bYTEBoss lesson 3 life of star
... The end of the life cycle of really massive stars is different to that of massive stars. After a really massive red giant collapses in a supernova explosion, it leaves a star so dense that not even light can escape its gravitational pull. This is called a black hole! Some scientists believe that the ...
... The end of the life cycle of really massive stars is different to that of massive stars. After a really massive red giant collapses in a supernova explosion, it leaves a star so dense that not even light can escape its gravitational pull. This is called a black hole! Some scientists believe that the ...
Homework #9 (Ch. 21)
... What is the Chandrasekhar mass (or limit), and what does it have to do with supernovae? 8. Chaisson Review and Discussion 21.9 How do the mechanisms responsible for Type I and Type II supernovae explain their observed differences? ...
... What is the Chandrasekhar mass (or limit), and what does it have to do with supernovae? 8. Chaisson Review and Discussion 21.9 How do the mechanisms responsible for Type I and Type II supernovae explain their observed differences? ...
1 - Stellar Life Cycle
... it's all over, a large fraction of the star is blown into space as a supernova remnant. A typical supernova remnant is at most few light-years across. (M 1 shown) ...
... it's all over, a large fraction of the star is blown into space as a supernova remnant. A typical supernova remnant is at most few light-years across. (M 1 shown) ...
SupernovaExplosionPhysics_8pages
... rotation and magnetic fields. The crab’s neutron star is indeed a very “loud” pulsar, faithfully producing a radio burst once per revolution, every 33.3 ms. The visible-light luminosity of a typical supernova is roughly 1042 J, with a peak power of 1036 J/s = 1036 W. This is about a factor 1010 grea ...
... rotation and magnetic fields. The crab’s neutron star is indeed a very “loud” pulsar, faithfully producing a radio burst once per revolution, every 33.3 ms. The visible-light luminosity of a typical supernova is roughly 1042 J, with a peak power of 1036 J/s = 1036 W. This is about a factor 1010 grea ...
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... Complete the pre-‐lab quiz with your team. Compile a list of resources you expect to use in the lab. Work with your team to complete the lab exercises and activities. Record your results and mar ...
... Complete the pre-‐lab quiz with your team. Compile a list of resources you expect to use in the lab. Work with your team to complete the lab exercises and activities. Record your results and mar ...
Scales in the UniverseApollo
... Cat’s Eye Planetary Nebula and white dwarf (A solar mass white dwarf would be only as big as the Earth) ...
... Cat’s Eye Planetary Nebula and white dwarf (A solar mass white dwarf would be only as big as the Earth) ...
Small images
... and SWIFT satellites. These bursts did not come from star forming regions, and in fact showed all the characteristics expected of merging neutron stars. It is widely believed that merging neutron stars (and neutron stars merging with black holes) have now been observed as short hard gamma-ray bursts ...
... and SWIFT satellites. These bursts did not come from star forming regions, and in fact showed all the characteristics expected of merging neutron stars. It is widely believed that merging neutron stars (and neutron stars merging with black holes) have now been observed as short hard gamma-ray bursts ...
Stellar Evolution (Powerpoint) 17
... • Very useful – they’re all the ~same – 1.4 solar mass white dwarfs undergoing nuclear fusion. This turns out to mean they are… • GREAT “standard candles” – objects of known luminosity, on which we can then use simple math to determine their distance. • So, any SN I and its host galaxy, we can find ...
... • Very useful – they’re all the ~same – 1.4 solar mass white dwarfs undergoing nuclear fusion. This turns out to mean they are… • GREAT “standard candles” – objects of known luminosity, on which we can then use simple math to determine their distance. • So, any SN I and its host galaxy, we can find ...
A Pulsar Shot Out from a Supernova Explosion! - Chandra X
... Answer: Traveling at 2000 km/sec, it would take the pulsar 12 minutes to travel through a star like our sun (1.4 million/2000 km/sec = 700 seconds or 12 minutes). Because the density of the pulsar is over one trillion times that of our sun, it would be like a bullet traveling through a cloud in the ...
... Answer: Traveling at 2000 km/sec, it would take the pulsar 12 minutes to travel through a star like our sun (1.4 million/2000 km/sec = 700 seconds or 12 minutes). Because the density of the pulsar is over one trillion times that of our sun, it would be like a bullet traveling through a cloud in the ...
