Life Cycle of a Star - Intervention Worksheet
... massive stars become black holes when they die. After a massive star explodes, a large amount of mass may remain. The gravity of the mass is so strong that gas is pulled inward, pulling more gas into a smaller and smaller space. Eventually, the gravity becomes so strong that nothing can escape, not ...
... massive stars become black holes when they die. After a massive star explodes, a large amount of mass may remain. The gravity of the mass is so strong that gas is pulled inward, pulling more gas into a smaller and smaller space. Eventually, the gravity becomes so strong that nothing can escape, not ...
Directed Reading Section: Characteristics of Stars
... d. They are brighter than the sun. 25. What are three types of actual motion that stars may have? _______________________________________________________________ _______________________________________________________________ _______________________________________________________________ Original c ...
... d. They are brighter than the sun. 25. What are three types of actual motion that stars may have? _______________________________________________________________ _______________________________________________________________ _______________________________________________________________ Original c ...
30-1 Directed Reading
... d. They are brighter than the sun. 25. What are three types of actual motion that stars may have? _______________________________________________________________ _______________________________________________________________ _______________________________________________________________ Original c ...
... d. They are brighter than the sun. 25. What are three types of actual motion that stars may have? _______________________________________________________________ _______________________________________________________________ _______________________________________________________________ Original c ...
Homework #8 Solutions - Department of Physics and Astronomy
... Problem 12-4: Find the distance in parsecs to a visual binary that consists of stars of absolute bolometric magnitudes of +5.0 and +2.0. The mean angular separation is 0.005”, and the observed orbital period is ten years. The stars obey the mass-luminosity relation, equations 125a, b, and c. What as ...
... Problem 12-4: Find the distance in parsecs to a visual binary that consists of stars of absolute bolometric magnitudes of +5.0 and +2.0. The mean angular separation is 0.005”, and the observed orbital period is ten years. The stars obey the mass-luminosity relation, equations 125a, b, and c. What as ...
Nuclear Astrophysics
... After the algebra (you should check, to make sure I’m right ), we arrive at the Mass Luminosity Relation for Main Sequence stars! ...
... After the algebra (you should check, to make sure I’m right ), we arrive at the Mass Luminosity Relation for Main Sequence stars! ...
La teoria del big bang y la formacion del Universo
... • Within a few hundred million years after the Big Bang, the hydrogen and helium had pulled together under the force of gravity to form stars, which shine because hydrogen atoms are fusing together to make helium atoms, releasing radiation energy in the process. • When the hydrogen runs out, the s ...
... • Within a few hundred million years after the Big Bang, the hydrogen and helium had pulled together under the force of gravity to form stars, which shine because hydrogen atoms are fusing together to make helium atoms, releasing radiation energy in the process. • When the hydrogen runs out, the s ...
A Tale of Star and Planet Formation
... We are using Keck to observe young binary systems as they form. These studies are difficult because binary stars are typically very close together in projection and because atmospheric distortions blur our observations. Keck can observe these stars because of a technology called Adaptive Optics. AO ...
... We are using Keck to observe young binary systems as they form. These studies are difficult because binary stars are typically very close together in projection and because atmospheric distortions blur our observations. Keck can observe these stars because of a technology called Adaptive Optics. AO ...
Star Formation Triggers More Star Formation
... This is National Dark Sky Week. Turn off unnecessary outdoor lighting and enjoy darker skies. Also, be sure to check out the web site at ...
... This is National Dark Sky Week. Turn off unnecessary outdoor lighting and enjoy darker skies. Also, be sure to check out the web site at ...
1. a. Collisionless Boltzmann—particles moving in smooth potential
... a. The difference of A-B=V0/R0 and using R0=8 kpc we get V0=220 km/s. Note that the errors in Oort’s A and B combine with errors in the distance to make V0 depressingly uncertain so you will see a variety of values used in the literature. b. We can derive V(R) for R
... a. The difference of A-B=V0/R0 and using R0=8 kpc we get V0=220 km/s. Note that the errors in Oort’s A and B combine with errors in the distance to make V0 depressingly uncertain so you will see a variety of values used in the literature. b. We can derive V(R) for R
Lecture 19
... doesn’t emit much light – very small and dim star, little black holes • More likely it is elementary particles other than normal matter ...
