate of nuclear reactions would increase. c. The luminosity would decrease because the outgoing energy has to pass through more layers in the ...
... a. The luminosity would increase because the star would become a nova. b. The luminosity would increase because the star’s central pressure would rise and the rate of nuclear reactions would increase. c. The luminosity would decrease because the outgoing energy has to pass through more layers in the ...
Stellar Masses and the Main Sequence
... ~ 10 Gyr = Main sequence lifetime of the Sun ~ 2 × 1033 gm = Mass of the Sun ~ 4 × 1033 ergs/sec = Luminosity of the Sun ~ 7 × 1010 cm = Radius of the Sun ~ 6.3 × 1018 ergs/gm = Energy from hydrogen fusion ~ 27 MeV = mass defect for hydrogen fusion ~ 0.7% = percent mass defect for hydrogen fusion ~ ...
... ~ 10 Gyr = Main sequence lifetime of the Sun ~ 2 × 1033 gm = Mass of the Sun ~ 4 × 1033 ergs/sec = Luminosity of the Sun ~ 7 × 1010 cm = Radius of the Sun ~ 6.3 × 1018 ergs/gm = Energy from hydrogen fusion ~ 27 MeV = mass defect for hydrogen fusion ~ 0.7% = percent mass defect for hydrogen fusion ~ ...
Lecture 16, PPT version
... • Extraordinarily bright, so can use them to measure distances to galaxies that are very far away: b = L / (4 d2) • Supernovae are the source of all heavy chemical elements! • The heavy chemical elements are produced during the explosion itself, when there is more than enough energy to fuse nuclei ...
... • Extraordinarily bright, so can use them to measure distances to galaxies that are very far away: b = L / (4 d2) • Supernovae are the source of all heavy chemical elements! • The heavy chemical elements are produced during the explosion itself, when there is more than enough energy to fuse nuclei ...
Exploring the Planet Forming Environments of Young Suns
... Greaves et al. (2008) collides and sticks together, building up larger bodies. May take about 10 Myr to build Jupiter. X GI: Gravitational instability leads to rapid planet formation. ...
... Greaves et al. (2008) collides and sticks together, building up larger bodies. May take about 10 Myr to build Jupiter. X GI: Gravitational instability leads to rapid planet formation. ...
Gravity simplest fusion
... • When a neutron star forms, the pull of gravity is so great that it overrides the electron degeneracy pressure of the atoms of the star. • The electrons are forced into their respective nuclei, where they combine with protons to form neutrons. This greatly decreases the size of each atom, and allow ...
... • When a neutron star forms, the pull of gravity is so great that it overrides the electron degeneracy pressure of the atoms of the star. • The electrons are forced into their respective nuclei, where they combine with protons to form neutrons. This greatly decreases the size of each atom, and allow ...
Life Cycle of a Star - Intervention Worksheet
... _____ The star begins to run out of fuel and expands into a red giant or red super giant. _____ Stars start out as diffused clouds of gas and dust drifting through space. A single one of these clouds is called a nebula _____ What happens next depends on the mass of the star. _____ Heat and pressure ...
... _____ The star begins to run out of fuel and expands into a red giant or red super giant. _____ Stars start out as diffused clouds of gas and dust drifting through space. A single one of these clouds is called a nebula _____ What happens next depends on the mass of the star. _____ Heat and pressure ...
Lecture Notes – Stars
... This happens in less than a second. The outer layers of the star are still collapsing and hit the hard neutron star in the centre, causing a violent rebound or shock wave to move outwards. The outer portion of the star is blown away at speeds of 5 000–30 000 km s−1 to form a supernova remnant. Super ...
... This happens in less than a second. The outer layers of the star are still collapsing and hit the hard neutron star in the centre, causing a violent rebound or shock wave to move outwards. The outer portion of the star is blown away at speeds of 5 000–30 000 km s−1 to form a supernova remnant. Super ...
Stellar Masses and the Main Sequence
... Measurements of main-sequence stars demonstrate that there is a mass-luminosity relationship, i.e., L ∝ Mη. For M > 1 M η ~3.88, while at lower masses, the relation flattens out. I good rule-of-thumb is L ∝ Mη, with η ~ 3.5. ...
... Measurements of main-sequence stars demonstrate that there is a mass-luminosity relationship, i.e., L ∝ Mη. For M > 1 M η ~3.88, while at lower masses, the relation flattens out. I good rule-of-thumb is L ∝ Mη, with η ~ 3.5. ...
Neutron Stars and Black Holes
... a)! They are only regular pulsing stars, so it is a natural evolution of stars with magnetic fields. b)! Supernova of a massive star, leaving a neutron core mass of 1.4 to 3 solar masses. c)! By evolution from a supergiant to a compact, hot, but pulsing star. d)! Through the evolution of a binary sy ...
