Handout 30
... The band that runs diagonally through the Hertzsprung-Russell diagram and extends from cool, dim, red stars at the lower right to hot, bright, blue stars at the upper left. ...
... The band that runs diagonally through the Hertzsprung-Russell diagram and extends from cool, dim, red stars at the lower right to hot, bright, blue stars at the upper left. ...
Conceptual Physics
... 3. In a random sample of stars in the Sun’s neighborhood, you would expect about 90% of them: a. To be red giants b. To be white dwarfs c. To be main sequence stars d. To have just been born e. To be older than the Sun 4. A star near the top of the main sequence has a mass about: a. Twice the Sun’s ...
... 3. In a random sample of stars in the Sun’s neighborhood, you would expect about 90% of them: a. To be red giants b. To be white dwarfs c. To be main sequence stars d. To have just been born e. To be older than the Sun 4. A star near the top of the main sequence has a mass about: a. Twice the Sun’s ...
Unit 3 - Section 9.2 2011 Star Characteristics0
... 2. There is also a spectral pattern for the Sun. What is the elemental composition of the Sun? 3. There are three “mystery stars.” Using a ruler, line up the spectral patterns of the elements to the mystery stars. 4. Answer the following questions. a. In which two mystery stars is calcium present? b ...
... 2. There is also a spectral pattern for the Sun. What is the elemental composition of the Sun? 3. There are three “mystery stars.” Using a ruler, line up the spectral patterns of the elements to the mystery stars. 4. Answer the following questions. a. In which two mystery stars is calcium present? b ...
Ch 20-21 Review
... 13) The Roche lobe of a star in a binary star system: A) resembles the ear of Edouard Roche, a French mathematician. B) is, in terms of the star's gravity, its "zone of influence." C) is the part of a rapidly rotating star that will eventually spin away to form planets. D) is the accretion disk aro ...
... 13) The Roche lobe of a star in a binary star system: A) resembles the ear of Edouard Roche, a French mathematician. B) is, in terms of the star's gravity, its "zone of influence." C) is the part of a rapidly rotating star that will eventually spin away to form planets. D) is the accretion disk aro ...
Black Holes - Solar Physics and Space Weather
... gravitational compression will overwhelm any and all forms of internal pressure, including degenerate neutrons and nuclear forces • The stellar corpse will collapse to a singularity, immediately around which the escape speed exceeds the speed of light • Far away from the black hole, the space is the ...
... gravitational compression will overwhelm any and all forms of internal pressure, including degenerate neutrons and nuclear forces • The stellar corpse will collapse to a singularity, immediately around which the escape speed exceeds the speed of light • Far away from the black hole, the space is the ...
Lab 2: The Planisphere
... distortion, constellations in the sky will not appear as they do on the planisphere, but the planisphere can help us identify bright stars and give us a general idea of where to look for other stars. It's also very useful in figuring out when certain star will rise or set. The best way to get comfor ...
... distortion, constellations in the sky will not appear as they do on the planisphere, but the planisphere can help us identify bright stars and give us a general idea of where to look for other stars. It's also very useful in figuring out when certain star will rise or set. The best way to get comfor ...
Solutions to test #2 taken on Monday
... 20. (5) Two galaxies orbit one another at a separation of 500 kpc. Their orbital period is estimated to be 30 billion years. Use Kepler’s third law to find the total mass of the pair. Show all work. Possibly helpful values and equations: 1 pc = 3 x 1018 cm, 1 pc = 206,265 ...
... 20. (5) Two galaxies orbit one another at a separation of 500 kpc. Their orbital period is estimated to be 30 billion years. Use Kepler’s third law to find the total mass of the pair. Show all work. Possibly helpful values and equations: 1 pc = 3 x 1018 cm, 1 pc = 206,265 ...
Lecture 13
... a nonnegligible fraction of the speed of light, the previous formulation is only a firstorder approximation Derivation requires special relativity, due to time dilation. We will just use the result, for a light emitter moving a speed v away from an observer, that: ...
