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... • How do we know the distance to stars and clusters in our galaxy? • Trigonometric parallax good out to 100 pc. • We believe galaxy is ~30 kpc wide. • How do we know? ...
... • How do we know the distance to stars and clusters in our galaxy? • Trigonometric parallax good out to 100 pc. • We believe galaxy is ~30 kpc wide. • How do we know? ...
Milky Way
... • What causes the mass to keep on increasing? • Don’t see anything there. Thus “dark” matter. ...
... • What causes the mass to keep on increasing? • Don’t see anything there. Thus “dark” matter. ...
Life Cycle of Stars - Lab Science Schedule
... or a black hole, depending on the star’s starting mass. The Life and Death of Stars Changes in stars may take place over a few million years or as much as several billion years – this is their life cycle. Some stars have existed almost since the origin of the universe, and others (such as our sun) h ...
... or a black hole, depending on the star’s starting mass. The Life and Death of Stars Changes in stars may take place over a few million years or as much as several billion years – this is their life cycle. Some stars have existed almost since the origin of the universe, and others (such as our sun) h ...
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... a. Halted by degeneracy pressure in the core. b. Halted when the atoms are pushed up against one another and contraction stops. c. Finally balanced by outward thermal pressure from nuclear reactions. d. Finally balanced by radiation emitted in the ...
... a. Halted by degeneracy pressure in the core. b. Halted when the atoms are pushed up against one another and contraction stops. c. Finally balanced by outward thermal pressure from nuclear reactions. d. Finally balanced by radiation emitted in the ...
On my webpage, find the link Star Life Cycle and use it to answer the
... A Solar Mass is equal to the mass of the Sun. If, for example, a star has 2 solar masses, it means it has twice as much mass as the Sun. Click the “brown dwarf” link in Option 1 6. How many solar masses are brown dwarfs on average? ...
... A Solar Mass is equal to the mass of the Sun. If, for example, a star has 2 solar masses, it means it has twice as much mass as the Sun. Click the “brown dwarf” link in Option 1 6. How many solar masses are brown dwarfs on average? ...
Properties of Stars
... Characteristics of Stars • Color is a clue to a star’s temperature • Very hot (30,000 K) stars emit their light in the blue spectrum, red stars are much cooler, stars with temperatures between 5000 and 6000 K appear yellow • Binary Stars – pairs of stars, pulled together by gravity, that orbit each ...
... Characteristics of Stars • Color is a clue to a star’s temperature • Very hot (30,000 K) stars emit their light in the blue spectrum, red stars are much cooler, stars with temperatures between 5000 and 6000 K appear yellow • Binary Stars – pairs of stars, pulled together by gravity, that orbit each ...
Notes- Stars
... Black Holes • Gravity is so strong that not even light can escape! • Often at the center of galaxies! • A Galaxy is a huge group of stars, dust, and gas held together by gravity • Milky way is a spiral galaxy, but galaxies can also be irregular or elliptical in shape ...
... Black Holes • Gravity is so strong that not even light can escape! • Often at the center of galaxies! • A Galaxy is a huge group of stars, dust, and gas held together by gravity • Milky way is a spiral galaxy, but galaxies can also be irregular or elliptical in shape ...
Stars and Moon Summative Review
... Identify the phases of the moon. How does the gravitational pull of the moon affect the Earth? (the side closest and the side farthest) What does a waxing moon indicate? Identify the cause of tides on Earth. Describe the effect that the elliptical orbit of the moon has on the Earth. ...
... Identify the phases of the moon. How does the gravitational pull of the moon affect the Earth? (the side closest and the side farthest) What does a waxing moon indicate? Identify the cause of tides on Earth. Describe the effect that the elliptical orbit of the moon has on the Earth. ...
20.1 Notes
... If the core that remains after a supernova has a mass of 1.4 – 3 solar masses it becomes a _______________ star, a very dense star that is a source of pulsating radio waves called _____________. ...
... If the core that remains after a supernova has a mass of 1.4 – 3 solar masses it becomes a _______________ star, a very dense star that is a source of pulsating radio waves called _____________. ...
Stellar Evolution and the HR Diagram Study Guide
... Which star will appear brighter in the night sky, a star with an apparent magnitude of 0 or a star with an apparent magnitude of +1? Star with apparent magnitude of 0 ...
... Which star will appear brighter in the night sky, a star with an apparent magnitude of 0 or a star with an apparent magnitude of +1? Star with apparent magnitude of 0 ...
the Study Guide
... such as in a supersonic jet or rocket ship. For example: 2G's are equal to twice the force of Earth's gravity. Galaxy: A giant cluster of stars in space. Galaxies can have different shapes, but the most common shape is a spiral, like our own Milky Way Galaxy. Scientists estimate that the Milky Way h ...
... such as in a supersonic jet or rocket ship. For example: 2G's are equal to twice the force of Earth's gravity. Galaxy: A giant cluster of stars in space. Galaxies can have different shapes, but the most common shape is a spiral, like our own Milky Way Galaxy. Scientists estimate that the Milky Way h ...
Chapter 29 Notes
... • Dark bands in the visible spectrum are caused by different chemical elements • 70% hydrogen 28% helium ...
