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Document
... working with a group of English astronomers, discovered a periodic signal in the radio part of the spectrum, coming from a distant galaxy. • Astronomers considered (briefly) the possibility of an alien civilization sending the regular pulses. ...
... working with a group of English astronomers, discovered a periodic signal in the radio part of the spectrum, coming from a distant galaxy. • Astronomers considered (briefly) the possibility of an alien civilization sending the regular pulses. ...
April11
... • If a white dwarf is in orbit around a red giant companion star, it can pull material off the companion and into an accretion disk around itself • Material in the accretion disk eventually falls to the surface of the white dwarf ...
... • If a white dwarf is in orbit around a red giant companion star, it can pull material off the companion and into an accretion disk around itself • Material in the accretion disk eventually falls to the surface of the white dwarf ...
Stars - Red, Blue, Old, New pt.4
... • The star gets to the point where it has a carbon core. • Core collapses but not hot enough to initiate carbon to oxygen fusion. • Most of star’s mass collapses to “degenerate matter” and star becomes a white dwarf. • Outer layers escape in a “planetary nebula”. ...
... • The star gets to the point where it has a carbon core. • Core collapses but not hot enough to initiate carbon to oxygen fusion. • Most of star’s mass collapses to “degenerate matter” and star becomes a white dwarf. • Outer layers escape in a “planetary nebula”. ...
The Fate of Massive Stars
... various Ions (including Fe) in stellar atmosphere Diagonal upper-luminosity cutoff that is temperature dependent Hotter --> Higher Luminosity cutoff Greater mass-loss/stellar winds for cooler stars at lower luminosities Stellar winds important contribution to ISM Massive Stars ability to quench star ...
... various Ions (including Fe) in stellar atmosphere Diagonal upper-luminosity cutoff that is temperature dependent Hotter --> Higher Luminosity cutoff Greater mass-loss/stellar winds for cooler stars at lower luminosities Stellar winds important contribution to ISM Massive Stars ability to quench star ...
Lec 25.2- STELLAR EVOLUTION SUMMARY
... also pulsate in X-ray and other wavelengths. . The pulsar's beams probably do not turn on and off. Instead, the energy is believed to be emitted from a point on the start hat faces toward and away from Earth as the star spins, somewhat like the effect of the rotating beacon of a lighthouse. The only ...
... also pulsate in X-ray and other wavelengths. . The pulsar's beams probably do not turn on and off. Instead, the energy is believed to be emitted from a point on the start hat faces toward and away from Earth as the star spins, somewhat like the effect of the rotating beacon of a lighthouse. The only ...
NOVAE and SUPERNOVAE
... The expanding remains of Type I supernova should contain no hydrogen, a prediction met by observations of the spectra of such remnants. These remnants will contain about 1.4 solar masses of iron and nickel. Type II supernova remnants contain a great deal of hydrogen – the ejected outer layers of the ...
... The expanding remains of Type I supernova should contain no hydrogen, a prediction met by observations of the spectra of such remnants. These remnants will contain about 1.4 solar masses of iron and nickel. Type II supernova remnants contain a great deal of hydrogen – the ejected outer layers of the ...
Irregular Galaxies
... iron atoms into new elements. • Huge clouds of dust, gas, and the new elements explode into space. • This forms a new nebula. • Once a star supernovas, the core that remains of it will become either a neutron star or a black hole. ...
... iron atoms into new elements. • Huge clouds of dust, gas, and the new elements explode into space. • This forms a new nebula. • Once a star supernovas, the core that remains of it will become either a neutron star or a black hole. ...
Activity: Stellar Evolution Scavenger Hunt - Chandra X
... The two clusters (known as NGC 884 and NGC 869) are strikingly similar in many ways and are believed to have originated from a single ancestral gas cloud some 12.8 million years ago. ...
... The two clusters (known as NGC 884 and NGC 869) are strikingly similar in many ways and are believed to have originated from a single ancestral gas cloud some 12.8 million years ago. ...
Life Cycle of a Star - Intervention Worksheet
... After a low or medium mass or star becomes a red giant, the outer parts grow bigger and drift into space, forming a cloud of gas called a planetary nebula. The blue-white hot core of the star that is left behind cools and becomes a white dwarf. The white dwarf eventually runs out of fuel and dies as ...
