Chapter 15: The Deaths of Massive Stars
... nuclear density), the core rebounds, colliding violently with infalling material. 4. This collision between the infalling material and the rebounding core produces two effects: (a) Enough energy is produced to fuse iron into heavier elements. (b) Shock waves are sent outward that throw off the outer ...
... nuclear density), the core rebounds, colliding violently with infalling material. 4. This collision between the infalling material and the rebounding core produces two effects: (a) Enough energy is produced to fuse iron into heavier elements. (b) Shock waves are sent outward that throw off the outer ...
Far Ultraviolet Spectroscopic Explorer
... Individual objects show a variety of characteristics that do not always track the “standard model.” Collectively, SNRs can affect star formation and galactic evolution ...
... Individual objects show a variety of characteristics that do not always track the “standard model.” Collectively, SNRs can affect star formation and galactic evolution ...
astro-ph/0504597 PDF
... their occurance and schedule the observing time at the world’s largest telescopes in advance. More over they are fleeting and must be observed carefully multiple times within the first few weeks, if they are discovered after passing the peak brightness, that will be of little use as the peak brightn ...
... their occurance and schedule the observing time at the world’s largest telescopes in advance. More over they are fleeting and must be observed carefully multiple times within the first few weeks, if they are discovered after passing the peak brightness, that will be of little use as the peak brightn ...
Lives of Stars - Amazon Web Services
... that nothing, not even light, can escape. After a very massive star dies in a supernova explosion, more than five times the mass of the sun may be left. The gravity of this mass is so strong that the gas is pulled inward, packing the gas into a smaller and smaller space. The gas becomes so densely p ...
... that nothing, not even light, can escape. After a very massive star dies in a supernova explosion, more than five times the mass of the sun may be left. The gravity of this mass is so strong that the gas is pulled inward, packing the gas into a smaller and smaller space. The gas becomes so densely p ...
Death of Stars notes
... continues to contract and eventually becomes hot enough (100 million Kelvin) for helium to begin to fuse into carbon and oxygen – core helium fusion – 3 He C + energy and C + He O + energy ...
... continues to contract and eventually becomes hot enough (100 million Kelvin) for helium to begin to fuse into carbon and oxygen – core helium fusion – 3 He C + energy and C + He O + energy ...
The Ultraluminous X-ray Source in Holmberg IX and its Environment
... of 3.6 Mpc in a dwarf galaxy companion of M81. Miller (1995) discovered the nebula around the position of the X-ray source and proposed that this object was an extremely luminous supernova remnant, but the presence of X-ray variability (La Parola et al. 2001) has shown that it is a compact X-ray sou ...
... of 3.6 Mpc in a dwarf galaxy companion of M81. Miller (1995) discovered the nebula around the position of the X-ray source and proposed that this object was an extremely luminous supernova remnant, but the presence of X-ray variability (La Parola et al. 2001) has shown that it is a compact X-ray sou ...
The Southern Fall PDF - Treasures of the Southern Sky
... Lacaille during his visit to South Africa in 1751–2. It is 8500 light-years away, and the component stars are all very young. The cluster is rather more compact than the Jewel Box Cluster, and there are traces of blue reflection nebulosity associated with the brighter stars and the red emission nebu ...
... Lacaille during his visit to South Africa in 1751–2. It is 8500 light-years away, and the component stars are all very young. The cluster is rather more compact than the Jewel Box Cluster, and there are traces of blue reflection nebulosity associated with the brighter stars and the red emission nebu ...
The H-R Diagram
... field lines of a strong magnetic field • Synchrotron radiation comes out mostly as radio waves. • Running the radio pulses through a speaker makes for some interesting sounds…. Remember, pulsars spin dozens to hundreds of times per second! • YouTube link “Pulsar Sounds” ...
... field lines of a strong magnetic field • Synchrotron radiation comes out mostly as radio waves. • Running the radio pulses through a speaker makes for some interesting sounds…. Remember, pulsars spin dozens to hundreds of times per second! • YouTube link “Pulsar Sounds” ...
Orion the Hunter
... Hunter. Its brightest stars form one of the best known celestial shapes, which is visible even from cities. The plane of the Milky Way clips the northeast corner of the constellation and manifests itself as a featureless, hazy band through the neighboring constellations of Gemini and Monoceros. Or ...
... Hunter. Its brightest stars form one of the best known celestial shapes, which is visible even from cities. The plane of the Milky Way clips the northeast corner of the constellation and manifests itself as a featureless, hazy band through the neighboring constellations of Gemini and Monoceros. Or ...
Foundation 1 - Discovering Astronomy
... continues to contract and eventually becomes hot enough (100 million Kelvin) for helium to begin to fuse into carbon and oxygen – core helium fusion – 3 He C + energy and C + He O + energy ...
... continues to contract and eventually becomes hot enough (100 million Kelvin) for helium to begin to fuse into carbon and oxygen – core helium fusion – 3 He C + energy and C + He O + energy ...
RED GIANTS
... Helium fusion begins at the center of a giant • While the exterior layers expand, the helium core continues to contract and eventually becomes hot enough (100 million kelvins) for helium to begin to fuse into carbon and oxygen – core helium fusion – 3 He a C + energy and C + He a O + energy – occur ...
... Helium fusion begins at the center of a giant • While the exterior layers expand, the helium core continues to contract and eventually becomes hot enough (100 million kelvins) for helium to begin to fuse into carbon and oxygen – core helium fusion – 3 He a C + energy and C + He a O + energy – occur ...
powerpoint file
... But the next layers out that crash onto it are still nuclear fuel; they get superheated and explode as a supernova. ...
