Open Houses at the Campus Observatory Astronomical Horizons Lecture
... Electron degeneracy pressure goes away because electrons combine with protons, making neutrons and neutrinos Neutrons collapse to the center, forming a neutron ...
... Electron degeneracy pressure goes away because electrons combine with protons, making neutrons and neutrinos Neutrons collapse to the center, forming a neutron ...
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 ...
Chapter 18 The Interstellar Medium
... The Ophiuchus dust cloud can be seen in this image. Its shape is irregular, with streamers to the upper left. ...
... The Ophiuchus dust cloud can be seen in this image. Its shape is irregular, with streamers to the upper left. ...
THE ORION CONSTELLATION the Great Hunter
... 1. Rigel (Beta Orionis) is the brightest star in the constellation. With an apparent visual magnitude of 0.18, it is also the sixth brightest star in the sky. Rigel is really a star system composed of three stars. It has been a known visual binary since 1831, possibly even earlier, when F. G. Struve ...
... 1. Rigel (Beta Orionis) is the brightest star in the constellation. With an apparent visual magnitude of 0.18, it is also the sixth brightest star in the sky. Rigel is really a star system composed of three stars. It has been a known visual binary since 1831, possibly even earlier, when F. G. Struve ...
Exploding Massive Stars:
... ascertain the core collapse supernova mechanism(s) understand supernova phenomenology e.g.: (1) element synthesis, (2) neutrino, gravitational wave, and gamma ray signatures provide theoretical foundation in support of OS experimental facilities (RHIC, SNO, RIA, NUSL) develop enabling technolo ...
... ascertain the core collapse supernova mechanism(s) understand supernova phenomenology e.g.: (1) element synthesis, (2) neutrino, gravitational wave, and gamma ray signatures provide theoretical foundation in support of OS experimental facilities (RHIC, SNO, RIA, NUSL) develop enabling technolo ...
Pulsar properties - Pulsar Search Collaboratory
... Size of emission region is bounded by the so-called `light cylinder’ - this is an imaginary surface that co-rotates with the neutron star. Einstein asserts the co-rotation speed cannot be greater than the speed of light, c. This sets a fundamental size for the emission region. ...
... Size of emission region is bounded by the so-called `light cylinder’ - this is an imaginary surface that co-rotates with the neutron star. Einstein asserts the co-rotation speed cannot be greater than the speed of light, c. This sets a fundamental size for the emission region. ...
Full 11x8.5" Calendar, High Resolution - Chandra X
... When a star like our Sun uses up all of the hydrogen in its core, it becomes what is called a “planetary nebula.” During this stage, the star begins to cool and expand, increasing its radius by tens to hundreds of times its original size. Eventually, the outer layers of the star are swept away by a ...
... When a star like our Sun uses up all of the hydrogen in its core, it becomes what is called a “planetary nebula.” During this stage, the star begins to cool and expand, increasing its radius by tens to hundreds of times its original size. Eventually, the outer layers of the star are swept away by a ...
Lecture 10: Interstellar gas
... expands as a shell into the ISM. The expanding shell compresses and heats up the IS gas; behind the shell the gas is left hot and rarefied. • The supernova shells are large structure, a few of them hundreds of parsecs (up to 3 kpc) in diameter, these sweep through the IS gas, they heat it to about 5 ...
... expands as a shell into the ISM. The expanding shell compresses and heats up the IS gas; behind the shell the gas is left hot and rarefied. • The supernova shells are large structure, a few of them hundreds of parsecs (up to 3 kpc) in diameter, these sweep through the IS gas, they heat it to about 5 ...
The Antares Emission Nebula and Mass Loss of α Sco A
... The Antares nebula has been known as a peculiar [Fe II] emission nebula, apparently without normal H II region lines. Long-slit VLT/UVES mapping shows that it is an H II region 3 in size around the B type star A Sco B, with a Balmer line recombination spectrum and [N II] lines, but no [O II] and [O ...
... The Antares nebula has been known as a peculiar [Fe II] emission nebula, apparently without normal H II region lines. Long-slit VLT/UVES mapping shows that it is an H II region 3 in size around the B type star A Sco B, with a Balmer line recombination spectrum and [N II] lines, but no [O II] and [O ...
Planetary Nebula
... Observers have long been aware of the unique structure of planetary nebula NGC 7008. Because the central star is so prominent, the original thinking on this nebula’s formation focused around the central star itself. But the motions of the gas are also being observed and a recent study suggest that s ...
... Observers have long been aware of the unique structure of planetary nebula NGC 7008. Because the central star is so prominent, the original thinking on this nebula’s formation focused around the central star itself. But the motions of the gas are also being observed and a recent study suggest that s ...
Observing Nebulosities: The Cygnus Superbubble Chris
... The Cygnus star-forming complex is one of the largest isolated features of interstellar gas and dust recognized in the Milky Way. In the sky, it is associated with the Northern Cross asterism, the bright supergiant star Deneb and the picturesque North America and Pelican emission nebulae (Fig. 1). O ...
