Multi-physics simulations using a hierarchical interchangeable
... evolution of the stars. We find that the star formation efficiency is a poor predictor of final state of the cluster. There are several arguments why the star formation efficiency is less important than has been found in earlier studies. The most dramatic event in the lifetime of a young cluster is ...
... evolution of the stars. We find that the star formation efficiency is a poor predictor of final state of the cluster. There are several arguments why the star formation efficiency is less important than has been found in earlier studies. The most dramatic event in the lifetime of a young cluster is ...
HR diagram
... located here are about 10 times larger than the Sun, and many time more luminous. Supergiants: A band extending across the top of the HR diagram from blue to red. These are extremely large and luminous stars. White dwarfs: A region in the lower left of the diagram. These are faint, hot, very sma ...
... located here are about 10 times larger than the Sun, and many time more luminous. Supergiants: A band extending across the top of the HR diagram from blue to red. These are extremely large and luminous stars. White dwarfs: A region in the lower left of the diagram. These are faint, hot, very sma ...
1. Stellar Evolution – Notes Astronomers classify stars according to
... On the H-R diagram, giant and supergiant stars lie above the main sequence, while white dwarfs are below the main sequence. Main-sequence stars are stars like the Sun but with different masses. The mass-luminosity relation expresses a direct correlation between mass and luminosity for main-sequence ...
... On the H-R diagram, giant and supergiant stars lie above the main sequence, while white dwarfs are below the main sequence. Main-sequence stars are stars like the Sun but with different masses. The mass-luminosity relation expresses a direct correlation between mass and luminosity for main-sequence ...
Astronomy Webquest Part 1: Life of Stars: Go to http://www.odec.ca
... Go to http://starchild.gsfc.nasa.gov/docs/StarChild/questions/question19.html and answer these questions: 1. True or False: Light year is a measurement time. It is a year of light. Evidence to support your answer:________________________________________________________________________________ 2. Lig ...
... Go to http://starchild.gsfc.nasa.gov/docs/StarChild/questions/question19.html and answer these questions: 1. True or False: Light year is a measurement time. It is a year of light. Evidence to support your answer:________________________________________________________________________________ 2. Lig ...
Slide 1
... If we know a star’s apparent magnitude and its distance from us, we can calculate its absolute (actual) luminosity. Absolute magnitude is the brightness stars would appear to be if they were all place at a standard distance of 10 pc. Therefore, absolute magnitude is an actual comparison of stellar l ...
... If we know a star’s apparent magnitude and its distance from us, we can calculate its absolute (actual) luminosity. Absolute magnitude is the brightness stars would appear to be if they were all place at a standard distance of 10 pc. Therefore, absolute magnitude is an actual comparison of stellar l ...
November 2005 - Otterbein University
... pressure (Pauli Exclusion Principle) at the end of the helium-burning stage • The core contracts until its temperature is high enough to fuse carbon into oxygen • Elements consumed in core • new elements form while previous elements continue to burn in outer layers ...
... pressure (Pauli Exclusion Principle) at the end of the helium-burning stage • The core contracts until its temperature is high enough to fuse carbon into oxygen • Elements consumed in core • new elements form while previous elements continue to burn in outer layers ...
Chap 11 Characterizing Stars v2
... magnitudes are plotted against surface temperatures). The H-R diagram reveals the existence of four major groupings of stars: main-sequence stars, giants, supergiants, and white dwarfs. The mass-luminosity relation expresses a direct correlation between a main-sequence star’s mass and the total ener ...
... magnitudes are plotted against surface temperatures). The H-R diagram reveals the existence of four major groupings of stars: main-sequence stars, giants, supergiants, and white dwarfs. The mass-luminosity relation expresses a direct correlation between a main-sequence star’s mass and the total ener ...
Astronomy - SparkNotes
... light into its intensity at different wavelengths or spectrum. Components: 1. Continuum: The smooth part of the spectrum (see Figure 1). Most objects emit light at all frequencies, but the shape of the spectrum depends on the physical process that produces the light. • Blackbody: A dense object that ...
... light into its intensity at different wavelengths or spectrum. Components: 1. Continuum: The smooth part of the spectrum (see Figure 1). Most objects emit light at all frequencies, but the shape of the spectrum depends on the physical process that produces the light. • Blackbody: A dense object that ...
Problem Set 2
... of a flux limit (i.e., an apparent magnitude limit). If we observe stars (or anything else) down to a fixed apparent brightness, we do not get a fair mixture of all of the stars in the sky (or observed volume), but we include more of the most luminous stars, which creep into the sample because of th ...
... of a flux limit (i.e., an apparent magnitude limit). If we observe stars (or anything else) down to a fixed apparent brightness, we do not get a fair mixture of all of the stars in the sky (or observed volume), but we include more of the most luminous stars, which creep into the sample because of th ...
2. Equations of Stellar Structure We already discussed that the
... So far, we have discussed the equations using r as the independent variable. Unfortunately it is inconvenient to specify the boundary conditions in r, as the outer radius R is not known before we solve the equations1 . Fortunately, we frequently want to solve the stellar equations as a function of t ...
