![Globular Cluster Formation in CDM Cosmologies](http://s1.studyres.com/store/data/008078157_1-0cd6a0578c5155df0648e08320217b1a-300x300.png)
Globular Cluster Formation in CDM Cosmologies
... - icy grains in protostellar disks? meteorite parent bodies? ...
... - icy grains in protostellar disks? meteorite parent bodies? ...
1 Josh Machado Science Section C. Language Arts Section E. 5/15
... stellar corpse known as a white dwarf. When a star comes to the end of its life, there are a number of ways it can die, as well as numerous varieties of stellar corpses that can be left behind. When stars around the size of our sun die, they become red giants, and eventually white dwarfs. A white dw ...
... stellar corpse known as a white dwarf. When a star comes to the end of its life, there are a number of ways it can die, as well as numerous varieties of stellar corpses that can be left behind. When stars around the size of our sun die, they become red giants, and eventually white dwarfs. A white dw ...
printer-friendly sample test questions
... 2nd Item Specification: Recognize the life-cycles of mid-size and massive stars and their stellar remnants. Depth of Knowledge Level 1 8. When fusion of hydrogen ceases in our Sun’s core, the Sun will A. explode as a supernova. B. collapse into white dwarf star. C. contract into a black hole. D. exp ...
... 2nd Item Specification: Recognize the life-cycles of mid-size and massive stars and their stellar remnants. Depth of Knowledge Level 1 8. When fusion of hydrogen ceases in our Sun’s core, the Sun will A. explode as a supernova. B. collapse into white dwarf star. C. contract into a black hole. D. exp ...
Origin of Planetary Systems
... Fig. 4. Photographs of star-forming regions taken by the famous Hubble Space Telescope. (a) The famous Orion Nebula, one of the many current sites of star formation in our Galaxy (Milky Way or Akashganga). This particular nebula is very well studied by astronomers because of its relative proximity t ...
... Fig. 4. Photographs of star-forming regions taken by the famous Hubble Space Telescope. (a) The famous Orion Nebula, one of the many current sites of star formation in our Galaxy (Milky Way or Akashganga). This particular nebula is very well studied by astronomers because of its relative proximity t ...
Medieval Astrology Course Fundamenta
... Planetary Sect: whilst no longer used in modern astrology it is vital in judging planetary condition. Aspects: explores the wide range of ways in which planets glance, behold, prohibit and besiege one another. Planetary Cycles: the astronomy of the spheres covering basics such as perihelion, aphelio ...
... Planetary Sect: whilst no longer used in modern astrology it is vital in judging planetary condition. Aspects: explores the wide range of ways in which planets glance, behold, prohibit and besiege one another. Planetary Cycles: the astronomy of the spheres covering basics such as perihelion, aphelio ...
Star Arsenic, Star Selenium The Big Bang produced lots of hydrogen
... The Big Bang produced lots of hydrogen and helium and a smidgen of lithium. All heavier elements found on the periodic table have been produced by stars over the last 13.7 billion years. Astronomers analyze starlight to determine the chemical makeup of stars, the origin of the elements, the ages of ...
... The Big Bang produced lots of hydrogen and helium and a smidgen of lithium. All heavier elements found on the periodic table have been produced by stars over the last 13.7 billion years. Astronomers analyze starlight to determine the chemical makeup of stars, the origin of the elements, the ages of ...
How are galaxies classified
... A: Supernovas are very bright and can cause a brief (few months) burst of radiation that can outshine an entire galaxy. A: During this explosion, a supernova can give off as much energy as our Sun could emit over its life span! ...
... A: Supernovas are very bright and can cause a brief (few months) burst of radiation that can outshine an entire galaxy. A: During this explosion, a supernova can give off as much energy as our Sun could emit over its life span! ...
dark matter
... Chemical evolution Finished last time by saying that all elements heavier than hydrogen and helium were formed in stars. The younger a star, the more material from previous generations of stars it will contain, and the higher their metallicity. Stars can be broadly split into two populations: Popula ...
... Chemical evolution Finished last time by saying that all elements heavier than hydrogen and helium were formed in stars. The younger a star, the more material from previous generations of stars it will contain, and the higher their metallicity. Stars can be broadly split into two populations: Popula ...
A STEP Expected Yield of Planets
... Combined to radial-velocimetry, it is the only way to determine the density, hence the global composition of a planet Transit spectroscopy offers additional possibilities not accessible for “normal” planets ...
... Combined to radial-velocimetry, it is the only way to determine the density, hence the global composition of a planet Transit spectroscopy offers additional possibilities not accessible for “normal” planets ...
Nuclear Fusion – when two H atoms combine to form one atom thus
... Nebula – Stars are formed or “born” in a nebula. Massive cosmic cloud of matter from which stars are created. Light Year – distance light travels in one year. 186,000 miles/sec – speed of light Life Cycle of a Star Stars start off as a nebula until a nuclear explosion causes the star to shine. The n ...
... Nebula – Stars are formed or “born” in a nebula. Massive cosmic cloud of matter from which stars are created. Light Year – distance light travels in one year. 186,000 miles/sec – speed of light Life Cycle of a Star Stars start off as a nebula until a nuclear explosion causes the star to shine. The n ...
Astronomy 110G Review Sheet for Exam #3 The
... other galaxies or “island universes” like the Milky Way? What suggested otherwise? What observations showed conclusively that they were extragalactic objects? (The last is the most important part.) How does one determine the mass of a galaxy? (There are several possible ways). How do these determina ...