Death of massive stars
... Type II supernovae are produced by the collapse and explosion of a massive star. They die away more sharply than the Type I (about 15 days), but then their magnitude plateaus until about 100 days past their explosion. They form from Population I stars in spiral galaxies. ...
... Type II supernovae are produced by the collapse and explosion of a massive star. They die away more sharply than the Type I (about 15 days), but then their magnitude plateaus until about 100 days past their explosion. They form from Population I stars in spiral galaxies. ...
powerpoint file
... Cygnus X-1’s brightness “flickers” in a thousandth of a second. For something to blink so quickly, it must be very small, less than 200 miles in diameter. In 1971, radio astronomers measured the position of Cygnus X-1 accurately. It coincides with the giant blue star HDE 226868. Such a large star co ...
... Cygnus X-1’s brightness “flickers” in a thousandth of a second. For something to blink so quickly, it must be very small, less than 200 miles in diameter. In 1971, radio astronomers measured the position of Cygnus X-1 accurately. It coincides with the giant blue star HDE 226868. Such a large star co ...
Stellar Evolution Hertzsprung-Russell Diagram Hertzsprung
... · most stars fit in a diagonal band that runs from the upper left (hot, blue, bright stars) to the lower right (cool, red, dim stars) called the main ...
... · most stars fit in a diagonal band that runs from the upper left (hot, blue, bright stars) to the lower right (cool, red, dim stars) called the main ...
Objectives
... radiate over its entire lifetime • Supernovas outshine ALL the stars in its own galaxy COMBINED!! • May even be visible on earth during daylight hours • very rare ...
... radiate over its entire lifetime • Supernovas outshine ALL the stars in its own galaxy COMBINED!! • May even be visible on earth during daylight hours • very rare ...
The Life Cycle of a star
... • A supernova can light up the sky for weeks. • The temperature in one can reach 1,000,000,000 °C. • The supernova then either becomes a neutron star or a black hole. ...
... • A supernova can light up the sky for weeks. • The temperature in one can reach 1,000,000,000 °C. • The supernova then either becomes a neutron star or a black hole. ...
Slide 1
... than Fe are formed by addition of neutrons and then beta decay (see overlay). The s process adds one neutron at a time, the r process many at a time. Ex. of s process: 114Cd + 1n --> 115Cd --> 115In + e- + ν . ...
... than Fe are formed by addition of neutrons and then beta decay (see overlay). The s process adds one neutron at a time, the r process many at a time. Ex. of s process: 114Cd + 1n --> 115Cd --> 115In + e- + ν . ...
Life of a star - bahringcarthnoians
... A red giant is a luminous giant star in a late phase of evolution, with between half and 10 times the mass of our sun. They have a large radius (up to hundreds of times larger than our sun) and their surface temperature is 5,000° Kelvin and lower. They are yelloworange to red in colour. Red giants ...
... A red giant is a luminous giant star in a late phase of evolution, with between half and 10 times the mass of our sun. They have a large radius (up to hundreds of times larger than our sun) and their surface temperature is 5,000° Kelvin and lower. They are yelloworange to red in colour. Red giants ...
Stars
... The Nebula Hypothesis The solar system (planets, satellites, asteroids, comets, etc.) formed along with the Sun 4.5 Byr ago from the gravitational collapse of an interstellar cloud of gas and dust. The planets and Sun formed from the same reservoir of interstellar matter and are therefore composed ...
... The Nebula Hypothesis The solar system (planets, satellites, asteroids, comets, etc.) formed along with the Sun 4.5 Byr ago from the gravitational collapse of an interstellar cloud of gas and dust. The planets and Sun formed from the same reservoir of interstellar matter and are therefore composed ...
doc - University of Texas Astronomy
... lines of evidence; 1. Visible companion has mass around 25Mo. Using the known period and the primary star’s orbital speed from the radial velocity, get sum of masses, and hence mass of invisible companion: about 10Mo must be black hole (assuming theoretical calculation of neutron star/black hole m ...