... After a low or medium mass or star becomes a red giant, the outer parts grow bigger and drift into space, forming a cloud of gas called a planetary nebula. The blue-white hot core of the star that is left behind cools and becomes a white dwarf. The white dwarf eventually runs out of fuel and dies as ...
Stellar Evolution
... per cubic centimeter (in English about 30 billion trillion). Most solids and liquids have similar numbers. At the earth’s surface our atmosphere has about 2.4 x 1019 molecules per cubic centimeter (about a thousand times less dense than liquid water). In most of interstellar space, there is about 1 ...
... per cubic centimeter (in English about 30 billion trillion). Most solids and liquids have similar numbers. At the earth’s surface our atmosphere has about 2.4 x 1019 molecules per cubic centimeter (about a thousand times less dense than liquid water). In most of interstellar space, there is about 1 ...
Solutions
... The right side integration is trivial. The left side gives 1/3T3 evaluated from Ti to Tf which works out to be 1/3Tf3. Simple algebra gives you the desired formula. d (5 points) How many years are needed for a one solar mass white dwarf with the radius of the Earth to cool to Tf=1500K? ...
... The right side integration is trivial. The left side gives 1/3T3 evaluated from Ti to Tf which works out to be 1/3Tf3. Simple algebra gives you the desired formula. d (5 points) How many years are needed for a one solar mass white dwarf with the radius of the Earth to cool to Tf=1500K? ...
October 2011
... bang, they should be slowing down due to their mutual gravitational pull. A supernova 1A is a special type of supernova. Each one follows a pattern which results in the same brightness at the source as a function of time. By observing the brightness on earth, the distance to the nova can be calculat ...
... bang, they should be slowing down due to their mutual gravitational pull. A supernova 1A is a special type of supernova. Each one follows a pattern which results in the same brightness at the source as a function of time. By observing the brightness on earth, the distance to the nova can be calculat ...
UNIT 4 - Rowan County Schools
... The Crab Nebula (M1) • The crab nebula is a supernova remnant (SNR) • A SNR is the expanding shell of gas that is ejected into space after a massive star reaches the end of it’s life and explodes. • The Crab nebula exploded in 1054 AD. It was observed by the Chinese and Arabs and was known to the C ...
... The Crab Nebula (M1) • The crab nebula is a supernova remnant (SNR) • A SNR is the expanding shell of gas that is ejected into space after a massive star reaches the end of it’s life and explodes. • The Crab nebula exploded in 1054 AD. It was observed by the Chinese and Arabs and was known to the C ...
PHYS3380_102615_bw
... We have observed disks around other stars. These could be new planetary systems in formation. ...
... We have observed disks around other stars. These could be new planetary systems in formation. ...
Stellar Evolution
... eventually run out of fuel and collapse due to gravity Low Mass Stars – consume fuel at a slow rate, may remain on main-sequence for up to 100 billion years, end up collapsing into white dwarfs Medium Mass Stars – go into red-giant stage, followed by collapse to white dwarf by blowing out their oute ...
... eventually run out of fuel and collapse due to gravity Low Mass Stars – consume fuel at a slow rate, may remain on main-sequence for up to 100 billion years, end up collapsing into white dwarfs Medium Mass Stars – go into red-giant stage, followed by collapse to white dwarf by blowing out their oute ...
Document
... The ash of one reaction, becomes the fuel of the next. • Fusion takes place in the core as long as the ...
... The ash of one reaction, becomes the fuel of the next. • Fusion takes place in the core as long as the ...
Star Cycle2013
... _____________ that marks the end of a very massive star’s life. When it occurs, the exploding star can outshine all of the other stars in the galaxy in total for several days and may leave behind only a crushed core. ...
... _____________ that marks the end of a very massive star’s life. When it occurs, the exploding star can outshine all of the other stars in the galaxy in total for several days and may leave behind only a crushed core. ...
Properties of Supernovae
... small diameter. This implosion causes a shock which bounces off the core, resulting in an explosion which we see as a Type II supernova. The shock carries of a large fraction of the stellar atmosphere at speeds of 13,000-30,000 km/s. In this exercise, you will study three supernovae: ...
... small diameter. This implosion causes a shock which bounces off the core, resulting in an explosion which we see as a Type II supernova. The shock carries of a large fraction of the stellar atmosphere at speeds of 13,000-30,000 km/s. In this exercise, you will study three supernovae: ...