... So far, we have discussed the equations using r as the independent variable. Unfortunately it is inconvenient to specify the boundary conditions in r, as the outer radius R is not known before we solve the equations1 . Fortunately, we frequently want to solve the stellar equations as a function of t ...
updated
... time) of planets. Hence these objects were called Planetary Nebulae even though the objects themselves have nothing whatsoever to do with planets or planetary formation. A better terminology would be to call them Post Red Giant Nebulae, but that hasn’t caught on. Eventually those outer layers of the ...
... time) of planets. Hence these objects were called Planetary Nebulae even though the objects themselves have nothing whatsoever to do with planets or planetary formation. A better terminology would be to call them Post Red Giant Nebulae, but that hasn’t caught on. Eventually those outer layers of the ...
Seeing Gravitational Waves - Carnegie Observatories User Webpages
... Theorists are working out the expected electromagnetic signature from neutron star and black hole mergers; the luminosity, time scale, and spectral energy distribution. The predicted counterpart is expected to be fainter than a supernova (but brighter than a nova), last for a few hours to a few days ...
... Theorists are working out the expected electromagnetic signature from neutron star and black hole mergers; the luminosity, time scale, and spectral energy distribution. The predicted counterpart is expected to be fainter than a supernova (but brighter than a nova), last for a few hours to a few days ...
Chapter 19 Star Formation
... Individual cloud fragments begin to collapse. Once the density is high enough, there is no further fragmentation. Reason: the star has become opaque to its own radiation: It has a photosphere! After this, the ‘trapped radiation heats the interior of the object as it contracts. Stage 3: Object become ...
... Individual cloud fragments begin to collapse. Once the density is high enough, there is no further fragmentation. Reason: the star has become opaque to its own radiation: It has a photosphere! After this, the ‘trapped radiation heats the interior of the object as it contracts. Stage 3: Object become ...
Chapter 19 Star Formation
... Individual cloud fragments begin to collapse. Once the density is high enough, there is no further fragmentation. Reason: the star has become opaque to its own radiation: It has a photosphere! After this, the ‘trapped radiation heats the interior of the object as it contracts. Stage 3: Object become ...
... Individual cloud fragments begin to collapse. Once the density is high enough, there is no further fragmentation. Reason: the star has become opaque to its own radiation: It has a photosphere! After this, the ‘trapped radiation heats the interior of the object as it contracts. Stage 3: Object become ...
December 2015
... called the Snowflake Nebula. Rather like a Christmas Tree decoration. Most of the illuminated gas cloud nebulas seen in our skies are emission nebulae. The light emission arises from gases ionized by high energy photons emitted from stars that have often been formed within the nebula. These star for ...
... called the Snowflake Nebula. Rather like a Christmas Tree decoration. Most of the illuminated gas cloud nebulas seen in our skies are emission nebulae. The light emission arises from gases ionized by high energy photons emitted from stars that have often been formed within the nebula. These star for ...
ASTRO 1050 The Structure of the Milky Way Galaxy
... halo, a larger cloud of stars that surround the entire Galaxy. The halo is much larger than the bulge. Our Milky Way Galaxy is made up of mostly stars, gas and dust. The dust blocks out light from distant stars, and makes it difficult to see most of the Galaxy, especially the bulge and parts of the ...
... halo, a larger cloud of stars that surround the entire Galaxy. The halo is much larger than the bulge. Our Milky Way Galaxy is made up of mostly stars, gas and dust. The dust blocks out light from distant stars, and makes it difficult to see most of the Galaxy, especially the bulge and parts of the ...
Stellar Physics 1
... A. A hot dense gas produces a continuous spectrum with no spectral lines. B. A hot diffuse gas produces bright spectral lines – an emission spectrum. C. A cool dense gas produces a continuous spectrum with no spectral lines. y D. A cool diffuse gas in front of a source of continuous spectrum produce ...
... A. A hot dense gas produces a continuous spectrum with no spectral lines. B. A hot diffuse gas produces bright spectral lines – an emission spectrum. C. A cool dense gas produces a continuous spectrum with no spectral lines. y D. A cool diffuse gas in front of a source of continuous spectrum produce ...
File - YEAR 11 EBSS PHYSICS DETAILED STUDIES
... last forever… Billions of years, yes, but not forever. A star may have enough fuel to last it billions of years, however models have shown that a stars life may not be as long. The hydrogen-hydrogen fusion process produces helium, as the concentration of helium builds up in the core, the reaction ...
... last forever… Billions of years, yes, but not forever. A star may have enough fuel to last it billions of years, however models have shown that a stars life may not be as long. The hydrogen-hydrogen fusion process produces helium, as the concentration of helium builds up in the core, the reaction ...
Life Cycle of a Star - Intervention Worksheet
... _____ The star begins to run out of fuel and expands into a red giant or red super giant. _____ Stars start out as diffused clouds of gas and dust drifting through space. A single one of these clouds is called a nebula _____ What happens next depends on the mass of the star. _____ Heat and pressure ...
... _____ The star begins to run out of fuel and expands into a red giant or red super giant. _____ Stars start out as diffused clouds of gas and dust drifting through space. A single one of these clouds is called a nebula _____ What happens next depends on the mass of the star. _____ Heat and pressure ...