... other galaxies or “island universes” like the Milky Way? What suggested otherwise? What observations showed conclusively that they were extragalactic objects? (The last is the most important part.) How does one determine the mass of a galaxy? (There are several possible ways). How do these determina ...
The sounds of the stars
... Some of Kepler’s biggest surprises have been in its sounding out of red giants. These are Sunlike stars that have exhausted the hydrogen at their cores, causing a fuel crisis that paradoxically leads them to swell up to more than 100 times their original diameters. In about 5 billion years’ time, fo ...
... Some of Kepler’s biggest surprises have been in its sounding out of red giants. These are Sunlike stars that have exhausted the hydrogen at their cores, causing a fuel crisis that paradoxically leads them to swell up to more than 100 times their original diameters. In about 5 billion years’ time, fo ...
1. What is the HR diagram? 1a. The HR diagram is a plot of a star`s
... The explosive start to Helium burning in the core for low mass stars. On the horizontal branch, how is the star powered? What burns where? Helium burning in the core. No real shell burning at this stage. On the asymptotic giant branch (AGB), can you ever get a helium burning shell outside a hydrogen ...
... The explosive start to Helium burning in the core for low mass stars. On the horizontal branch, how is the star powered? What burns where? Helium burning in the core. No real shell burning at this stage. On the asymptotic giant branch (AGB), can you ever get a helium burning shell outside a hydrogen ...
Wednesday, April 23 - Otterbein University
... thrown into space by supernovae – Condense into new stars and planets – Elements heavier than iron form during supernovae explosions ...
... thrown into space by supernovae – Condense into new stars and planets – Elements heavier than iron form during supernovae explosions ...
Preface
... 2. What is the coupling between the incident plasma and the ionosphere/upper atmosphere or the surface? The electric current systems (planetary surface, ionosphere, and boundaries) around other planetary bodies can be quite different from their terrestrial analogues. This makes ionospheric morpholog ...
... 2. What is the coupling between the incident plasma and the ionosphere/upper atmosphere or the surface? The electric current systems (planetary surface, ionosphere, and boundaries) around other planetary bodies can be quite different from their terrestrial analogues. This makes ionospheric morpholog ...
Presentation - Harvard-Smithsonian Center for Astrophysics
... Symbiotic Star: AG Dra This stellar system consists of a red giant whose wind and surrounding nebula is photoionized by a hot white dwarf companion. Spectrum is complex with narrow nebular emission, and the surprising presencs of high ionization forbidden lines. These conditions are quite different ...
... Symbiotic Star: AG Dra This stellar system consists of a red giant whose wind and surrounding nebula is photoionized by a hot white dwarf companion. Spectrum is complex with narrow nebular emission, and the surprising presencs of high ionization forbidden lines. These conditions are quite different ...
Main-sequence stage Stellar lifetimes
... End states of stars - I • White dwarfs / neutron stars / black holes • Low-mass stars: – At end of core He fusion, still have shell sources of H and He fusion. – Star returns to red as an asymptotic giant-branch (AGB) star. – Core cannot become hot enough for further fusion. – Within 104 to 105 year ...
... End states of stars - I • White dwarfs / neutron stars / black holes • Low-mass stars: – At end of core He fusion, still have shell sources of H and He fusion. – Star returns to red as an asymptotic giant-branch (AGB) star. – Core cannot become hot enough for further fusion. – Within 104 to 105 year ...
What YOU can do! - Bangalore Astronomical Society
... Dark Matter and Dark Energy Cosmic Microwave Background Radiation ...
... Dark Matter and Dark Energy Cosmic Microwave Background Radiation ...
The Cycle of Star Formation
... Eventually, the protostar will fuse hydrogen in its core. This energy will greatly increase the radiation pressure that the photons create on their surroundings. A stellar wind will begin to blow material away. ...
... Eventually, the protostar will fuse hydrogen in its core. This energy will greatly increase the radiation pressure that the photons create on their surroundings. A stellar wind will begin to blow material away. ...
The Universe - Solon City Schools
... Which type of galaxy has old red stars? elliptical Which type of galaxy has young blue stars? spiral ...
... Which type of galaxy has old red stars? elliptical Which type of galaxy has young blue stars? spiral ...
powerpoint - Physics @ IUPUI
... • This is done by radiation pressure and gas pressure (they counteract gravity). • But to keep this up requires the constant generation of energy in the core. ...
... • This is done by radiation pressure and gas pressure (they counteract gravity). • But to keep this up requires the constant generation of energy in the core. ...
STARS: how they are born, live and die
... about the size of Earth. Its weight supported against further collapse by electron degeneracy pressure, it will do nothing but sit there and cool off, for eternity. ...
... about the size of Earth. Its weight supported against further collapse by electron degeneracy pressure, it will do nothing but sit there and cool off, for eternity. ...
AN INTERSTELLAR CLOUD WITH A HIGH CON
... The interstellar absorption lines due to the CN molecule have been observed only in a few bright stars, on spectrograms obtained on high-contrast emulsions with the highest spectral resolving powers available (Adams 1943, 1949). The intensity of the strongest CN line, R(O) of the (0, 0) band in the ...
... The interstellar absorption lines due to the CN molecule have been observed only in a few bright stars, on spectrograms obtained on high-contrast emulsions with the highest spectral resolving powers available (Adams 1943, 1949). The intensity of the strongest CN line, R(O) of the (0, 0) band in the ...
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.