cassiopeia a - Chandra X
... HOW: The supernova that created Cas A is thought to have occurred when a star about 25 times as massive as the Sun ran out of fuel for nuclear power. Its core then collapsed to form an ultra-dense object called a neutron star, and the outer layers of the star were ejected at enormous speeds (see ill ...
... HOW: The supernova that created Cas A is thought to have occurred when a star about 25 times as massive as the Sun ran out of fuel for nuclear power. Its core then collapsed to form an ultra-dense object called a neutron star, and the outer layers of the star were ejected at enormous speeds (see ill ...
10.2 Galaxies
... The Milky Way • Looking into the night sky, in one direction we see many sky objects since we are looking through the arms of our galaxy. In other directions we see fewer sky objects since we are not looking through our galaxy’s arms. ...
... The Milky Way • Looking into the night sky, in one direction we see many sky objects since we are looking through the arms of our galaxy. In other directions we see fewer sky objects since we are not looking through our galaxy’s arms. ...
Branches of Earth Science
... Galaxy is a huge collection of stars bound by ______________ o Contain various star ______________ ______________ of galaxies in the universe 3 types of galaxies o Spiral o Elliptical o Irregular ...
... Galaxy is a huge collection of stars bound by ______________ o Contain various star ______________ ______________ of galaxies in the universe 3 types of galaxies o Spiral o Elliptical o Irregular ...
What is a supernova - University of Warwick
... Super fact As far back as AD184 in China astronomers have been able to observe and record supernovae. October 1604 was the last time a supernova in the Milky Way galaxy became visible on Earth . It was measured in detail by the German ...
... Super fact As far back as AD184 in China astronomers have been able to observe and record supernovae. October 1604 was the last time a supernova in the Milky Way galaxy became visible on Earth . It was measured in detail by the German ...
Protostars and planets
... between planets and stars seemed too obvious to require precise formulation when the only planets known were those in the Solar System: the most massive of them is only MJupiter ≈ 10−3 M⊙ , and there are many of them follow approximately circular orbits about the Sun (indeed “planet” comes from Gree ...
... between planets and stars seemed too obvious to require precise formulation when the only planets known were those in the Solar System: the most massive of them is only MJupiter ≈ 10−3 M⊙ , and there are many of them follow approximately circular orbits about the Sun (indeed “planet” comes from Gree ...
Stellar evolution
... - Shells appear as a nebula around star, called "Planetary Nebula" (awful, historical name, nothing to do with planets. ...
... - Shells appear as a nebula around star, called "Planetary Nebula" (awful, historical name, nothing to do with planets. ...
Stellar Evolution
... Neutron Stars After a supernova, an extremely dense core of neutrons may be left in what is called a neutron star. These neutron stars are so dense that one teaspoon of material from a neutron star would weigh billions of tons. All stars rotate and thus have angular momentum. When a star loses ...
... Neutron Stars After a supernova, an extremely dense core of neutrons may be left in what is called a neutron star. These neutron stars are so dense that one teaspoon of material from a neutron star would weigh billions of tons. All stars rotate and thus have angular momentum. When a star loses ...
Beyond solar system
... This is why stars have very large masses. The sun’s diameter is 1,4 million km long, 100 times more than the earth’s. But the sun is an average star. Star diameters range from a few hundredths to hundreds of times the solar one. Yet even star dimensions, no matter how large, are small compared to th ...
... This is why stars have very large masses. The sun’s diameter is 1,4 million km long, 100 times more than the earth’s. But the sun is an average star. Star diameters range from a few hundredths to hundreds of times the solar one. Yet even star dimensions, no matter how large, are small compared to th ...
LIGO Star Chart
... You may recall from reading your LIGO Explorer Sheet that Betelgeuse is a red super giant and that if our sun were to be replaced by Betelgeuse the surface of the star’s atmosphere would extend almost to the orbit of Jupiter! Betelgeuse is a very old star that is a prime candidate for self-destructi ...
