a description of planets and stars you may see
... third-largest member of the Local Group of galaxies, which includes the Milky Way Galaxy, the Andromeda Galaxy. It is one of the most distant permanent objects that can be viewed with the naked eye. The Ring nebula (also known as M57) is a planetary nebula is located in the constellation of Lyra. It ...
... third-largest member of the Local Group of galaxies, which includes the Milky Way Galaxy, the Andromeda Galaxy. It is one of the most distant permanent objects that can be viewed with the naked eye. The Ring nebula (also known as M57) is a planetary nebula is located in the constellation of Lyra. It ...
Stars - HMXEarthScience
... Sequence” star during which size, the star grows in size as it uses up its fuel 5. Eventually when the hydrogen fuel becomes exhausted, the star expands greatly becoming a giant or a supergiant ...
... Sequence” star during which size, the star grows in size as it uses up its fuel 5. Eventually when the hydrogen fuel becomes exhausted, the star expands greatly becoming a giant or a supergiant ...
Slayt 1
... However, as a gas temperature goes up, the average speed of the particles goes up and the protons get closer before repelling one another. If the proton get very close, the short-range nuclear force ...
... However, as a gas temperature goes up, the average speed of the particles goes up and the protons get closer before repelling one another. If the proton get very close, the short-range nuclear force ...
Stellar Evolution Notes
... A galaxy is a group of hundreds of billions of stars that are relatively close to each other. Our galaxy, the Milky Way, contains over 100 billion stars. The universe has more than 100 billion galaxies with each galaxy containing an average of 100 billion stars. ...
... A galaxy is a group of hundreds of billions of stars that are relatively close to each other. Our galaxy, the Milky Way, contains over 100 billion stars. The universe has more than 100 billion galaxies with each galaxy containing an average of 100 billion stars. ...
Stellar Evolution Notes
... A galaxy is a group of hundreds of billions of stars that are relatively close to each other. Our galaxy, the Milky Way, contains over 100 billion stars. The universe has more than 100 billion galaxies with each galaxy containing an average of 100 billion stars. ...
... A galaxy is a group of hundreds of billions of stars that are relatively close to each other. Our galaxy, the Milky Way, contains over 100 billion stars. The universe has more than 100 billion galaxies with each galaxy containing an average of 100 billion stars. ...
Planetary Nebula
... Credit: Bruce Balick (U. Washington) et al., HST, NASA • After a star like the Sun completes fusion in its core, it throws off its outer layers in a brief, beautiful cosmic display called a planetary nebula. NGC 3242 is such a planetary nebula, with the stellar remnant white dwarf star visible at th ...
... Credit: Bruce Balick (U. Washington) et al., HST, NASA • After a star like the Sun completes fusion in its core, it throws off its outer layers in a brief, beautiful cosmic display called a planetary nebula. NGC 3242 is such a planetary nebula, with the stellar remnant white dwarf star visible at th ...
Stars and Deep Time
... • A star like the Sun will eventually explode to be a brief “Nova” (bright for several weeks or months) ...
... • A star like the Sun will eventually explode to be a brief “Nova” (bright for several weeks or months) ...
8-3-Star_Classification STUDENT
... able to know what the school looked like from a distance? Of course not. All you could do is look out the windows and get some view of part of the building. If you looked out enough windows you might get a general idea but you could never know for sure if you were right about all its features. ...
... able to know what the school looked like from a distance? Of course not. All you could do is look out the windows and get some view of part of the building. If you looked out enough windows you might get a general idea but you could never know for sure if you were right about all its features. ...
PPT
... White Dwarfs are supported by electron degeneracy pressure • in a low-mass star, Fusion stops after He -->C and O • Just cools off and fizzles out ...
... White Dwarfs are supported by electron degeneracy pressure • in a low-mass star, Fusion stops after He -->C and O • Just cools off and fizzles out ...
1” “Sky-Notes” of the Open University Astronomy Club. October 2005
... about 25. Unfortunately a 17 day old Moon interferes. The long lasting Taurids commence activity on the 20th with activity continuing until 30th November. Bright but slow moving meteors. Don’t forget the potential spectacle of bright sporadic events. If you are fortunate enough to observe a very fir ...
... about 25. Unfortunately a 17 day old Moon interferes. The long lasting Taurids commence activity on the 20th with activity continuing until 30th November. Bright but slow moving meteors. Don’t forget the potential spectacle of bright sporadic events. If you are fortunate enough to observe a very fir ...
Document
... and cools forming a red giant Step 6: Once the red giant is unable to support itself the outer layers will come off forming a planetary nebula and the super heated core of the star will remain which is a white dwarf 6. Explain why stars appear to move in the night sky. (MC) Because Earth moves 7. Un ...
... and cools forming a red giant Step 6: Once the red giant is unable to support itself the outer layers will come off forming a planetary nebula and the super heated core of the star will remain which is a white dwarf 6. Explain why stars appear to move in the night sky. (MC) Because Earth moves 7. Un ...
http://hcs.harvard.edu/~jus/0302/bester.pdf
... On July 4, 1054, a Chinese peasant and amateur astronomer may have looked up from his or her rice field to witness a spectacular stellar event. A bright object appeared suddenly and continued to shine its inexplicable light in the terrestrial sky for almost two years. The remnant of this explosion i ...
