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Research Powerpoint - Department of Astronomy
... surveys to binary stars to the shape of dark matter halos. Pictured above are recently discovered “binary” stars. Such very wide systems are easily perturbed and possibly disrupted by passing stars and, possibly, dark-matter subhalos. The constellation of Ursa Major (top middle) contains six bright ...
... surveys to binary stars to the shape of dark matter halos. Pictured above are recently discovered “binary” stars. Such very wide systems are easily perturbed and possibly disrupted by passing stars and, possibly, dark-matter subhalos. The constellation of Ursa Major (top middle) contains six bright ...
Directed Reading Section: Characteristics of Stars
... Original content Copyright © Holt McDougal. All rights reserved. Additions and changes to the original content are the responsibility of the instructor. ...
... Original content Copyright © Holt McDougal. All rights reserved. Additions and changes to the original content are the responsibility of the instructor. ...
30-1 Directed Reading
... Original content Copyright © Holt McDougal. All rights reserved. Additions and changes to the original content are the responsibility of the instructor. ...
... Original content Copyright © Holt McDougal. All rights reserved. Additions and changes to the original content are the responsibility of the instructor. ...
Life Cycle of Stars
... and note important events. Also, ask students to predict what will happen next. 7. After all the stars are “dead,” review the sequence you have just covered. Point out which stars died first, which last. Which stars deflated and which stars exploded? What is the main difference between those stars? ...
... and note important events. Also, ask students to predict what will happen next. 7. After all the stars are “dead,” review the sequence you have just covered. Point out which stars died first, which last. Which stars deflated and which stars exploded? What is the main difference between those stars? ...
Impressions of the 27th IAU General Assembly at Rio de Janeiro
... four percent of the content of the universe. Approximately 20 percent of the content of the universe is "dark matter." That leaves more than three fourth of all content of the universe unaccounted for. This "dark energy" is unlike anything that present day science understands. It exerts a repulsive ...
... four percent of the content of the universe. Approximately 20 percent of the content of the universe is "dark matter." That leaves more than three fourth of all content of the universe unaccounted for. This "dark energy" is unlike anything that present day science understands. It exerts a repulsive ...
Word
... such as Iron and Nickel metal, will "sink" to the center of the planet. Lighter material, such as silicates, will float to the top, and as the planet cools, form a solid crust. Secondly, the molten planet will release any gases that were originally trapped in its interior. This outgassing will remov ...
... such as Iron and Nickel metal, will "sink" to the center of the planet. Lighter material, such as silicates, will float to the top, and as the planet cools, form a solid crust. Secondly, the molten planet will release any gases that were originally trapped in its interior. This outgassing will remov ...
When you look up at the night sky, thousands of objects
... Although the concept of black holes is still being investigated, scientists have several theories about how they form and affect nearby matter and energy. As extremely massive stars age, they begin to collapse. Scientists think the matter in these stars is drawn inward, creating an extremely small y ...
... Although the concept of black holes is still being investigated, scientists have several theories about how they form and affect nearby matter and energy. As extremely massive stars age, they begin to collapse. Scientists think the matter in these stars is drawn inward, creating an extremely small y ...
Stellar Masses and the Main Sequence
... τ #~ 10 Gyr = Main sequence lifetime of the Sun 1 M #~ 2 × 1033 gm = Mass of the Sun" 1 L #~ 4 × 1033 ergs/sec = Luminosity of the Sun 1 R #~ 7 × 1010 cm = Radius of the Sun Q ~ 6.3 × 1018 ergs/gm = Energy from hydrogen fusion Δm ~ 27 MeV = mass defect in hydrogen fusion Δm ~ 0.7% = percent mass ...
... τ #~ 10 Gyr = Main sequence lifetime of the Sun 1 M #~ 2 × 1033 gm = Mass of the Sun" 1 L #~ 4 × 1033 ergs/sec = Luminosity of the Sun 1 R #~ 7 × 1010 cm = Radius of the Sun Q ~ 6.3 × 1018 ergs/gm = Energy from hydrogen fusion Δm ~ 27 MeV = mass defect in hydrogen fusion Δm ~ 0.7% = percent mass ...
powerpoint
... NEBULA (cloud of gas and dust)… aka the STELLAR NURSERY • The nebula begins to contract due to gravity in response to some interstellar disturbance • One or more PROTOSTARS are formed ...
... NEBULA (cloud of gas and dust)… aka the STELLAR NURSERY • The nebula begins to contract due to gravity in response to some interstellar disturbance • One or more PROTOSTARS are formed ...
The star is moving away from earth
... The color of the star indicates that it has a size and surface temperature similar to that of the Sun. Using this information, the astronomer can conclude that the star 1.is older than the Sun. 2.will survive for several billion years. 3.is moving very quickly away from Earth. 4.has a mass similar t ...