... The Cygnus star-forming complex is one of the largest isolated features of interstellar gas and dust recognized in the Milky Way. In the sky, it is associated with the Northern Cross asterism, the bright supergiant star Deneb and the picturesque North America and Pelican emission nebulae (Fig. 1). O ...
FASTER THAN THE SPEED OF LIGHT
... Orion nebula: The Advanced Camera for Surveys - Wide Field and Planetary Camera 2 - Near Infrared Camera - MultiObject Spectrometer. The Hubble telescope took 520 images of the Orion nebula as it made 105 orbits around the earth. The images were taken in five colors, to make this picture. They also ...
... Orion nebula: The Advanced Camera for Surveys - Wide Field and Planetary Camera 2 - Near Infrared Camera - MultiObject Spectrometer. The Hubble telescope took 520 images of the Orion nebula as it made 105 orbits around the earth. The images were taken in five colors, to make this picture. They also ...
View the sky`s greatest nebula
... lies roughly 10' north of M42. This section features a hot, bright star (center) that is ionizing the gas near it. This creates a sphere of glowing hydrogen, which appears pink. This image was shot through a 20-inch RC Optical Systems RitcheyChrétien telescope at f/8.4 with an SBIG ST10XME CCD camer ...
... lies roughly 10' north of M42. This section features a hot, bright star (center) that is ionizing the gas near it. This creates a sphere of glowing hydrogen, which appears pink. This image was shot through a 20-inch RC Optical Systems RitcheyChrétien telescope at f/8.4 with an SBIG ST10XME CCD camer ...
L5 Protoplanetary disks Part I
... The rotation, density, temperature in the protoplanetary disk are very important for the formation of planets: They are the initial and boundary conditions of planet formation. From what we have seen, protoplanetary disks are generally believed to have relatively small mass, typically a few percents ...
... The rotation, density, temperature in the protoplanetary disk are very important for the formation of planets: They are the initial and boundary conditions of planet formation. From what we have seen, protoplanetary disks are generally believed to have relatively small mass, typically a few percents ...
English Summary
... that time about the existence of stars, planets, comets, but also about some objects which had a nebulous appearance. Telescopes at that time were not able to reveal their nature. Charles Messier (1730-1817) was a comet seeker and in 1784 he published a catalogue (known as the Messier Catalogue) in ...
... that time about the existence of stars, planets, comets, but also about some objects which had a nebulous appearance. Telescopes at that time were not able to reveal their nature. Charles Messier (1730-1817) was a comet seeker and in 1784 he published a catalogue (known as the Messier Catalogue) in ...
Supernovae — Oct 21 10/21/2011 • Outline
... • In the first year of the period Chih-ho, …, a guest star appeared several degrees SE of Thien-kuan. After more than a year it gradually became invisible.p550. ...
... • In the first year of the period Chih-ho, …, a guest star appeared several degrees SE of Thien-kuan. After more than a year it gradually became invisible.p550. ...
Lecture 13 - Star Formation
... • Gas is mainly hydrogen, but also contains other elements and molecules. • Density is typically around 1 atom per cubic centimeter. ...
... • Gas is mainly hydrogen, but also contains other elements and molecules. • Density is typically around 1 atom per cubic centimeter. ...
White dwarfs that crossed the Chandrasekhar limit
... matter and gathers more due to gravity. At a certain point, nuclear reaction is sparked at its core balancing the gravitational collapse and thus a star gets established. Once the star runs out of nuclear fuel, due to the crushing gravity, it violently explodes forming an outer shell and an inner co ...
... matter and gathers more due to gravity. At a certain point, nuclear reaction is sparked at its core balancing the gravitational collapse and thus a star gets established. Once the star runs out of nuclear fuel, due to the crushing gravity, it violently explodes forming an outer shell and an inner co ...
Chandra Observation of Pulsar Wind Nebula
... • The morphology of a PWN is determined by the interaction with the environment. If the pulsar – is in a low density cavity, then the structure of the PWN reflects mainly the pulsar wind geometry. – is surrounded by the SNR ejecta, the wind materials will be well confined, and the expansion of the P ...
... • The morphology of a PWN is determined by the interaction with the environment. If the pulsar – is in a low density cavity, then the structure of the PWN reflects mainly the pulsar wind geometry. – is surrounded by the SNR ejecta, the wind materials will be well confined, and the expansion of the P ...
A historical perspective on the discovery of neutron stars
... Pulsars and supernova remnants Actually very small number of pulsars have been found in a supernova remnant (SNR). SNR could contain a neutron star which is not seen as a pulsar because the radiation beam does not intersect the line of sight (CCO). Pulsars can live much longer than the SNR where th ...
... Pulsars and supernova remnants Actually very small number of pulsars have been found in a supernova remnant (SNR). SNR could contain a neutron star which is not seen as a pulsar because the radiation beam does not intersect the line of sight (CCO). Pulsars can live much longer than the SNR where th ...
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.