Chapter 12
... The white dwarf is an object about the size of the Earth! (~0.01 solar radii, 12,000 km) The collapse is stopped due to ...
... The white dwarf is an object about the size of the Earth! (~0.01 solar radii, 12,000 km) The collapse is stopped due to ...
ASTR1010_HW06
... begins as small grains collide and stick until 100 meter clumps of solid material are produced. At this point, collisions continue to increase the size of the clumps, but now the collisions must occur more gently (think of glancing as opposed to head-on collisions). When the clumps have grown into p ...
... begins as small grains collide and stick until 100 meter clumps of solid material are produced. At this point, collisions continue to increase the size of the clumps, but now the collisions must occur more gently (think of glancing as opposed to head-on collisions). When the clumps have grown into p ...
The Evolution of Stars - hrsbstaff.ednet.ns.ca
... Gravity is the force that keeps us safely planted here on Earth, but it is more that just that. Gravity, or gravitation, is the natural phenomenon by which all objects with mass attract other objects. Without gravity the universe would be a very different place. ...
... Gravity is the force that keeps us safely planted here on Earth, but it is more that just that. Gravity, or gravitation, is the natural phenomenon by which all objects with mass attract other objects. Without gravity the universe would be a very different place. ...
Solution - Caltech Astronomy
... m A = 4.13 MŸ , mB = 0.998 MŸ . (d) Assuming the orbital separation is much larger than the stellar radii, and that the orbits are circular, we can treat the velocity of the stars during eclipse as completely in the plane of the sky. For circular orbits, the maximum radial velocities given are the c ...
... m A = 4.13 MŸ , mB = 0.998 MŸ . (d) Assuming the orbital separation is much larger than the stellar radii, and that the orbits are circular, we can treat the velocity of the stars during eclipse as completely in the plane of the sky. For circular orbits, the maximum radial velocities given are the c ...
ASTR 553/554 (1) : Questions
... questions that follow, work with either I(R) or µ(R), which ever your prefer. b. What's the surface brightness, I(0), at the center of the Milky Way disk, and what's the disk's total luminosity in LV, . c. Using MV, = 4.82, calculate the Milky Way's absolute magnitude, MV. If viewed from Virgo (dist ...
... questions that follow, work with either I(R) or µ(R), which ever your prefer. b. What's the surface brightness, I(0), at the center of the Milky Way disk, and what's the disk's total luminosity in LV, . c. Using MV, = 4.82, calculate the Milky Way's absolute magnitude, MV. If viewed from Virgo (dist ...
MULTIPLE CHOICE. Choose the one alternative that best
... A) The rotation dissipates and any residual is left in small overall rotation of the star. B) The rotation rate remains the same and results in stellar rotation. C) The rotation rate increases and results in fast rotation of the star. D) The rotation rate increases and results in a disk of material ...
... A) The rotation dissipates and any residual is left in small overall rotation of the star. B) The rotation rate remains the same and results in stellar rotation. C) The rotation rate increases and results in fast rotation of the star. D) The rotation rate increases and results in a disk of material ...
Properties of Stars: The H
... • There is a very interesting story of the chemical enrichment history of the Galaxy and Universe that goes with these `metal-poor’ stars that we will return to in a few weeks. For now will only note that the chemically deficient stars are the oldest stars in the Galaxy. So far the most chemically d ...
... • There is a very interesting story of the chemical enrichment history of the Galaxy and Universe that goes with these `metal-poor’ stars that we will return to in a few weeks. For now will only note that the chemically deficient stars are the oldest stars in the Galaxy. So far the most chemically d ...
AY1 Homework for Quiz 2: Spring 2017
... 9. “Hydrostatic” models for the Sun or other stars are based on (check any that are correct): ____ A. Gas pressure compressing stars to the point just before they become liquid ____ B. Balancing the fo ...
... 9. “Hydrostatic” models for the Sun or other stars are based on (check any that are correct): ____ A. Gas pressure compressing stars to the point just before they become liquid ____ B. Balancing the fo ...
Properties of Stars
... Sometimes the orbital plane is lined up so that the stars pass in front of each other as seen from the Earth. Each eclipse will cause the total light from the system to decrease. The amount of the decrease will depend on how much of each star is covered up (they can have different sizes) and on the ...
... Sometimes the orbital plane is lined up so that the stars pass in front of each other as seen from the Earth. Each eclipse will cause the total light from the system to decrease. The amount of the decrease will depend on how much of each star is covered up (they can have different sizes) and on the ...
Chapter 3 - BITS Pilani
... • What are the typical temperatures here ? 4400 K (outermost layer) – 9400 K (innermost layer) • What are the typical densities here ? ~ 10-3 kg/m3 (innermost layer) • What is happening here ? ...