... doesn’t emit much light – very small and dim star, little black holes • More likely it is elementary particles other than normal matter ...
type II supernova
... • This sudden collapse of a massive star's core into a volume over a million times smaller than its original volume is really bad news for the star. The outer layers of the star come raining down onto the core. Somehow this collapse changes into an explosion: a type II supernova. The process by whic ...
... • This sudden collapse of a massive star's core into a volume over a million times smaller than its original volume is really bad news for the star. The outer layers of the star come raining down onto the core. Somehow this collapse changes into an explosion: a type II supernova. The process by whic ...
Document
... donor shrinks as a consequence of its mass loss, increasing the rate at which it loses mass stable mass transfer - the Roche-lobe of the mass donor grows as a consequence of its mass loss, stopping the mass transfer ...
... donor shrinks as a consequence of its mass loss, increasing the rate at which it loses mass stable mass transfer - the Roche-lobe of the mass donor grows as a consequence of its mass loss, stopping the mass transfer ...
Part 2
... • At low T (solar center), the cycle is too slow to be important, but the C → N transformation is working. • Equivalent cycles involving Na and Mg exist and operate partially at higher temperature (≈ 5 · 107 K). • With increasing temperature, the CNO-cycle becomes more dominant. ...
... • At low T (solar center), the cycle is too slow to be important, but the C → N transformation is working. • Equivalent cycles involving Na and Mg exist and operate partially at higher temperature (≈ 5 · 107 K). • With increasing temperature, the CNO-cycle becomes more dominant. ...
ppt
... slowly eaten away by the ultraviolet radiation, a denser than average globule of gas begins to be uncovered ...
... slowly eaten away by the ultraviolet radiation, a denser than average globule of gas begins to be uncovered ...
Temperature of stars
... Planets do not generate light like a stars do. They are heated by the light they absorb, not by the light they reflect. ...
... Planets do not generate light like a stars do. They are heated by the light they absorb, not by the light they reflect. ...
10.2 Galaxies
... • If the nebula cloud is massive enough, gravity within the cloud will be large enough to shrink it and to raise its temperature above 10 000 000 degrees celsius, a temperature at which atomic fusion happens, releasing huge amounts of energy in the form of all kinds of electromagnetic radiation (gam ...
... • If the nebula cloud is massive enough, gravity within the cloud will be large enough to shrink it and to raise its temperature above 10 000 000 degrees celsius, a temperature at which atomic fusion happens, releasing huge amounts of energy in the form of all kinds of electromagnetic radiation (gam ...
Chapter 3: the Sun - University of Waterloo
... collapsing material forms a disk. Eventually T becomes high enough that molecular hydrogen dissociates; this absorbs some of the energy supporting the protostar, so the core begins to collapse further, until it becomes ~30% larger than the present Solar radius (but still much less massive). The prot ...
... collapsing material forms a disk. Eventually T becomes high enough that molecular hydrogen dissociates; this absorbs some of the energy supporting the protostar, so the core begins to collapse further, until it becomes ~30% larger than the present Solar radius (but still much less massive). The prot ...
S E D
... variables; P,T, p and u (internal energy). Another equation of state which is very different is for degeneracy. It is important when talking about very high density and low temperature. Degeneracy: The pressure rises due to the Pauli exclusion principle, meaning that it prevents particles to enter i ...
... variables; P,T, p and u (internal energy). Another equation of state which is very different is for degeneracy. It is important when talking about very high density and low temperature. Degeneracy: The pressure rises due to the Pauli exclusion principle, meaning that it prevents particles to enter i ...
Luminosity and magnitude
... Wien’s law: the hotter the object the bluer is its emission. Stefan’s law: energy emitted per unit area increases as the 4th power of the temperature….. Luminosity radius2 * temperture4 ...
... Wien’s law: the hotter the object the bluer is its emission. Stefan’s law: energy emitted per unit area increases as the 4th power of the temperature….. Luminosity radius2 * temperture4 ...
4.5.5. Black Holes
... the event horizon. To the Minkowskian observer at r , light emitted by an ingoing particle will be redshifted by an increasing amount as the particle approaches the event horizon. Physically, one possible way to form black holes is through the collapse of stars or cluster of stars [see S.W.Hawki ...