... But the next layers out that crash onto it are still nuclear fuel; they get superheated and explode as a supernova. ...
Document
... Thousands of times the mass of the Sun. Temperatures 10 – 100 K. In such a cloud: – If a star’s worth of matter should clump together in a denser region than the rest of the cloud: – Gravitational attraction will win out over their combined pressure. – The clump will begin to collapse. – The cold cl ...
... Thousands of times the mass of the Sun. Temperatures 10 – 100 K. In such a cloud: – If a star’s worth of matter should clump together in a denser region than the rest of the cloud: – Gravitational attraction will win out over their combined pressure. – The clump will begin to collapse. – The cold cl ...
Calculating the Age of a Planetary Nebula
... The object imaged by the Faulkes Telescope North for this activity was the planetary nebula (PN) commonly known as the Ghost of Jupiter nebula (NGC 3242). A planetary nebula is the remnant of a star about the size of our Sun. This star has fused all the material it can and has ended its life by puff ...
... The object imaged by the Faulkes Telescope North for this activity was the planetary nebula (PN) commonly known as the Ghost of Jupiter nebula (NGC 3242). A planetary nebula is the remnant of a star about the size of our Sun. This star has fused all the material it can and has ended its life by puff ...
W > 1 - The Open University
... the group, especially Merope. Nebula/UHC filters will help. The Hyades oc is another naked eye star cluster although more spread out than the Pleiades. The first magnitude star Aldebaran (0.9) is not a member of the cluster and appears brighter as it is closer to us, 21 parsecs - about halfway to th ...
... the group, especially Merope. Nebula/UHC filters will help. The Hyades oc is another naked eye star cluster although more spread out than the Pleiades. The first magnitude star Aldebaran (0.9) is not a member of the cluster and appears brighter as it is closer to us, 21 parsecs - about halfway to th ...
1: Properties of Pulsars
... dwarfs. Only neutron stars were left as a possible explanation. Periods for radial oscillations of neutron stars were predicted to be larger than 1 second and were hence incompatible with the periods of the first discovered pulsars. Finally, another property of pulsars, also most easily observed in ...
... dwarfs. Only neutron stars were left as a possible explanation. Periods for radial oscillations of neutron stars were predicted to be larger than 1 second and were hence incompatible with the periods of the first discovered pulsars. Finally, another property of pulsars, also most easily observed in ...
The Great Nebula in Orion
... Astronomers have little information about the wider context in which the young Solar System developed. Nevertheless, under the reasonable assumption that the Orion Nebula is a typical star-forming region, it presents astronomers with a valuable laboratory for observing star and planetary system for ...
... Astronomers have little information about the wider context in which the young Solar System developed. Nevertheless, under the reasonable assumption that the Orion Nebula is a typical star-forming region, it presents astronomers with a valuable laboratory for observing star and planetary system for ...
Lect16-3-28-and-30-1..
... recent supernova, a star that exploded in 1054. We know this date precisely, because it was recorded by the Chinese. At the center of the Crab nebula there is a pulsar, a rapidly rotating neutron star. This confirms our theoretical ideas that such objects j should remain after a supernova explosion. ...
... recent supernova, a star that exploded in 1054. We know this date precisely, because it was recorded by the Chinese. At the center of the Crab nebula there is a pulsar, a rapidly rotating neutron star. This confirms our theoretical ideas that such objects j should remain after a supernova explosion. ...
Document
... • Same thing with dust clouds in space. • Since space is full of dust, the farther away stars are, the redder they look. • Enough dust and eventually all visible light is scattered or absorbed. ...
... • Same thing with dust clouds in space. • Since space is full of dust, the farther away stars are, the redder they look. • Enough dust and eventually all visible light is scattered or absorbed. ...
Star Formation - University of Redlands
... • Same thing with dust clouds in space. • Since space is full of dust, the farther away stars are, the redder they look. • Enough dust and eventually all visible light is scattered or absorbed. ...
... • Same thing with dust clouds in space. • Since space is full of dust, the farther away stars are, the redder they look. • Enough dust and eventually all visible light is scattered or absorbed. ...
Einstein
... light is emitted by charged particles moving close to the speed of light around magnetic fields. • Emission (mostly radio) is concentrated at the magnetic poles and focused into a beam. • Whether we see a pulsar depends on the geometry. – if the polar beam sweeps by Earth’s direction once each rotat ...
... light is emitted by charged particles moving close to the speed of light around magnetic fields. • Emission (mostly radio) is concentrated at the magnetic poles and focused into a beam. • Whether we see a pulsar depends on the geometry. – if the polar beam sweeps by Earth’s direction once each rotat ...
Introduction to Astronomy
... – When fusion in a high-mass star stops, core continues contracting, but no pressure to stop it – Temperature increases so much the Iron nuclei start to break apart – Collapse pushes electrons into protons, creating bulk of neutrons at nuclear density – Rapid implosion causes material to “bounce” of ...
... – When fusion in a high-mass star stops, core continues contracting, but no pressure to stop it – Temperature increases so much the Iron nuclei start to break apart – Collapse pushes electrons into protons, creating bulk of neutrons at nuclear density – Rapid implosion causes material to “bounce” of ...
Disks around low-mass stars in extreme environments
... How to distinguish the young low-mass stars from the millions of old background stars in the field-of-view ? Solution: X-ray observations Old star ...
... How to distinguish the young low-mass stars from the millions of old background stars in the field-of-view ? Solution: X-ray observations Old star ...
Crab Nebula
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.