... You may recall from reading your LIGO Explorer Sheet that Betelgeuse is a red super giant and that if our sun were to be replaced by Betelgeuse the surface of the star’s atmosphere would extend almost to the orbit of Jupiter! Betelgeuse is a very old star that is a prime candidate for self-destructi ...
Star Characteristics
... Color + Temperature = Length of life Blue and white are the brightest Yellow stars last 10 billion years Red stars last longer It then turns into a super giant or red giant. ...
... Color + Temperature = Length of life Blue and white are the brightest Yellow stars last 10 billion years Red stars last longer It then turns into a super giant or red giant. ...
test - Scioly.org
... dwarf-type star, cooler than the Sun, while the other is a white dwarf, the stms are so close that they complete their orbital revolution in slightly over 6 1/2 hours and have a light curve illustrated in figure #2 D) SN 2Ollfe A) HM Cancri E) NGC 1846 B) SS Cvpi ...
... dwarf-type star, cooler than the Sun, while the other is a white dwarf, the stms are so close that they complete their orbital revolution in slightly over 6 1/2 hours and have a light curve illustrated in figure #2 D) SN 2Ollfe A) HM Cancri E) NGC 1846 B) SS Cvpi ...
Ch. 25 Properties of Stars
... The more negative, the brighter and the more positive, the dimmer Astronomers estimate that there are 200-400 billion stars in our Milky Way Galaxy, but we can only see about 2,500 visible to the naked eye on Earth ...
... The more negative, the brighter and the more positive, the dimmer Astronomers estimate that there are 200-400 billion stars in our Milky Way Galaxy, but we can only see about 2,500 visible to the naked eye on Earth ...
Stars - RSM Home
... • Stars can be classified by their size, mass, brightness, color, temperature, spectrum, and age. A star’s classification can change as it ages. • Main-Sequence Stars After a star forms, it enters the second and longest stage of its life cycle known as the main sequence. Energy is generated in the c ...
... • Stars can be classified by their size, mass, brightness, color, temperature, spectrum, and age. A star’s classification can change as it ages. • Main-Sequence Stars After a star forms, it enters the second and longest stage of its life cycle known as the main sequence. Energy is generated in the c ...
Unit 6--Astronomy
... 31.Another name for the interstellar matter that will eventually form a star is ____. a. supernova ...
... 31.Another name for the interstellar matter that will eventually form a star is ____. a. supernova ...
SALT Science – UW Madison
... the context of galaxy formation and evolution. We study this through the properties of luminous quasar host galaxies, objects in which the galaxy is actively feeding its black hole. This proposal focuses on a carefully selected sample of SDSS quasars, chosen over well-defined ranges of black hole ma ...
... the context of galaxy formation and evolution. We study this through the properties of luminous quasar host galaxies, objects in which the galaxy is actively feeding its black hole. This proposal focuses on a carefully selected sample of SDSS quasars, chosen over well-defined ranges of black hole ma ...
Stellar Evolution and the HR Diagram – Study Guide
... c. Which is brighter, the sun or a white dwarf? The Sun (but not as hot) d. Is Vega brighter than our sun? Yes (closer to upper top of diagram) e. Is Antares hotter than our sun? No, it’s a giant, class K or M (lower on diagram) 23. Stars that move off the main sequence first move to the _Giant_ reg ...
... c. Which is brighter, the sun or a white dwarf? The Sun (but not as hot) d. Is Vega brighter than our sun? Yes (closer to upper top of diagram) e. Is Antares hotter than our sun? No, it’s a giant, class K or M (lower on diagram) 23. Stars that move off the main sequence first move to the _Giant_ reg ...
ASTRONOMY 313
... hydrogen at 1215 Å (corresponding to a transition between the first and second energy levels of neutral hydrogen atoms) is observed in the optical spectrum of HS1946+7658 to be in emission at a wavelength of 4884.3 Å, in the blue-green region. a. ...
... hydrogen at 1215 Å (corresponding to a transition between the first and second energy levels of neutral hydrogen atoms) is observed in the optical spectrum of HS1946+7658 to be in emission at a wavelength of 4884.3 Å, in the blue-green region. a. ...
