Stellar Evolution - FSU High Energy Physics
... • Stars support themselves against gravitational collapse by generating thermonuclear energy • Most stars are composed mainly of Hydrogen and thus fuse together to form Helium. ...
... • Stars support themselves against gravitational collapse by generating thermonuclear energy • Most stars are composed mainly of Hydrogen and thus fuse together to form Helium. ...
Document
... are about to form new stars. They also create the heavier elements (such as gold, silver, lead, and uranium) and distribute these as well. Their remnants generate the cosmic rays which lead to mutation and evolution in living cells. These supernovae, then, are key to the evolution of the Universe an ...
... are about to form new stars. They also create the heavier elements (such as gold, silver, lead, and uranium) and distribute these as well. Their remnants generate the cosmic rays which lead to mutation and evolution in living cells. These supernovae, then, are key to the evolution of the Universe an ...
GLY 1001 Earth Science Name:__Answers
... Red giant – A large, cool star of high luminosity, a star occupying the upper-right portion of the Hertzsprung-Russell Diagram. Reflection nebula – A relatively dense dust cloud in interstellar space that is illuminated by starlight. Spiral galaxy – A flattened, rotating galaxy with pinwheel-like ar ...
... Red giant – A large, cool star of high luminosity, a star occupying the upper-right portion of the Hertzsprung-Russell Diagram. Reflection nebula – A relatively dense dust cloud in interstellar space that is illuminated by starlight. Spiral galaxy – A flattened, rotating galaxy with pinwheel-like ar ...
Introduction to Stellar Evolution
... Half of it is radiated away as luminosity (and its more luminous than it will be When hydrogen is burning) ...
... Half of it is radiated away as luminosity (and its more luminous than it will be When hydrogen is burning) ...
The interstellar medium
... If we know the intrinsic colors of certain kinds of stars (by spectral type, for example), we can use the observed colors to determine how much they have been reddened by interstellar dust. ...
... If we know the intrinsic colors of certain kinds of stars (by spectral type, for example), we can use the observed colors to determine how much they have been reddened by interstellar dust. ...
Lecture 1
... The core collapses in less than 1 second! When it becomes too compressed, protons and electrons combine to become neutrons. However, neutrons do not want to combine, so they can support the core (at least for a short time) and the core rebounds- sending the shell exploding out into space. ...
... The core collapses in less than 1 second! When it becomes too compressed, protons and electrons combine to become neutrons. However, neutrons do not want to combine, so they can support the core (at least for a short time) and the core rebounds- sending the shell exploding out into space. ...
No Slide Title
... • And what isn’t the same (some are slower than others), we’ve been able to calibrate •Need to get extra mass onto WD => ...
... • And what isn’t the same (some are slower than others), we’ve been able to calibrate •Need to get extra mass onto WD => ...
Public outreach: any limit?
... 66 candidates selected so far (follow-up spectroscopy in course) ...
... 66 candidates selected so far (follow-up spectroscopy in course) ...
glossary - Discovery Education
... nebula and a white dwarf. parsec — a distance of 3.26 light-years; used to measure immense distances in space. planetary nebula — a ring of dust and gas blown off a red giant star after it undergoes an explosion. pulsar — a rapidly spinning neutron star that sends out pulses of radiation at regular ...
... nebula and a white dwarf. parsec — a distance of 3.26 light-years; used to measure immense distances in space. planetary nebula — a ring of dust and gas blown off a red giant star after it undergoes an explosion. pulsar — a rapidly spinning neutron star that sends out pulses of radiation at regular ...
Astronomy Learning Objectives and Study Questions for Chapter 13
... 3. Explain why the Sun will or will not ever become a nova. 4. Describe what spectral observation distinguishes a Type Ia from a Type II supernova, and briefly explain why the spectra of these objects are different. 5. Draw a neat, well labeled sketch of a rotating neutron star and explain how this ...
... 3. Explain why the Sun will or will not ever become a nova. 4. Describe what spectral observation distinguishes a Type Ia from a Type II supernova, and briefly explain why the spectra of these objects are different. 5. Draw a neat, well labeled sketch of a rotating neutron star and explain how this ...
Stages 12 to 14
... Stage 12 – Low Mass Stars The carbon rich core continues to contract and heat up. Carbon fusion requires a temperature of 500 to 600 million K. The core will contract until electron degeneracy pressure once again takes over, and contraction ends If the star is similar to the sun, the mass is too sm ...
... Stage 12 – Low Mass Stars The carbon rich core continues to contract and heat up. Carbon fusion requires a temperature of 500 to 600 million K. The core will contract until electron degeneracy pressure once again takes over, and contraction ends If the star is similar to the sun, the mass is too sm ...
08 October: Stellar life after the Main Sequence
... • Evolved stars have fused (used up) the hydrogen in their cores • The centers of these stars consist of burned out, incredibly dense cores, surrounded by shells where nuclear reactions are occurring • The outer parts of the stars get big, red, and bloated • Evolved stars move around in the upper pa ...
... • Evolved stars have fused (used up) the hydrogen in their cores • The centers of these stars consist of burned out, incredibly dense cores, surrounded by shells where nuclear reactions are occurring • The outer parts of the stars get big, red, and bloated • Evolved stars move around in the upper pa ...
protostars low mass stars intermediatemass stars red giant planetary
... When an intermediatemass star leaves the main sequence as it runs out of hydrogen, the shell of gases around the star begin to expand and cool, causing a reddish glow.This is where the term red giant comes from. These stars are very bright because of their larger surface area. The core bec ...
... When an intermediatemass star leaves the main sequence as it runs out of hydrogen, the shell of gases around the star begin to expand and cool, causing a reddish glow.This is where the term red giant comes from. These stars are very bright because of their larger surface area. The core bec ...
Requiem for a Star
... Stars Comparable to Sun • M up to about 3 or 4 solar masses • As a Main Sequence star can only use hydrogen as a fuel • When hydrogen is exhausted collapse of interior is inevitable • Increase in temperature caused by collapse suddenly ignites unprocessed hydrogen, causing star to expand to become ...
... Stars Comparable to Sun • M up to about 3 or 4 solar masses • As a Main Sequence star can only use hydrogen as a fuel • When hydrogen is exhausted collapse of interior is inevitable • Increase in temperature caused by collapse suddenly ignites unprocessed hydrogen, causing star to expand to become ...
29.3 – Stellar Evolution
... – Higher temperature causes helium atoms fuse into carbon atoms – Causes outer shell to expand greatly ...
... – Higher temperature causes helium atoms fuse into carbon atoms – Causes outer shell to expand greatly ...
Universe, Earth, and The Solar System Characteristics of Stars
... A white dwarf is only about the size of the Earth but as much as mass as the sun. A neutron star is the remains of high-mass stars. A black hole is an object with gravity so strong that not even light can escape. These are usually formed from the death of the most massive stars. ...
... A white dwarf is only about the size of the Earth but as much as mass as the sun. A neutron star is the remains of high-mass stars. A black hole is an object with gravity so strong that not even light can escape. These are usually formed from the death of the most massive stars. ...
Life Cycle of a Star
... gets hotter as it shrinks, b/c of friction. • Nuclear fusion of H begins at 14 million degrees K. ...
... gets hotter as it shrinks, b/c of friction. • Nuclear fusion of H begins at 14 million degrees K. ...
Planetary nebula
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.