AST301.Ch21.StellarExpl - University of Texas Astronomy
... Here is an image of the Cas A SNR in X-rays (left) and at radio wavelengths (right). The X-rays are emitted because the gas is so hot (~ million degrees K), while the radio emission is from electrons that are gyrating at nearly the speed of light around the strong magnetic field in the remnant—this ...
... Here is an image of the Cas A SNR in X-rays (left) and at radio wavelengths (right). The X-rays are emitted because the gas is so hot (~ million degrees K), while the radio emission is from electrons that are gyrating at nearly the speed of light around the strong magnetic field in the remnant—this ...
Evolution Cycle of Stars
... Sun's diameter; approximately the diameter of the Earth. The surface temperature of a white dwarf is 8000C or more, but being smaller than the Sun their overall luminosity's are 1% of the Sun or less. • White dwarfs are the shrunken remains of normal stars, whose nuclear energy supplies have been us ...
... Sun's diameter; approximately the diameter of the Earth. The surface temperature of a white dwarf is 8000C or more, but being smaller than the Sun their overall luminosity's are 1% of the Sun or less. • White dwarfs are the shrunken remains of normal stars, whose nuclear energy supplies have been us ...
The Birth of Stars
... The formation of planets occurs at the same time as the formation of stars ...
... The formation of planets occurs at the same time as the formation of stars ...
The star
... It is three thousand light years to the Vatican. Once, I believed that space could have no power over faith, just as I believed that the heavens declared the glory of God’s handiwork. Now I have seen that handiwork, and my faith is sorely troubled. I stare at the crucifix that hangs on the cabin wal ...
... It is three thousand light years to the Vatican. Once, I believed that space could have no power over faith, just as I believed that the heavens declared the glory of God’s handiwork. Now I have seen that handiwork, and my faith is sorely troubled. I stare at the crucifix that hangs on the cabin wal ...
Life Cycle of a Star notes
... release of gravitational energy, it is not yet hot enough to produce nuclear reactions within its center. ...
... release of gravitational energy, it is not yet hot enough to produce nuclear reactions within its center. ...
File
... The passing fires had seared its rocks and burned away the mantle of frozen gas that must have covered it in the days before the disaster. We landed, and we found the Vault. Its builders had made sure that we would. The monolithic marker that stood above the entrance was now a fused stump, but even ...
... The passing fires had seared its rocks and burned away the mantle of frozen gas that must have covered it in the days before the disaster. We landed, and we found the Vault. Its builders had made sure that we would. The monolithic marker that stood above the entrance was now a fused stump, but even ...
Crab Nebula
![](https://en.wikipedia.org/wiki/Special:FilePath/Crab_Nebula.jpg?width=300)
The Crab Nebula (catalogue designations M1, NGC 1952, Taurus A) is a supernova remnant and pulsar wind nebula in the constellation of Taurus. It is not, as its name might suggest, in Cancer. The now-current name is due to William Parsons, 3rd Earl of Rosse, who observed the object in 1840 using a 36-inch telescope and produced a drawing that looked somewhat like a crab. Corresponding to a bright supernova recorded by Chinese astronomers in 1054, the nebula was observed later by English astronomer John Bevis in 1731. The nebula was the first astronomical object identified with a historical supernova explosion.At an apparent magnitude of 8.4, comparable to that of Saturn's moon Titan, it is not visible to the naked eye but can be made out using binoculars under favourable conditions. The nebula lies in the Perseus Arm of the Milky Way galaxy, at a distance of about 2.0 kiloparsecs (6,500 ly) from Earth. It has a diameter of 3.4 parsecs (11 ly), corresponding to an apparent diameter of some 7 arcminutes, and is expanding at a rate of about 1,500 kilometres per second (930 mi/s), or 0.5% c.At the center of the nebula lies the Crab Pulsar, a neutron star 28–30 kilometres (17–19 mi) across with a spin rate of 30.2 times per second, which emits pulses of radiation from gamma rays to radio waves. At X-ray and gamma ray energies above 30 keV, the Crab is generally the strongest persistent source in the sky, with measured flux extending to above 10 TeV. The nebula's radiation allows for the detailed studying of celestial bodies that occult it. In the 1950s and 1960s, the Sun's corona was mapped from observations of the Crab's radio waves passing through it, and in 2003, the thickness of the atmosphere of Saturn's moon Titan was measured as it blocked out X-rays from the nebula.