![Globular Cluster Formation in CDM Cosmologies](http://s1.studyres.com/store/data/006073409_1-ea8c0069b88bb24651f398d3f50b6fca-300x300.png)
Globular Cluster Formation in CDM Cosmologies
... optical polarimetry) with molecular streaks Cloud mass 2x10^4 solar masses Low efficiency of star ...
... optical polarimetry) with molecular streaks Cloud mass 2x10^4 solar masses Low efficiency of star ...
AST101 Lecture 20 The Ecology of the Galaxy
... • About 1010 years old • 105 - 106 stars • Radius ~ 10 light years • Most massive star: ~ 1 solar mass • ~150 globular clusters known in Milky Way ...
... • About 1010 years old • 105 - 106 stars • Radius ~ 10 light years • Most massive star: ~ 1 solar mass • ~150 globular clusters known in Milky Way ...
47th Lunar and Planetary Science Conference (2016) 3021
... [email protected], and Center for Stable Isotopes, University of New Mexico, Albuquerque, NM 87131 Introduction: The formation of our solar system is a fairly well understood process. It is thought that a dense interstellar molecular cloud collapsed to form the protoplanetary disk ([e.g.,1] at 4.568 Ga ...
... [email protected], and Center for Stable Isotopes, University of New Mexico, Albuquerque, NM 87131 Introduction: The formation of our solar system is a fairly well understood process. It is thought that a dense interstellar molecular cloud collapsed to form the protoplanetary disk ([e.g.,1] at 4.568 Ga ...
BAS - Monthly Sky Guide - Brisbane Astronomical Society
... Auriga has three star clusters discovered by Charles Messier in the 18 th century. Messier 36 is a large open cluster of about 60 stars. Messier 37 is another beautiful open cluster and Messier 38 is yet another cluster that is slightly fainter. All are worth seeking out in a low to moderate power ...
... Auriga has three star clusters discovered by Charles Messier in the 18 th century. Messier 36 is a large open cluster of about 60 stars. Messier 37 is another beautiful open cluster and Messier 38 is yet another cluster that is slightly fainter. All are worth seeking out in a low to moderate power ...
observed
... estimate within our Galaxy, the Milky Way. 1920’s: Edwin Hubble used these Standard Candles (Cepheid Variable stars) to get a much larger distance to Andromeda. Hence S And was 20,000 times brighter than a “normal” nova… Baade therefore dubbed these objects “super-novae”. ...
... estimate within our Galaxy, the Milky Way. 1920’s: Edwin Hubble used these Standard Candles (Cepheid Variable stars) to get a much larger distance to Andromeda. Hence S And was 20,000 times brighter than a “normal” nova… Baade therefore dubbed these objects “super-novae”. ...
Stellar Evolution: The Lives of Stars
... hunters upper left shoulder. Betelgeuse has such a short life due to its massive size, about 300 times the mass of the Sun (it consumes its nuclear fuel very fast), and so it would have been seen as a blue white star 10,000 years ago. Then over the period of human civilization it turned white then y ...
... hunters upper left shoulder. Betelgeuse has such a short life due to its massive size, about 300 times the mass of the Sun (it consumes its nuclear fuel very fast), and so it would have been seen as a blue white star 10,000 years ago. Then over the period of human civilization it turned white then y ...
Stellar types - schoolphysics
... These are stars with masses more than ten times that of the Sun. They are very cool with surface temperatures between about 3500K and 4500K. Betelgeuse in Orion is an example of this type of star. It has a diameter of about 500 million km – large enough to contain the whole of the Earth’s orbit! Fur ...
... These are stars with masses more than ten times that of the Sun. They are very cool with surface temperatures between about 3500K and 4500K. Betelgeuse in Orion is an example of this type of star. It has a diameter of about 500 million km – large enough to contain the whole of the Earth’s orbit! Fur ...
The Size of the Universe (1920) Harlow Shapley Heber Curtis
... The Great Debate: The Size of the Universe ...
... The Great Debate: The Size of the Universe ...
Unit 2 Review Guide
... 11. What color would galaxies shift towards if they were moving towards us? 12. What is the name of the cluster that our galaxy is in? 13. What are 2 possibilities for the ultimate fate of the universe? 14. What is a nebula? 15. What force causes stars to form? 16. What do we call a beginning star t ...
... 11. What color would galaxies shift towards if they were moving towards us? 12. What is the name of the cluster that our galaxy is in? 13. What are 2 possibilities for the ultimate fate of the universe? 14. What is a nebula? 15. What force causes stars to form? 16. What do we call a beginning star t ...
PHYSICS 1500 ASTRONOMY Sample Exam Solutions Section B
... ~80% N2 and ~20% 02. Most of the original CO2 has been incorporated into rocks via the oceans; some was converted to 02 via photosynthesis. The N2 just sat there. Mars' atmosphere is 104 times less thick than Venus, but has a similar composition - it has been slowly lost over time because of the pla ...
... ~80% N2 and ~20% 02. Most of the original CO2 has been incorporated into rocks via the oceans; some was converted to 02 via photosynthesis. The N2 just sat there. Mars' atmosphere is 104 times less thick than Venus, but has a similar composition - it has been slowly lost over time because of the pla ...
stars
... Be stars are non-supergiant B-type stars whose spectra have, or had at some time, one or more Balmer lines in emission. The mystery of the "Be phenomenon" is that the emission, which is well understood to originate from a flattened circumstellar disk (e.g. Struve, 1931), can come and go episodically ...