... • What are the typical temperatures here ? 4400 K (outermost layer) – 9400 K (innermost layer) • What are the typical densities here ? ~ 10-3 kg/m3 (innermost layer) • What is happening here ? ...
3 rd stage of a star`s life = red giant
... 2. Very massive stars will become blue giants during their main sequence. Their main sequence may last only a few hundred thousand years. 3. Smaller stars, like the Sun, will burn for several billion years during their main sequence stage. ...
... 2. Very massive stars will become blue giants during their main sequence. Their main sequence may last only a few hundred thousand years. 3. Smaller stars, like the Sun, will burn for several billion years during their main sequence stage. ...
Slide 1
... Modelling the Sun • A star like the Sun can burn steadily for billions of years, so it must radiate energy at the same rate that it generates it from fusion reactions Physicist can use these ideas to develop models of the inside of a star. ...
... Modelling the Sun • A star like the Sun can burn steadily for billions of years, so it must radiate energy at the same rate that it generates it from fusion reactions Physicist can use these ideas to develop models of the inside of a star. ...
Black Holes - Department of Physics, USU
... fast-spinning disk around its equator • Near the event horizon, infalling matter is speeding around at near the speed of light!!! • This causes extreme frictional heating in the gas, making it emit X-rays and gamma-rays – 10’s of millions of degrees Kelvin ...
... fast-spinning disk around its equator • Near the event horizon, infalling matter is speeding around at near the speed of light!!! • This causes extreme frictional heating in the gas, making it emit X-rays and gamma-rays – 10’s of millions of degrees Kelvin ...
ppt
... M83 is a barred spiral galaxy with a starburst nucleus, located in the Centaurus A group, at a distance of 3.7 Mpc. It was observed by Chandra in 2000 April. About 55% of the total emission in the nuclear region is unresolved. About 80% of the unresolved nuclear emission can be attributed to hot the ...
... M83 is a barred spiral galaxy with a starburst nucleus, located in the Centaurus A group, at a distance of 3.7 Mpc. It was observed by Chandra in 2000 April. About 55% of the total emission in the nuclear region is unresolved. About 80% of the unresolved nuclear emission can be attributed to hot the ...
Incredible Shrinking Stars
... smaller than the stellar core. The stellar core was rotating (because it was part of a rotating star). When the core collapses, the rotation is concentrated (sort of) in the neutron. Consequently, tbe neutron star ends up spinning very rapidly 4. The interior of a neutron star consists of neutrons. ...
... smaller than the stellar core. The stellar core was rotating (because it was part of a rotating star). When the core collapses, the rotation is concentrated (sort of) in the neutron. Consequently, tbe neutron star ends up spinning very rapidly 4. The interior of a neutron star consists of neutrons. ...
Measuring the Properties of Stars
... (m + M)P2 = a3 is a useful equation for determining total mass of a binary system when measurements of the separation between the primary and secondary bodies, and the calculation of the period of revolution of the secondary body about the primary body can be made. Actually, this equation can determ ...
... (m + M)P2 = a3 is a useful equation for determining total mass of a binary system when measurements of the separation between the primary and secondary bodies, and the calculation of the period of revolution of the secondary body about the primary body can be made. Actually, this equation can determ ...
Black Holes
... • The event horizon is referred to as such because if an event occurs within the boundary, information from that event cannot reach an outside observer, making it impossible to determine if such an event occurred. • To a distant observer, clocks near a black hole appear to tick more slowly than tho ...
... • The event horizon is referred to as such because if an event occurs within the boundary, information from that event cannot reach an outside observer, making it impossible to determine if such an event occurred. • To a distant observer, clocks near a black hole appear to tick more slowly than tho ...
Solutions2
... Problem 3: Why is the earth warm? Assume a blackbody-like planet orbits a star in a circular orbit with radius a. The star has radius R? and effective surface temperature T? . a) Assuming that energy is conserved, derive an equation for the effective surface temperature of the planet. The temperatur ...
... Problem 3: Why is the earth warm? Assume a blackbody-like planet orbits a star in a circular orbit with radius a. The star has radius R? and effective surface temperature T? . a) Assuming that energy is conserved, derive an equation for the effective surface temperature of the planet. The temperatur ...
Gravitation Key:
... 11. When a star runs out of fuel and slows its rate of energy emission, gravitational forces can compress the star to the point that it can become a black hole. What must the radius of Rigel A be to become a black hole? Hint: Escape velocity should equal the speed of light, use goalseek to set escap ...