... the event horizon. To the Minkowskian observer at r , light emitted by an ingoing particle will be redshifted by an increasing amount as the particle approaches the event horizon. Physically, one possible way to form black holes is through the collapse of stars or cluster of stars [see S.W.Hawki ...
Astronomy 100, Fall 2006 Name: Due: November 28, 2006 at 11 a.m.
... In 1965, two Bell Lab researchers, Arno Penzias and Robert Wilson, discovered that, no matter where they pointed their microwave telescope, they found microwave radiation corresponding (remember Wien’s Law?) to a temperature of 3 Kelvins. ...
... In 1965, two Bell Lab researchers, Arno Penzias and Robert Wilson, discovered that, no matter where they pointed their microwave telescope, they found microwave radiation corresponding (remember Wien’s Law?) to a temperature of 3 Kelvins. ...
4th Six Weeks Review key
... 23. At which point in the diagram above is fusion taking place? ____C____ Hertzsprung-Russell Diagram 24. HR diagrams show the relationships between __brightness__ and __temperature___ of stars in the universe. 25. On an HR Diagram you find the __hot_ stars on the left side and the __cool_ stars on ...
... 23. At which point in the diagram above is fusion taking place? ____C____ Hertzsprung-Russell Diagram 24. HR diagrams show the relationships between __brightness__ and __temperature___ of stars in the universe. 25. On an HR Diagram you find the __hot_ stars on the left side and the __cool_ stars on ...
Observing the Universe 3
... 8. What two things does the intrinsic (actual) brightness of a star depend on? (i) ……………………………….………………………….. (ii) ……………………………………….………………….. 9. Two stars are of the same actual brightness but one looks fainter than the other when seen from the Earth. Why is this? ...
... 8. What two things does the intrinsic (actual) brightness of a star depend on? (i) ……………………………….………………………….. (ii) ……………………………………….………………….. 9. Two stars are of the same actual brightness but one looks fainter than the other when seen from the Earth. Why is this? ...
Main sequence
In astronomy, the main sequence is a continuous and distinctive band of stars that appears on plots of stellar color versus brightness. These color-magnitude plots are known as Hertzsprung–Russell diagrams after their co-developers, Ejnar Hertzsprung and Henry Norris Russell. Stars on this band are known as main-sequence stars or ""dwarf"" stars.After a star has formed, it generates thermal energy in the dense core region through the nuclear fusion of hydrogen atoms into helium. During this stage of the star's lifetime, it is located along the main sequence at a position determined primarily by its mass, but also based upon its chemical composition and other factors. All main-sequence stars are in hydrostatic equilibrium, where outward thermal pressure from the hot core is balanced by the inward pressure of gravitational collapse from the overlying layers. The strong dependence of the rate of energy generation in the core on the temperature and pressure helps to sustain this balance. Energy generated at the core makes its way to the surface and is radiated away at the photosphere. The energy is carried by either radiation or convection, with the latter occurring in regions with steeper temperature gradients, higher opacity or both.The main sequence is sometimes divided into upper and lower parts, based on the dominant process that a star uses to generate energy. Stars below about 1.5 times the mass of the Sun (or 1.5 solar masses (M☉)) primarily fuse hydrogen atoms together in a series of stages to form helium, a sequence called the proton–proton chain. Above this mass, in the upper main sequence, the nuclear fusion process mainly uses atoms of carbon, nitrogen and oxygen as intermediaries in the CNO cycle that produces helium from hydrogen atoms. Main-sequence stars with more than two solar masses undergo convection in their core regions, which acts to stir up the newly created helium and maintain the proportion of fuel needed for fusion to occur. Below this mass, stars have cores that are entirely radiative with convective zones near the surface. With decreasing stellar mass, the proportion of the star forming a convective envelope steadily increases, whereas main-sequence stars below 0.4 M☉ undergo convection throughout their mass. When core convection does not occur, a helium-rich core develops surrounded by an outer layer of hydrogen.In general, the more massive a star is, the shorter its lifespan on the main sequence. After the hydrogen fuel at the core has been consumed, the star evolves away from the main sequence on the HR diagram. The behavior of a star now depends on its mass, with stars below 0.23 M☉ becoming white dwarfs directly, whereas stars with up to ten solar masses pass through a red giant stage. More massive stars can explode as a supernova, or collapse directly into a black hole.