... a)! They are only regular pulsing stars, so it is a natural evolution of stars with magnetic fields. b)! Supernova of a massive star, leaving a neutron core mass of 1.4 to 3 solar masses. c)! By evolution from a supergiant to a compact, hot, but pulsing star. d)! Through the evolution of a binary sy ...
ppt - Wladimir Lyra
... What happens to the inert Helium core? It keeps contracting and heating At some point the density is so high it goes degenerate A phase transition has occured The core stops behaving like a gas and starts behaving more like a solid ...
... What happens to the inert Helium core? It keeps contracting and heating At some point the density is so high it goes degenerate A phase transition has occured The core stops behaving like a gas and starts behaving more like a solid ...
Stellar Evolution: The Live and Death of a Star
... hundreds of times the luminosity of the sun and its radius is around 100 solar radii ...
... hundreds of times the luminosity of the sun and its radius is around 100 solar radii ...
Star Life
... 8) The smallest of stars will end their life as which of the following? a. Black Hole b. White Dwarf c. Super Red Giant d. Neutron Star 9) A main sequence star is mostly made of which two elements? a. Hydrogen and Carbon b. Hydrogen and Helium c. Helium and Carbon d. Helium and Iron 10) Which stage ...
... 8) The smallest of stars will end their life as which of the following? a. Black Hole b. White Dwarf c. Super Red Giant d. Neutron Star 9) A main sequence star is mostly made of which two elements? a. Hydrogen and Carbon b. Hydrogen and Helium c. Helium and Carbon d. Helium and Iron 10) Which stage ...
STARS
... – Blue (Short λ) = Hot – Red (Long λ) = Cool – The hotter they are the faster they burn out ...
... – Blue (Short λ) = Hot – Red (Long λ) = Cool – The hotter they are the faster they burn out ...
The Life and Death of Stars
... It has been doing this for 4.5 billion years Has enough Hydrogen in the core for 5 billion years What happens when all the core hydrogen is burnt? – the core will collapse, become denser and hotter – Helium starts to fuse into Carbon and Oxygen ...
... It has been doing this for 4.5 billion years Has enough Hydrogen in the core for 5 billion years What happens when all the core hydrogen is burnt? – the core will collapse, become denser and hotter – Helium starts to fuse into Carbon and Oxygen ...
Stellar Evolution Reading Questions Integrated Science 2 Name
... 2. The birthplaces of stars are dark, cool interstellar ______________. These nebulae are made up of ____________ and gases. For some reason, some nebulae become dense enough to begin to _______________. A shock wave from an ___________________ of a nearby star may trigger the contraction. Once the ...
... 2. The birthplaces of stars are dark, cool interstellar ______________. These nebulae are made up of ____________ and gases. For some reason, some nebulae become dense enough to begin to _______________. A shock wave from an ___________________ of a nearby star may trigger the contraction. Once the ...
Slide 1
... • Stars greater than eight solar masses can have fusion in their cores going all the way up to iron, which is stable against further fusion. • The star continues to collapse after the iron core is found, implodes, and then explodes as a supernova. ...
... • Stars greater than eight solar masses can have fusion in their cores going all the way up to iron, which is stable against further fusion. • The star continues to collapse after the iron core is found, implodes, and then explodes as a supernova. ...
PHY-105: Final Stages of Stellar Evolution
... Photodisintegration → ν burst, which preceeds maximum light and can be used to “trigger” on supernovae. Remnant is either a neutron star or black hole – we’ll look at both of these in more detail next lecture(s). With photodisintegration, core collapses extremely rapidly, dissociating itself from th ...
... Photodisintegration → ν burst, which preceeds maximum light and can be used to “trigger” on supernovae. Remnant is either a neutron star or black hole – we’ll look at both of these in more detail next lecture(s). With photodisintegration, core collapses extremely rapidly, dissociating itself from th ...
Life Cycle of a Star - Intervention Worksheet
... _____ Heat and pressure build in the core of the protostar until nuclear fusion takes place. _____ The force of gravity pulls a nebula together forming clumps called protostars. _____ Hydrogen atoms are fused together generating an enormous amount of energy igniting the star causing it to shine. ...
... _____ Heat and pressure build in the core of the protostar until nuclear fusion takes place. _____ The force of gravity pulls a nebula together forming clumps called protostars. _____ Hydrogen atoms are fused together generating an enormous amount of energy igniting the star causing it to shine. ...
The Life Cycles of 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 ...
ASTR 1120H – Spring Semester 2010 Exam 2 – Answers The
... Astronomers learn about mass from binary stars (a fundamental parameter that cannot be obtained from single stars). The mass can be calculated, using Newton's version of Kepler's 3rd law, from the binary system's period and orbital separation. 9. What are H II regions? Near what kinds of stars are t ...
... Astronomers learn about mass from binary stars (a fundamental parameter that cannot be obtained from single stars). The mass can be calculated, using Newton's version of Kepler's 3rd law, from the binary system's period and orbital separation. 9. What are H II regions? Near what kinds of stars are t ...