... a nonnegligible fraction of the speed of light, the previous formulation is only a firstorder approximation Derivation requires special relativity, due to time dilation. We will just use the result, for a light emitter moving a speed v away from an observer, that: ...
The Cycle of Star Formation
... Star Forming Regions in the Infrared Due to the friction in the disk, matter flows onto the star. As the star’s mass increases, its core grows hotter. At this time, since the star is still surrounded by dust, it is invisible in the optical. But the heat from the star begins to warm the dust. ...
... Star Forming Regions in the Infrared Due to the friction in the disk, matter flows onto the star. As the star’s mass increases, its core grows hotter. At this time, since the star is still surrounded by dust, it is invisible in the optical. But the heat from the star begins to warm the dust. ...
Stellar Remnants
... • an odd radio signal with a rapid pulse rate of one burst per 1.33 seconds • more pulsating radio sources were discovered and eventually were named pulsars • No clue what they were! ...
... • an odd radio signal with a rapid pulse rate of one burst per 1.33 seconds • more pulsating radio sources were discovered and eventually were named pulsars • No clue what they were! ...
Review Questions for Exam #2
... • In the spectra below, the temperature is the same for all three spectra. Why are the lines different strengths? ...
... • In the spectra below, the temperature is the same for all three spectra. Why are the lines different strengths? ...
Summer Triangle (Winter in the south hemisphere) Lyra
... Lyra, the Harp, is a small constellation with a very recognizable shape. It is one of the few constellations that actually resembles the object for which it is named. Lyra is located between Hercules 武仙座 and Cygnus 天鵝座, and is best seen from May through November. Lyra includes the brilliant star Veg ...
... Lyra, the Harp, is a small constellation with a very recognizable shape. It is one of the few constellations that actually resembles the object for which it is named. Lyra is located between Hercules 武仙座 and Cygnus 天鵝座, and is best seen from May through November. Lyra includes the brilliant star Veg ...
Life Cycle of a Star
... • The core shrinks and the outer parts expand • It turns red as it is cooling • This phase will last until the star exhausts its remaining fuel. • The pressure of the nuclear reaction is not strong enough to equalize the force of gravity so the star will collapse. ...
... • The core shrinks and the outer parts expand • It turns red as it is cooling • This phase will last until the star exhausts its remaining fuel. • The pressure of the nuclear reaction is not strong enough to equalize the force of gravity so the star will collapse. ...
Star formation slides
... T-Tauri was the first star of a type found to have both disks and jet outflows… … and we know star formation in a fragmenting parent cloud is a complex process, involving competing mass-accretion & mass-loss processes ...
... T-Tauri was the first star of a type found to have both disks and jet outflows… … and we know star formation in a fragmenting parent cloud is a complex process, involving competing mass-accretion & mass-loss processes ...
NOVAE and SUPERNOVAE
... of energy. Novae are caused by the transfer of matter onto a white dwarf within a binary system from a companion star, which has overfilled its Roche lobe. This transferred matter first orbits the WD in an accretion disk, a flattened, rotating structure surrounding the white dwarf. Matter grad ...
... of energy. Novae are caused by the transfer of matter onto a white dwarf within a binary system from a companion star, which has overfilled its Roche lobe. This transferred matter first orbits the WD in an accretion disk, a flattened, rotating structure surrounding the white dwarf. Matter grad ...
Life Cycle of a Star
... • The core shrinks and the outer parts expand • It turns red as it is cooling • This phase will last until the star exhausts its remaining fuel. • The pressure of the nuclear reaction is not strong enough to equalize the force of gravity so the star will collapse. ...
... • The core shrinks and the outer parts expand • It turns red as it is cooling • This phase will last until the star exhausts its remaining fuel. • The pressure of the nuclear reaction is not strong enough to equalize the force of gravity so the star will collapse. ...