... The color of the star indicates that it has a size and surface temperature similar to that of the Sun. Using this information, the astronomer can conclude that the star 1.is older than the Sun. 2.will survive for several billion years. 3.is moving very quickly away from Earth. 4.has a mass similar t ...
Stellar Evolution and the fate of the Solar System
... YUV420 codec decompressor are needed to see this picture. ...
... YUV420 codec decompressor are needed to see this picture. ...
HST Paα Survey of the Galactic Center – Seeking the Missing
... Fig. 6 compares the magnitude distribution in 1.9µm with a stellar population synthesis model. This comparison shows that the overall shape of the distribution can be reasonably modelled with a constant star formation rate, plus a major burst about 350 Myr ago. The large deviation of the distributio ...
... Fig. 6 compares the magnitude distribution in 1.9µm with a stellar population synthesis model. This comparison shows that the overall shape of the distribution can be reasonably modelled with a constant star formation rate, plus a major burst about 350 Myr ago. The large deviation of the distributio ...
Supernovae
... Type II: More massive, so when Si-burning begins, star shrinks very rapidly 8 < M star < 15 M → Neutron Star 15 M < Mstar → Black Hole ...
... Type II: More massive, so when Si-burning begins, star shrinks very rapidly 8 < M star < 15 M → Neutron Star 15 M < Mstar → Black Hole ...
THE NUMBER OF HABITABLE PLANETS IN THE MILKY WAY
... of the central star mass and the age of the corresponding planetary system [5]. In previous studies climatic constraints, e.g. the presence of liquid water at the planetary surface, have been used to assess the habitability of terrestrial planets around different types of stars [3]. Our method [6] d ...
... of the central star mass and the age of the corresponding planetary system [5]. In previous studies climatic constraints, e.g. the presence of liquid water at the planetary surface, have been used to assess the habitability of terrestrial planets around different types of stars [3]. Our method [6] d ...
The Hubble Space Telescope
... How Does Hubble Create the Images? Images come from Hubble in black and white. Colors are assigned based on chemical elements present Blue = Oxygen Red = Sulfur ...
... How Does Hubble Create the Images? Images come from Hubble in black and white. Colors are assigned based on chemical elements present Blue = Oxygen Red = Sulfur ...
White Dwarfs - Chandra X
... While still in his twenties Subrahmanyan Chandrasekhar, the Chandra X-ray Observatory's namesake, used relativity theory and quantum mechanics to show that degenerate electron pressure can do only so much. If the mass of the white dwarf becomes greater than about 1.4 times the mass of the sun—called ...
... While still in his twenties Subrahmanyan Chandrasekhar, the Chandra X-ray Observatory's namesake, used relativity theory and quantum mechanics to show that degenerate electron pressure can do only so much. If the mass of the white dwarf becomes greater than about 1.4 times the mass of the sun—called ...
The Properties of Stars
... A and the Sun, for example, are both spectral class G2 stars and have about the same luminosity L = 3.86×1026 W. On the other hand, the apparent magnitude of Alpha Centauri A is 0.1 and the apparent magnitude of the Sun is –26.8. The difference is due to the fact that the Sun is much closer to us th ...
... A and the Sun, for example, are both spectral class G2 stars and have about the same luminosity L = 3.86×1026 W. On the other hand, the apparent magnitude of Alpha Centauri A is 0.1 and the apparent magnitude of the Sun is –26.8. The difference is due to the fact that the Sun is much closer to us th ...
Unit 8 Chapter 30 Stars, Galaxies and the Universe
... Stage 3: After a star is formed it continues hydrogen fusion. Eventually the hydrogen is used up. This triggers fusion on the outside of the core. The star expands when the core temperature becomes hot enough; it starts to fuse other elements. The gases begin to blow away in bursts until a fierce ho ...
... Stage 3: After a star is formed it continues hydrogen fusion. Eventually the hydrogen is used up. This triggers fusion on the outside of the core. The star expands when the core temperature becomes hot enough; it starts to fuse other elements. The gases begin to blow away in bursts until a fierce ho ...
Lecture Notes – Stars
... become unstable. The star pulsates and ejects its outer layers. H: Planetary nebula phase – the core is exposed as a very hot white dwarf, and the ejected envelope forms a nebula which is visible for ∼ 104 yr (not long!). I: White dwarfdom – the inert carbon core is supported by degenerate electron ...
... become unstable. The star pulsates and ejects its outer layers. H: Planetary nebula phase – the core is exposed as a very hot white dwarf, and the ejected envelope forms a nebula which is visible for ∼ 104 yr (not long!). I: White dwarfdom – the inert carbon core is supported by degenerate electron ...