... On July 4, 1054, a Chinese peasant and amateur astronomer may have looked up from his or her rice field to witness a spectacular stellar event. A bright object appeared suddenly and continued to shine its inexplicable light in the terrestrial sky for almost two years. The remnant of this explosion i ...
Stellar Evolution
... • Mass of Sun • Radius of Earth • Hot as Sun’s core • A million times denser than lead • Slowly cool off ...
... • Mass of Sun • Radius of Earth • Hot as Sun’s core • A million times denser than lead • Slowly cool off ...
Stars
... • Then, star collapses under the weight and because it is electron degenerate, energy created will not expand the star and shut off the fusion. • So, entire star (carbon, mostly) undergoes fusion at once. What a star normally takes billions of years to burn, this star burns all at once. BIG explosio ...
... • Then, star collapses under the weight and because it is electron degenerate, energy created will not expand the star and shut off the fusion. • So, entire star (carbon, mostly) undergoes fusion at once. What a star normally takes billions of years to burn, this star burns all at once. BIG explosio ...
Lives and Deaths of Stars (middle school)
... Contraction stops when the gravity is balanced by thermal pressure Stars are held together by gravity. Gravity tries to compress everything to the center. What holds an ordinary star up and prevents total collapse is thermal and radiation pressure. The thermal and radiation pressure tries to expand ...
... Contraction stops when the gravity is balanced by thermal pressure Stars are held together by gravity. Gravity tries to compress everything to the center. What holds an ordinary star up and prevents total collapse is thermal and radiation pressure. The thermal and radiation pressure tries to expand ...
The Life Cycle of Stars
... As core contracts further->pressure rise->helium-rich core begins to undergo fusion->produces heavier elements, such as carbon->as it expands, it sends gas and dust into space and begins to lose mass->caused it to move off the main sequence band. ...
... As core contracts further->pressure rise->helium-rich core begins to undergo fusion->produces heavier elements, such as carbon->as it expands, it sends gas and dust into space and begins to lose mass->caused it to move off the main sequence band. ...
Deep Space Mystery Note Form 3
... The core could have temperatures of billions of degrees Celsius. Iron atoms are so squeezed so much. The forces of their nuclei create a recoil of the squeezed core. Then is the supernova. Type II Type II Binary stars are when there are two stars and they revolve around each other. In ...
... The core could have temperatures of billions of degrees Celsius. Iron atoms are so squeezed so much. The forces of their nuclei create a recoil of the squeezed core. Then is the supernova. Type II Type II Binary stars are when there are two stars and they revolve around each other. In ...
Powerpoint for today
... Explanation: "beamed" radiation from rapidly spinning neutron star. Usually neutron stars are pulsars for 107 years after supernova. ...
... Explanation: "beamed" radiation from rapidly spinning neutron star. Usually neutron stars are pulsars for 107 years after supernova. ...
Constellation
... pearls' surrounding an Exploding Star Two decades ago, astronomers spotted one of the brightest exploding stars in more than 400 years. This image shows the entire region around the supernova. The most prominent feature in the image is a ring with dozens of bright spots. A shock wave of material unl ...
... pearls' surrounding an Exploding Star Two decades ago, astronomers spotted one of the brightest exploding stars in more than 400 years. This image shows the entire region around the supernova. The most prominent feature in the image is a ring with dozens of bright spots. A shock wave of material unl ...
Life cycle of a star
... cools and dims. When it stops shining, the now dead star is called a Black Dwarf. ...
... cools and dims. When it stops shining, the now dead star is called a Black Dwarf. ...
Sample exam 2
... 13. Suppose you are looking at the emission spectrum of gaseous helium. You dutifully write down the wavelengths of emission. You notice a power dial on the side of emission lamp and, just for fun, decide to turn up the power. The color of the helium lamp changes and you look through the spectroscop ...
... 13. Suppose you are looking at the emission spectrum of gaseous helium. You dutifully write down the wavelengths of emission. You notice a power dial on the side of emission lamp and, just for fun, decide to turn up the power. The color of the helium lamp changes and you look through the spectroscop ...
CAPSTONE-poster
... Our team decided to explore planetary nebulae because we wanted to know how were they formed, why they had so many colors, why they were called planetary nebulae, the significance of their names, their composition, how many possibly existed in the Milky Way galaxy, their approximate age, their first ...
... Our team decided to explore planetary nebulae because we wanted to know how were they formed, why they had so many colors, why they were called planetary nebulae, the significance of their names, their composition, how many possibly existed in the Milky Way galaxy, their approximate age, their first ...
stars - allenscience
... massive explosion called a Supernova. The end result is also a planetary nebula. Supernova are so bright that they can outshine an entire galaxy for a period of time. ...
... massive explosion called a Supernova. The end result is also a planetary nebula. Supernova are so bright that they can outshine an entire galaxy for a period of time. ...
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.