Amie Bickert - ColonialAcademyScience
... Step 1: Nebula is formed Step 2: In the densest part of the nebula gas and dust are pushed together and when it becomes heavy enough to form a star it is called a protostar. ...
... Step 1: Nebula is formed Step 2: In the densest part of the nebula gas and dust are pushed together and when it becomes heavy enough to form a star it is called a protostar. ...
The Young Astronomers Newsletter Volume 22 Number 3 February
... studying dusty, planet-forming disks around young stars and is now part of one of the world's biggest telescopes the 8-meter Gemini South telescope in Chile. ...
... studying dusty, planet-forming disks around young stars and is now part of one of the world's biggest telescopes the 8-meter Gemini South telescope in Chile. ...
First Light: Physical Characterization of Early Star Formation in the
... the merging of clumps of gas and stars, accompanied by slower accretion of gas. In this picture, dwarf galaxies may represent protogalactic fragments that have not yet been accreted into larger galaxies. However, a recent VLT spectroscopic study of red giants in four dwarf spheroidal companions to t ...
... the merging of clumps of gas and stars, accompanied by slower accretion of gas. In this picture, dwarf galaxies may represent protogalactic fragments that have not yet been accreted into larger galaxies. However, a recent VLT spectroscopic study of red giants in four dwarf spheroidal companions to t ...
Five Women at the Crossroads of Astronomy - Physics
... luckier than we are because they lived outside enough to be much more familiar with the sky than are most people today. And I think that if somehow we could get the public to go on a very dark night out into the country and to look at the Milky Way, most of the children would be overwhelmed. When I ...
... luckier than we are because they lived outside enough to be much more familiar with the sky than are most people today. And I think that if somehow we could get the public to go on a very dark night out into the country and to look at the Milky Way, most of the children would be overwhelmed. When I ...
Answers - Physics
... • D) stops spinning 11) What are pulsars? • A) rapidly spinning neutron stars • B) rapidly spinning black holes • C) stars that change temperature rapidly • D) stars that change size rapidly 12) Where does the energy that pulsars emit come from? • A) heat • B) fusion • C) gravity • D) spin 13) If we ...
... • D) stops spinning 11) What are pulsars? • A) rapidly spinning neutron stars • B) rapidly spinning black holes • C) stars that change temperature rapidly • D) stars that change size rapidly 12) Where does the energy that pulsars emit come from? • A) heat • B) fusion • C) gravity • D) spin 13) If we ...
The Components and Origin of the Universe
... 2. at first, the universe was hot (10 32 C) and energy went rushing out in all directions energy became cooled enough to become matter 3. matter then cooled enough to form protons, electrons and neutrons (subatomic particles) 4. subatomic particles combined to form mostly hydrogen but some helium n ...
... 2. at first, the universe was hot (10 32 C) and energy went rushing out in all directions energy became cooled enough to become matter 3. matter then cooled enough to form protons, electrons and neutrons (subatomic particles) 4. subatomic particles combined to form mostly hydrogen but some helium n ...
Unit 1
... • Low-mass stars rely on the protonproton cycle for their internal energy • Higher mass stars have much higher internal temperatures (20 million K!), so another fusion process dominates – An interaction involving Carbon, Nitrogen and Oxygen absorbs protons and releases helium nuclei – Roughly the sa ...
... • Low-mass stars rely on the protonproton cycle for their internal energy • Higher mass stars have much higher internal temperatures (20 million K!), so another fusion process dominates – An interaction involving Carbon, Nitrogen and Oxygen absorbs protons and releases helium nuclei – Roughly the sa ...
The Milky Way - Chandra X
... illuminated by brilliant clusters of young stars. These clouds and star clusters are part of the Orion spiral arm. As we move further out, fifty thousand light years from the Sun, other spiral arms of the Galaxy come into view along with the central bulge, where the Galaxy's supermassive black hole ...
... illuminated by brilliant clusters of young stars. These clouds and star clusters are part of the Orion spiral arm. As we move further out, fifty thousand light years from the Sun, other spiral arms of the Galaxy come into view along with the central bulge, where the Galaxy's supermassive black hole ...
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.