The Properties of Stars
... A and the Sun, for example, are both spectral class G2 stars and have about the same luminosity L = 3.86×1026 W. On the other hand, the apparent magnitude of Alpha Centauri A is 0.1 and the apparent magnitude of the Sun is –26.8. The difference is due to the fact that the Sun is much closer to us th ...
... A and the Sun, for example, are both spectral class G2 stars and have about the same luminosity L = 3.86×1026 W. On the other hand, the apparent magnitude of Alpha Centauri A is 0.1 and the apparent magnitude of the Sun is –26.8. The difference is due to the fact that the Sun is much closer to us th ...
The Life Cycles of Stars, Part I
... has nothing left to fuse (because of iron's nuclear structure, it does not permit its atoms to fuse into heavier elements) and fusion ceases. In less than a second, the star begins the final phase of its gravitational collapse. The core temperature rises to over 100 billion degrees as the iron atoms ...
... has nothing left to fuse (because of iron's nuclear structure, it does not permit its atoms to fuse into heavier elements) and fusion ceases. In less than a second, the star begins the final phase of its gravitational collapse. The core temperature rises to over 100 billion degrees as the iron atoms ...
On the importance of nucleation for the formation of quark cores
... is formed. (F. Weber, 2000) ...
... is formed. (F. Weber, 2000) ...
Disk Galaxies: Structural Components
... • Collapse of an over-dense region of space (containing more gas and dark matter than average) under gravity • Disks are produced as the cloud of material spins faster and faster as the gravitational collapse progresses • To conserve angular momentum, the spin speed must increase inversely proportio ...
... • Collapse of an over-dense region of space (containing more gas and dark matter than average) under gravity • Disks are produced as the cloud of material spins faster and faster as the gravitational collapse progresses • To conserve angular momentum, the spin speed must increase inversely proportio ...
Lecture 12: Age, Metalicity, and Observations Abundance
... SFR(M " yr #1 ) = 7.9 $10#42 L(H% )(ergs#1 ) = 1.08 $10#53 Q(H o )(s#1 ) Q(H o ) is the ionising photon luminosity constants are derived from evol. synthesis models (e.g., Kennicutt 1982) ...
... SFR(M " yr #1 ) = 7.9 $10#42 L(H% )(ergs#1 ) = 1.08 $10#53 Q(H o )(s#1 ) Q(H o ) is the ionising photon luminosity constants are derived from evol. synthesis models (e.g., Kennicutt 1982) ...
January - WVU Planetarium - West Virginia University
... Big Dipper (Ursa Major). This is easy to do as all seven stars of the dipper are nice and bright. Once you have found this constellation, find the two stars in the side of the bowl which we will call “pointer stars ” because they point the way to the North Star. Draw an imaginary line as shown in th ...
... Big Dipper (Ursa Major). This is easy to do as all seven stars of the dipper are nice and bright. Once you have found this constellation, find the two stars in the side of the bowl which we will call “pointer stars ” because they point the way to the North Star. Draw an imaginary line as shown in th ...
Planetary nebula
![](https://commons.wikimedia.org/wiki/Special:FilePath/NGC6543.jpg?width=300)
A planetary nebula, often abbreviated as PN or plural PNe, is a kind of emission nebula consisting of an expanding glowing shell of ionized gas ejected from old red giant stars late in their lives. The word ""nebula"" is Latin for mist or cloud and the term ""planetary nebula"" is a misnomer that originated in the 1780s with astronomer William Herschel because when viewed through his telescope, these objects appeared to him to resemble the rounded shapes of planets. Herschel's name for these objects was popularly adopted and has not been changed. They are a relatively short-lived phenomenon, lasting a few tens of thousands of years, compared to a typical stellar lifetime of several billion years.A mechanism for formation of most planetary nebulae is thought to be the following: at the end of the star's life, during the red giant phase, the outer layers of the star are expelled by strong stellar winds. Eventually, after most of the red giant's atmosphere is dissipated, the exposed hot, luminous core emits ultraviolet radiation to ionize the ejected outer layers of the star. Absorbed ultraviolet light energises the shell of nebulous gas around the central star, appearing as a bright coloured planetary nebula at several discrete visible wavelengths.Planetary nebulae may play a crucial role in the chemical evolution of the Milky Way, returning material to the interstellar medium from stars where elements, the products of nucleosynthesis (such as carbon, nitrogen, oxygen and neon), have been created. Planetary nebulae are also observed in more distant galaxies, yielding useful information about their chemical abundances.In recent years, Hubble Space Telescope images have revealed many planetary nebulae to have extremely complex and varied morphologies. About one-fifth are roughly spherical, but the majority are not spherically symmetric. The mechanisms which produce such a wide variety of shapes and features are not yet well understood, but binary central stars, stellar winds and magnetic fields may play a role.