... • Dark bands in the visible spectrum are caused by different chemical elements • 70% hydrogen 28% helium ...
Unit E Space Exploration Section 1 Notnd Space has changed over
... of a star in which gravity is so strong that not even light from radiation going on inside the ...
... of a star in which gravity is so strong that not even light from radiation going on inside the ...
The hierarchical structure of the Universe (go from little to large)
... - Everything you see is part of the Galaxy • The glow of the Milky Way • Stars • Star clusters (open clusters and globular clusters) • Planetary nebulae (dying stars) • Supernova remnants (stars that blew up) • Diffuse nebulae (glowing interstellar gas) ...
... - Everything you see is part of the Galaxy • The glow of the Milky Way • Stars • Star clusters (open clusters and globular clusters) • Planetary nebulae (dying stars) • Supernova remnants (stars that blew up) • Diffuse nebulae (glowing interstellar gas) ...
19Nov_2014
... • Low-mass stars create carbon and oxygen in their cores at the end of their lifespan, thanks to the higher temperatures and pressures present in a red giant star • High-mass stars produce heavier elements like silicon, magnesium, etc., by nuclear fusion in their cores – Temperatures are much higher ...
... • Low-mass stars create carbon and oxygen in their cores at the end of their lifespan, thanks to the higher temperatures and pressures present in a red giant star • High-mass stars produce heavier elements like silicon, magnesium, etc., by nuclear fusion in their cores – Temperatures are much higher ...
Universe and Galaxy Short Study Guide
... theory does not suggest an explosion into space, but instead that there is an expansion of space with matter going along for the ride. galaxy clusters. These groups of galaxies may have from a few to hundreds of member galaxies and may range in sizes up to 30 million ly. In a cluster, most of the in ...
... theory does not suggest an explosion into space, but instead that there is an expansion of space with matter going along for the ride. galaxy clusters. These groups of galaxies may have from a few to hundreds of member galaxies and may range in sizes up to 30 million ly. In a cluster, most of the in ...
The Life Cycle of Stars
... When the hydrogen supply in the core begins to run out, and the star is no longer generating heat by nuclear fusion, the core becomes unstable and contracts. The outer shell of the star, which is still mostly hydrogen, starts to expand. As it expands, it cools and glows red. The star has now reached ...
... When the hydrogen supply in the core begins to run out, and the star is no longer generating heat by nuclear fusion, the core becomes unstable and contracts. The outer shell of the star, which is still mostly hydrogen, starts to expand. As it expands, it cools and glows red. The star has now reached ...
Requiem for a Star
... Stars Comparable to Sun • M up to about 3 or 4 solar masses • As a Main Sequence star can only use hydrogen as a fuel • When hydrogen is exhausted collapse of interior is inevitable • Increase in temperature caused by collapse suddenly ignites unprocessed hydrogen, causing star to expand to become ...
... Stars Comparable to Sun • M up to about 3 or 4 solar masses • As a Main Sequence star can only use hydrogen as a fuel • When hydrogen is exhausted collapse of interior is inevitable • Increase in temperature caused by collapse suddenly ignites unprocessed hydrogen, causing star to expand to become ...
Pluto(2274km)- Pluto is a dwarf planet, and was classified as such in
... Sun(1.39x10^6km)The Sun is a G-type main sequence star based on its spectral class. The temperature of the photosphere (the outer shell of a star) is about 10,000°F. It is composed mostly of hydrogen, some helium, and smaller quantities of heavier elements including oxygen. It is the most important ...
... Sun(1.39x10^6km)The Sun is a G-type main sequence star based on its spectral class. The temperature of the photosphere (the outer shell of a star) is about 10,000°F. It is composed mostly of hydrogen, some helium, and smaller quantities of heavier elements including oxygen. It is the most important ...
lecture23
... More luminous variable stars have large Period Variability is EXTREMELY USEFUL, because it is an absolute distance indicator ...
... More luminous variable stars have large Period Variability is EXTREMELY USEFUL, because it is an absolute distance indicator ...
chapter10
... The Fate of our Sun and the End of Earth • Sun will expand to a red giant in ~ 5 billion years • Expands to ~ Earth’s orbit • Earth will then be ...
... The Fate of our Sun and the End of Earth • Sun will expand to a red giant in ~ 5 billion years • Expands to ~ Earth’s orbit • Earth will then be ...
From the Everett and Seattle Astronomical
... temperature gas. The atoms in the cloud are energized by ultraviolet light from a nearby star and emit radiation as they fall back into lower energy states. Emission nebulae are sites of recent and ongoing star formation. The Orion nebulae, also know as M42, is a good example of an emission nebulae. ...
... temperature gas. The atoms in the cloud are energized by ultraviolet light from a nearby star and emit radiation as they fall back into lower energy states. Emission nebulae are sites of recent and ongoing star formation. The Orion nebulae, also know as M42, is a good example of an emission nebulae. ...
PHYS 175 (2014) Final Examination Name: ___SOLUTION_____
... 29. Which of the following statements about the cosmic background radiation is incorrect? ...
... 29. Which of the following statements about the cosmic background radiation is incorrect? ...
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.