... lines of evidence; 1. Visible companion has mass around 25Mo. Using the known period and the primary star’s orbital speed from the radial velocity, get sum of masses, and hence mass of invisible companion: about 10Mo must be black hole (assuming theoretical calculation of neutron star/black hole m ...
Publisher: Emily Barrosse Acquisitions Editor: Kelley Tyner
... Though the details can differ, all stars containing less than about ten times the Sun’s mass will have the same fate. As fusion exhausts the hydrogen in their centers, their internal pressure will diminish. Gravity will pull the core in, and the core will heat up again. Hydrogen will begin “burning” ...
... Though the details can differ, all stars containing less than about ten times the Sun’s mass will have the same fate. As fusion exhausts the hydrogen in their centers, their internal pressure will diminish. Gravity will pull the core in, and the core will heat up again. Hydrogen will begin “burning” ...
Document
... Only in high mass stars do we find the C-N-O cycle of nuclear fusion. In low mass stars the pressure due to gravity isn’t as high as the pressure in the core of a high mass star. Only a high mass star ends in an explosion that spreads carbon back into the gas and dust between stars. None of the abov ...
... Only in high mass stars do we find the C-N-O cycle of nuclear fusion. In low mass stars the pressure due to gravity isn’t as high as the pressure in the core of a high mass star. Only a high mass star ends in an explosion that spreads carbon back into the gas and dust between stars. None of the abov ...
Stars
... When a Type II supernova first becomes visible, the temperature of the expanding cloud of debris is so high that most radiation is emitted as ultraviolet light. As the cloud expands, its temperature drops. One week after the explosion, the temperature has fallen to 6000 K and the cloud radiates most ...
... When a Type II supernova first becomes visible, the temperature of the expanding cloud of debris is so high that most radiation is emitted as ultraviolet light. As the cloud expands, its temperature drops. One week after the explosion, the temperature has fallen to 6000 K and the cloud radiates most ...
Study Guide Ch10,11 and 12
... to explain their energy output and other characteristics. 11. Briefly relate the story of the discovery of quasars 12. Describe the current explanation of quasars and their energy sources. ...
... to explain their energy output and other characteristics. 11. Briefly relate the story of the discovery of quasars 12. Describe the current explanation of quasars and their energy sources. ...
Standard candles
... Supernovae occur when massive stars explode at the end of their lives. A white dwarf star in a binary pair with a red dwarf star steals mass from the red dwarf until it is too massive to support itself against gravity any more. Then its core collapses, starting a runaway nuclear reaction and a brigh ...
... Supernovae occur when massive stars explode at the end of their lives. A white dwarf star in a binary pair with a red dwarf star steals mass from the red dwarf until it is too massive to support itself against gravity any more. Then its core collapses, starting a runaway nuclear reaction and a brigh ...
Document
... • The result of the catastrophic collapse is the rebound and explosion of the core. • From start of collapse to now: 1 second! • Matter thrown back into the interstellar medium. • Matter rushing outwards, fuses with matter rushing inwards. • Every element after Fe is made in the instant of a superno ...
... • The result of the catastrophic collapse is the rebound and explosion of the core. • From start of collapse to now: 1 second! • Matter thrown back into the interstellar medium. • Matter rushing outwards, fuses with matter rushing inwards. • Every element after Fe is made in the instant of a superno ...
Stellar Explosions
... Material falls onto the white dwarf from its mainsequence companion When enough material has accreted, fusion can reignite very suddenly, burning off the new material Material keeps being transferred to the white dwarf, and the process repeats, as illustrated here ...
... Material falls onto the white dwarf from its mainsequence companion When enough material has accreted, fusion can reignite very suddenly, burning off the new material Material keeps being transferred to the white dwarf, and the process repeats, as illustrated here ...
History of supernova observation
The known history of supernova observation goes back to 185 CE, when, supernova SN 185 appeared, the oldest appearance of a supernova recorded by humankind. Several additional supernovae within the Milky Way galaxy have been recorded since that time, with SN 1604 being the most recent supernova to be observed in this galaxy.Since the development of the telescope, the field of supernova discovery has expanded to other galaxies. These occurrences provide important information on the distances of galaxies. Successful models of supernova behavior have also been developed, and the role of supernovae in the star formation process is now increasingly understood.