The correct answers are written in bold, italic and underlined. The
... • At the very bottom of the main sequence, massive stars being cool because of their great mass • At the very top of the main sequence, massive stars being very hot and active • In the middle of the main sequence, with very hot but less massive stars positioned higher and massive red giant stars pos ...
... • At the very bottom of the main sequence, massive stars being cool because of their great mass • At the very top of the main sequence, massive stars being very hot and active • In the middle of the main sequence, with very hot but less massive stars positioned higher and massive red giant stars pos ...
The Most Massive LMC Star Sk
... needs a longer time scale. This may be a general trend of massive star formation - 3,000 MG emitting an extremely powerful wind of 10-3 ,5 MG yr- 1 at 3,500 that they form in groups. Two recent km S-1. Today from the works of several results seem to confirm this impression. The first example is the ...
... needs a longer time scale. This may be a general trend of massive star formation - 3,000 MG emitting an extremely powerful wind of 10-3 ,5 MG yr- 1 at 3,500 that they form in groups. Two recent km S-1. Today from the works of several results seem to confirm this impression. The first example is the ...
Hertzsprung-Russell Diagram
... Specific to each element Used to identify elements present Universal ...
... Specific to each element Used to identify elements present Universal ...
Stars
... cook up elements more massive than iron, all the way to platinum. In the 15 billion year history of our Galaxy, about a quarter billion supernovae have each recycled about 10 M of metal-enriched gas back into the interstellar medium. This is a total of more than 1 billion M or more than 1 % of the ...
... cook up elements more massive than iron, all the way to platinum. In the 15 billion year history of our Galaxy, about a quarter billion supernovae have each recycled about 10 M of metal-enriched gas back into the interstellar medium. This is a total of more than 1 billion M or more than 1 % of the ...
Ch. 26.5: The Expanding Universe
... Dark Matter = Does not give off radiation & cannot be detected Exerts gravitational force on visible matter Universe may be 90% + dark matter Why do we think Dark Matter exists? Galaxies are accelerating faster than they should be (based on the observable matter in the Universe). The acceleration du ...
... Dark Matter = Does not give off radiation & cannot be detected Exerts gravitational force on visible matter Universe may be 90% + dark matter Why do we think Dark Matter exists? Galaxies are accelerating faster than they should be (based on the observable matter in the Universe). The acceleration du ...
Targets for Small Telescopes
... NGC 2070 is known as the Tarantula Nebula. It is also catalogued as Caldwell 103. Also sometimes known as 30 Doradus. It was discovered in ~1751 by Lacaille. It is a massive and luminous HII region, located within the Large Magellanic Cloud. It is the largest known HII region within the local group ...
... NGC 2070 is known as the Tarantula Nebula. It is also catalogued as Caldwell 103. Also sometimes known as 30 Doradus. It was discovered in ~1751 by Lacaille. It is a massive and luminous HII region, located within the Large Magellanic Cloud. It is the largest known HII region within the local group ...
Powerpoint - Astronomy at Swarthmore College
... plots show the speed at which the material is moving towards or away from the observer, who is positioned in the top center of the image. Blue corresponds to material moving towards the observer (which would be blueshifted), while red corresponds to material moving away from the observer (red-shifte ...
... plots show the speed at which the material is moving towards or away from the observer, who is positioned in the top center of the image. Blue corresponds to material moving towards the observer (which would be blueshifted), while red corresponds to material moving away from the observer (red-shifte ...
HR Diagram and Life of a star
... from 100-1000 times the size of the sun GIANTS- large bright stars a bit smaller and fainter than Super giants Super giants in the Red temp range tend to be in their last stages of life. They are out of hydrogen and are now fusing Helium into Carbon. White Dwarfs- are the small, dense remains of low ...
... from 100-1000 times the size of the sun GIANTS- large bright stars a bit smaller and fainter than Super giants Super giants in the Red temp range tend to be in their last stages of life. They are out of hydrogen and are now fusing Helium into Carbon. White Dwarfs- are the small, dense remains of low ...