Astronomy 102, Spring 2003 Solutions to Review Problems
... star is older? Which star started its life with more mass? Given that we’ve talked about how far apart stars are in the galaxy, they almost never run into each other. (It’s a different matter in the cores of globular clusters, and even right at the center of our galaxy, but consider the Solar neighb ...
... star is older? Which star started its life with more mass? Given that we’ve talked about how far apart stars are in the galaxy, they almost never run into each other. (It’s a different matter in the cores of globular clusters, and even right at the center of our galaxy, but consider the Solar neighb ...
Sco
... It may grow larger as time goes Distance between the stars at periastron is d = 24 R1 Primary’s Roche lobe size ~ 0.6 d or ~ 15 R1 Consequences: Some disk material may flow into the secondary’s Roche lobe Disk may become denser and line emission will rise Single- or triple-peak profiles may be obser ...
... It may grow larger as time goes Distance between the stars at periastron is d = 24 R1 Primary’s Roche lobe size ~ 0.6 d or ~ 15 R1 Consequences: Some disk material may flow into the secondary’s Roche lobe Disk may become denser and line emission will rise Single- or triple-peak profiles may be obser ...
Today`s Powerpoint
... If core with about 3 MSun or more collapses, not even neutron pressure can stop it (total mass of star about 25 MSun). Core collapses to a point, a "singularity". Gravity is so strong that nothing can escape, not even light => black hole. Schwarzschild radius for Earth is 1 cm. For a 3 MSun object, ...
... If core with about 3 MSun or more collapses, not even neutron pressure can stop it (total mass of star about 25 MSun). Core collapses to a point, a "singularity". Gravity is so strong that nothing can escape, not even light => black hole. Schwarzschild radius for Earth is 1 cm. For a 3 MSun object, ...
dtu7ech13 - Fort Thomas Independent Schools
... The Crab’s visible flashes and X-ray pulses have identical periods of 0.033 seconds. ...
... The Crab’s visible flashes and X-ray pulses have identical periods of 0.033 seconds. ...
Day 1212
... A supernova is a gigantic explosion in which the temperature in the collapsing core reaches 10 billion K and atomic nuclei are split into neutrons and protons. When very massive stars, with masses greater than 25 times that of the Sun, collapse past the neutron-star stage, they form a black hole. ...
... A supernova is a gigantic explosion in which the temperature in the collapsing core reaches 10 billion K and atomic nuclei are split into neutrons and protons. When very massive stars, with masses greater than 25 times that of the Sun, collapse past the neutron-star stage, they form a black hole. ...
ASTR 300 Stars and Stellar Systems Spring 2011
... 2. The parallax of the bright star Vega is 0.129 seconds of arc. What is the distance of Vega in parsecs ? In light-years ? We have the relation d(pc) = 1/p(arcsec) so the distance to Vega is d = 1/0.129 = 7.752 parsecs. One parsec = 3.26 light-years, so d = 3.26 × 7.753 = 25.3 ly. By how much, duri ...
... 2. The parallax of the bright star Vega is 0.129 seconds of arc. What is the distance of Vega in parsecs ? In light-years ? We have the relation d(pc) = 1/p(arcsec) so the distance to Vega is d = 1/0.129 = 7.752 parsecs. One parsec = 3.26 light-years, so d = 3.26 × 7.753 = 25.3 ly. By how much, duri ...
Test 2, Nov. 17, 2015 - Physics@Brock
... (d) [No comparison of their surface temperatures can be made.] 16. A photon can be absorbed by an atom only if the photon energy is equal to the energy difference of two atomic energy levels. (a) True. (b) False. 17. Star Betelgeuse in Orion is 120,000 times more luminous than the Sun, yet its surfa ...
... (d) [No comparison of their surface temperatures can be made.] 16. A photon can be absorbed by an atom only if the photon energy is equal to the energy difference of two atomic energy levels. (a) True. (b) False. 17. Star Betelgeuse in Orion is 120,000 times more luminous than the Sun, yet its surfa ...
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.