... Be stars are non-supergiant B-type stars whose spectra have, or had at some time, one or more Balmer lines in emission. The mystery of the "Be phenomenon" is that the emission, which is well understood to originate from a flattened circumstellar disk (e.g. Struve, 1931), can come and go episodically ...
Stellar Evolution
... so little mass that no fusion can occur. Therefore they are never main-sequence stars. It glows with infrared light generated from its gravitational contraction like Jupiter does. They don’t “evolve” but stay brown dwarfs and slowly fade over 100s of billions of years ...
... so little mass that no fusion can occur. Therefore they are never main-sequence stars. It glows with infrared light generated from its gravitational contraction like Jupiter does. They don’t “evolve” but stay brown dwarfs and slowly fade over 100s of billions of years ...
Stars & Galaxies
... professional development ONLY; and may not be used for other purposes, in whole or part, without the expressed written permission of their ESC-TESCCC coordinator for the region handling your subscription. TESCCC grants subscribers the right to edit this multimedia presentation for intra-district pro ...
... professional development ONLY; and may not be used for other purposes, in whole or part, without the expressed written permission of their ESC-TESCCC coordinator for the region handling your subscription. TESCCC grants subscribers the right to edit this multimedia presentation for intra-district pro ...
Linking Asteroids and Meteorites through Reflectance Spectroscopy
... • Can fuse Carbon and heavier elements • Helium Capture can also occur where Helium can be fused into heavy elements ...
... • Can fuse Carbon and heavier elements • Helium Capture can also occur where Helium can be fused into heavy elements ...
Stellar Evolution
... so little mass that no fusion can occur. Therefore they are never main-sequence stars. It glows with infrared light generated from its gravitational contraction like Jupiter does. They don’t “evolve” but stay brown dwarfs and slowly fade over 100s of billions of years ...
... so little mass that no fusion can occur. Therefore they are never main-sequence stars. It glows with infrared light generated from its gravitational contraction like Jupiter does. They don’t “evolve” but stay brown dwarfs and slowly fade over 100s of billions of years ...
Stellar Birth - ahsastronomy
... • The cloud typically begins to shrink in size and the appearance of a potostar can be seen at the center. ...
... • The cloud typically begins to shrink in size and the appearance of a potostar can be seen at the center. ...
Slide 1 - cosmos.esa.int
... “normal” supernovae, most of our intuition gained from these low-entropy models is not so useful for BH formation. • The neutrino signal from these collapses may be detectable. We need detailed spectra and details of formation. • We’re working on new models, requests taken. ...
... “normal” supernovae, most of our intuition gained from these low-entropy models is not so useful for BH formation. • The neutrino signal from these collapses may be detectable. We need detailed spectra and details of formation. • We’re working on new models, requests taken. ...
Scientific Justification
... are the coolest class of pulsating white dwarfs. Just as earthquakes allow seismologists to study the interior of the Earth, the global pulsations in white dwarfs send gravity-driven seismic waves deep through the interior and bring information to the surface in the form of brightness variations. We ...
... are the coolest class of pulsating white dwarfs. Just as earthquakes allow seismologists to study the interior of the Earth, the global pulsations in white dwarfs send gravity-driven seismic waves deep through the interior and bring information to the surface in the form of brightness variations. We ...
Presentation - Science in the News
... Status Report • neutral hydrogen • neutral helium Everywhere. EVERYWHERE! • not much else ...
... Status Report • neutral hydrogen • neutral helium Everywhere. EVERYWHERE! • not much else ...
4th Six Weeks Review key
... 31. Fusion occurs when ___hydrogen_ atoms fuse to form __helium____ with the resulting change in mass releases energy. 32. What type of star is our sun? (circle one) MASSIVE or AVERAGE 33. Our sun is a _____main sequence star and is the color ___yellow___. 34. Where is our sun located within the Mil ...
... 31. Fusion occurs when ___hydrogen_ atoms fuse to form __helium____ with the resulting change in mass releases energy. 32. What type of star is our sun? (circle one) MASSIVE or AVERAGE 33. Our sun is a _____main sequence star and is the color ___yellow___. 34. Where is our sun located within the Mil ...
June - San Bernardino Valley Amateur Astronomers
... Cloud survey/Cambridge Astronomical Survey Unit) ...
... Cloud survey/Cambridge Astronomical Survey Unit) ...
Slide 1
... collapsing down and crushing the core of the star. As long as we have nuclear fusion pushing out, our star can fight off gravity. ...
... collapsing down and crushing the core of the star. As long as we have nuclear fusion pushing out, our star can fight off gravity. ...
Stars and Their Life Cycles
... Main Sequence Stars • all stars fuse hydrogen into helium • 90% of all stars, including our Sun, are main sequence stars (average stars) • range from high luminosity (brightness) and high surface temperature to low luminosity and low surface temperature ...
... Main Sequence Stars • all stars fuse hydrogen into helium • 90% of all stars, including our Sun, are main sequence stars (average stars) • range from high luminosity (brightness) and high surface temperature to low luminosity and low surface temperature ...
The Life and Death of Stars
... Like our sun they fuse Hydrogen to Helium for fuel When core Hydrogen runs out the star collapses (cf our Sun) It will start fusing Helium to Carbon Eventually core Helium runs out and star collapses again Gets even hotter than before Carbon fuses into heavier elements Process of: star collapse – fu ...
... Like our sun they fuse Hydrogen to Helium for fuel When core Hydrogen runs out the star collapses (cf our Sun) It will start fusing Helium to Carbon Eventually core Helium runs out and star collapses again Gets even hotter than before Carbon fuses into heavier elements Process of: star collapse – fu ...
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.