Quiz 1 Review
... 18. What is a supernova? List 2 reasons why supernovas are important. When fusion is no longer going on in a star’s core it collapses colliding with the core. This is one of the most energetic events in the universe. More energy is emitted during the supernova than the star emitted its entire life. ...
... 18. What is a supernova? List 2 reasons why supernovas are important. When fusion is no longer going on in a star’s core it collapses colliding with the core. This is one of the most energetic events in the universe. More energy is emitted during the supernova than the star emitted its entire life. ...
Folie 1 - univie.ac.at
... typical time scales for their variability ranging from an hour to several weeks and aiming for a frequency resolution sufficient for asteroseismology, BRITE-Constellation expects to observe on average 20 stars simultaneously. ...
... typical time scales for their variability ranging from an hour to several weeks and aiming for a frequency resolution sufficient for asteroseismology, BRITE-Constellation expects to observe on average 20 stars simultaneously. ...
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... Gas infall into the potential wells of the dark matter fluctuations leads to increased density, formation of H2, molecular line cooling, further condensation and cloud fragmentation, leading to the formation of the first stars ...
... Gas infall into the potential wells of the dark matter fluctuations leads to increased density, formation of H2, molecular line cooling, further condensation and cloud fragmentation, leading to the formation of the first stars ...
A Summary of Stages
... the exact value is not known) are producing sufficient energy by just using the proton-proton chain of nuclear reactions, higher-mass stars must primarily rely on the carbon cycle to produce their greater requirements of energy to balance their greater gravity. The carbon atoms help the hydrogen ato ...
... the exact value is not known) are producing sufficient energy by just using the proton-proton chain of nuclear reactions, higher-mass stars must primarily rely on the carbon cycle to produce their greater requirements of energy to balance their greater gravity. The carbon atoms help the hydrogen ato ...
Day 1212
... A supernova is a gigantic explosion in which the temperature in the collapsing core reaches 10 billion K and atomic nuclei are split into neutrons and protons. When very massive stars, with masses greater than 25 times that of the Sun, collapse past the neutron-star stage, they form a black hole. ...
... A supernova is a gigantic explosion in which the temperature in the collapsing core reaches 10 billion K and atomic nuclei are split into neutrons and protons. When very massive stars, with masses greater than 25 times that of the Sun, collapse past the neutron-star stage, they form a black hole. ...
Young Galaxies Grow - Astronomical Society of the Pacific
... are formed along spiral arms. Our Milky Way is a spiral galaxy. Such disk galaxies mostly assembled in earlier epochs, but they continue to form stars today from remaining gas within the spiral arms. They are also surrounded by extended reservoirs of low-density gas thought to be too sparse to clump ...
... are formed along spiral arms. Our Milky Way is a spiral galaxy. Such disk galaxies mostly assembled in earlier epochs, but they continue to form stars today from remaining gas within the spiral arms. They are also surrounded by extended reservoirs of low-density gas thought to be too sparse to clump ...
Forming disk galaxies in magneto-hydro
... SuperMUC has played a decisive role in making the present simulations possible. Within our project, we are currently working on substantially scaling up the numerical resolution and dynamic range achieved in our simulations of the formation of Milky Way-sized galaxies, thereby allowing a treatment o ...
... SuperMUC has played a decisive role in making the present simulations possible. Within our project, we are currently working on substantially scaling up the numerical resolution and dynamic range achieved in our simulations of the formation of Milky Way-sized galaxies, thereby allowing a treatment o ...
astronomy webquest…… explore the universe
... Stars and planets are made from gases in a __________________. The Milky Way Galaxy is approximately _______________ light years across. How much longer will our Sun last? _________________________ Lifetimes of stars range from ___________ to ____________ years. Our star orbits the centre of our gal ...
... Stars and planets are made from gases in a __________________. The Milky Way Galaxy is approximately _______________ light years across. How much longer will our Sun last? _________________________ Lifetimes of stars range from ___________ to ____________ years. Our star orbits the centre of our gal ...
Lecture 13 (pdf from the powerpoint)
... • We observe stars at various stages of evolution, and can piece together a description of the evolution of stars in general • Computer models provide a “fast-forward” look at the evolution of stars. • Stars begin as clouds of gas and dust, which collapse to form a stellar disk. This disk eventually ...