... 11. When a star runs out of fuel and slows its rate of energy emission, gravitational forces can compress the star to the point that it can become a black hole. What must the radius of Rigel A be to become a black hole? Hint: Escape velocity should equal the speed of light, use goalseek to set escap ...
mam.evolution
... a) electrons must be moving quickly to change orbitals b) the high temperature is necessary to fully cook the new ...
... a) electrons must be moving quickly to change orbitals b) the high temperature is necessary to fully cook the new ...
Comet Pan-Starrs 12 March 2013
... • Spectral types O and B • Masses up to ~ 120 M • Luminosities up to ~106 L • Radii up to ~100 R • What sets the upper mass limit? Radiation Pressure (L) exceeds gravity (M/R2) ...
... • Spectral types O and B • Masses up to ~ 120 M • Luminosities up to ~106 L • Radii up to ~100 R • What sets the upper mass limit? Radiation Pressure (L) exceeds gravity (M/R2) ...
Document
... 2) It is impossible to define the position & momentum of a particle to an accuracy better than Planck’s constant, h. I.e., if !x & !px are the uncertainties in the position & momentum of a particle, respectively, then • Pressure arises from the random motions of particles. Thus, for electrons, even ...
... 2) It is impossible to define the position & momentum of a particle to an accuracy better than Planck’s constant, h. I.e., if !x & !px are the uncertainties in the position & momentum of a particle, respectively, then • Pressure arises from the random motions of particles. Thus, for electrons, even ...
Stars & Galaxies
... • The remnants of the explosion could become a neutron star • Stars this size usually undergo fusion for less time than the sun-like stars. • As a supergiant can suddenly explode into a supernova. ...
... • The remnants of the explosion could become a neutron star • Stars this size usually undergo fusion for less time than the sun-like stars. • As a supergiant can suddenly explode into a supernova. ...
Outline2a
... The Beginning of Star Formation Where there is gas, there is also dust, which absorbs and scatters light. Dust in space can be seen in silhouette, as it blocks out the light from more distant stars. ...
... The Beginning of Star Formation Where there is gas, there is also dust, which absorbs and scatters light. Dust in space can be seen in silhouette, as it blocks out the light from more distant stars. ...
Stars, Galaxies and the Universe FORM A
... (c) Neutron stars have intense gravity and can bend light. (d) All pulsars are neutron stars. (e) Massive stars collapse to form neutron stars. 42. Stars in a binary system orbit ___. (a) on elliptical paths (b) around the North Pole star (c) in each other’s Roche Lobes (d) around a common center of ...
... (c) Neutron stars have intense gravity and can bend light. (d) All pulsars are neutron stars. (e) Massive stars collapse to form neutron stars. 42. Stars in a binary system orbit ___. (a) on elliptical paths (b) around the North Pole star (c) in each other’s Roche Lobes (d) around a common center of ...
Cygnus X-1
Cygnus X-1 (abbreviated Cyg X-1) is a well-known galactic X-ray source, thought to be a black hole, in the constellation Cygnus. It was discovered in 1964 during a rocket flight and is one of the strongest X-ray sources seen from Earth, producing a peak X-ray flux density of 6977229999999999999♠2.3×10−23 Wm−2 Hz−1 (7003230000000000000♠2.3×103 Jansky). Cygnus X-1 was the first X-ray source widely accepted to be a black hole and it remains among the most studied astronomical objects in its class. The compact object is now estimated to have a mass about 14.8 times the mass of the Sun and has been shown to be too small to be any known kind of normal star, or other likely object besides a black hole. If so, the radius of its event horizon is about 7004440000000000000♠44 km.Cygnus X-1 belongs to a high-mass X-ray binary system about 7019574266339685654♠6070 ly from the Sun that includes a blue supergiant variable star designated HDE 226868 which it orbits at about 0.2 AU, or 20% of the distance from the Earth to the Sun. A stellar wind from the star provides material for an accretion disk around the X-ray source. Matter in the inner disk is heated to millions of degrees, generating the observed X-rays. A pair of jets, arranged perpendicular to the disk, are carrying part of the energy of the infalling material away into interstellar space.This system may belong to a stellar association called Cygnus OB3, which would mean that Cygnus X-1 is about five million years old and formed from a progenitor star that had more than 7001400000000000000♠40 solar masses. The majority of the star's mass was shed, most likely as a stellar wind. If this star had then exploded as a supernova, the resulting force would most likely have ejected the remnant from the system. Hence the star may have instead collapsed directly into a black hole.Cygnus X-1 was the subject of a friendly scientific wager between physicists Stephen Hawking and Kip Thorne in 1975, with Hawking betting that it was not a black hole. He conceded the bet in 1990 after observational data had strengthened the case that there was indeed a black hole in the system. This hypothesis has not been confirmed due to a lack of direct observation but has generally been accepted from indirect evidence.