... • We observe stars at various stages of evolution, and can piece together a description of the evolution of stars in general • Computer models provide a “fast-forward” look at the evolution of stars. • Stars begin as clouds of gas and dust, which collapse to form a stellar disk. This disk eventually ...
Stars with mass less than 0.5 solar masses
... finishes. As a conseguence, the nuclear fusion finishes too, and so the star starts to contract under the pressure of its own mass. Then, the destiny of the star depends on its mass: ...
... finishes. As a conseguence, the nuclear fusion finishes too, and so the star starts to contract under the pressure of its own mass. Then, the destiny of the star depends on its mass: ...
What We Know About Stars So Far
... •Scientists also figured out that the color of the star told us something about their temperature •Red-colored stars are cooler in temperature compared to bluecolored stars. ...
... •Scientists also figured out that the color of the star told us something about their temperature •Red-colored stars are cooler in temperature compared to bluecolored stars. ...
Student Literacy
... universe. One of the Milky Wayʼs neighboring galaxies is Andromeda. It is 2 million light years away. It is so far away that you canʼt see its individual stars. You can only see a hazy spot in the night sky produced by the combined light of the stars. The pictures below were taken by the Hubble Spac ...
... universe. One of the Milky Wayʼs neighboring galaxies is Andromeda. It is 2 million light years away. It is so far away that you canʼt see its individual stars. You can only see a hazy spot in the night sky produced by the combined light of the stars. The pictures below were taken by the Hubble Spac ...
Slide 1
... Leaving the Solar System, our next stop will be at the Alpha Centauri system. Source: Wikipedia ...
... Leaving the Solar System, our next stop will be at the Alpha Centauri system. Source: Wikipedia ...
Life Cycles of Stars
... • Equivalent to entire Earth’s nuclear arsenal going off one km away - every second • This energy output would last for days ...
... • Equivalent to entire Earth’s nuclear arsenal going off one km away - every second • This energy output would last for days ...
Cosmo: Student`s Workbook
... western world goes by a number of names. Eg The Aristotelian, the Classical, the geocentric, the Ptolmaic and the Medieval. It was a perfectly sensible model in that it satisfied the senses. The Earth was regarded as stationary and nailed in at the centre of the Universe. All heavenly bodies were th ...
... western world goes by a number of names. Eg The Aristotelian, the Classical, the geocentric, the Ptolmaic and the Medieval. It was a perfectly sensible model in that it satisfied the senses. The Earth was regarded as stationary and nailed in at the centre of the Universe. All heavenly bodies were th ...
H II region
An H II region is a large, low-density cloud of partially ionized gas in which star formation has recently taken place. The short-lived blue stars forged in these regions emit copious amounts of ultraviolet light that ionize the surrounding gas. H II regions—sometimes several hundred light-years across—are often associated with giant molecular clouds. The first known H II region was the Orion Nebula, which was discovered in 1610 by Nicolas-Claude Fabri de Peiresc.H II regions are named for the large amount of ionised atomic hydrogen they contain, referred to as H II, pronounced H-two by astronomers (an H I region being neutral atomic hydrogen, and H2 being molecular hydrogen). Such regions have extremely diverse shapes, because the distribution of the stars and gas inside them is irregular. They often appear clumpy and filamentary, sometimes showing bizarre shapes such as the Horsehead Nebula. H II regions may give birth to thousands of stars over a period of several million years. In the end, supernova explosions and strong stellar winds from the most massive stars in the resulting star cluster will disperse the gases of the H II region, leaving behind a cluster of birthed stars such as the Pleiades.H II regions can be seen to considerable distances in the universe, and the study of extragalactic H II regions is important in determining the distance and chemical composition of other galaxies. Spiral and irregular galaxies contain many H II regions, while elliptical galaxies are almost devoid of them. In the spiral galaxies, including the Milky Way, H II regions are concentrated in the spiral arms, while in the irregular galaxies they are distributed chaotically. Some galaxies contain huge H II regions, which may contain tens of thousands of stars. Examples include the 30 Doradus region in the Large Magellanic Cloud and NGC 604 in the Triangulum Galaxy.