Everything Under and Over The Stars
... happen to the solar system? There was a recent supernova called SN1993J in a star system, which is not mentioned. The powerful shockwave traveled at 44 million mph, but 5 years later it slowed down because of drag caused by particles. There has been a supernova in the Milky Way, around the 1700’s. A ...
... happen to the solar system? There was a recent supernova called SN1993J in a star system, which is not mentioned. The powerful shockwave traveled at 44 million mph, but 5 years later it slowed down because of drag caused by particles. There has been a supernova in the Milky Way, around the 1700’s. A ...
Astronomy 170: Aug. 24 10am class
... • If you didn’t get the honors section instructions, get them from Megan. • We increased the enrollment limit for the honors section, Section 3. If you are in Section 2 and want honors credit for this class, you must fill out a change of section form and have Prof. Bechtold sign it. ...
... • If you didn’t get the honors section instructions, get them from Megan. • We increased the enrollment limit for the honors section, Section 3. If you are in Section 2 and want honors credit for this class, you must fill out a change of section form and have Prof. Bechtold sign it. ...
The Life of a Star
... after the main-sequence stage. • This is a star that expands and cools because it has used up all of its hydrogen. • The center of the star shrinks, but the atmosphere gets very large. • The star may become a supergiant (100 times bigger than the sun). ...
... after the main-sequence stage. • This is a star that expands and cools because it has used up all of its hydrogen. • The center of the star shrinks, but the atmosphere gets very large. • The star may become a supergiant (100 times bigger than the sun). ...
REVIEW: STAR`S TEST
... Explain how the e and m are related. A small amount of _____________ can become a huge amount of ____________ What is the speed of light ? List the visible light from longest to shortest wavelengths. ...
... Explain how the e and m are related. A small amount of _____________ can become a huge amount of ____________ What is the speed of light ? List the visible light from longest to shortest wavelengths. ...
Section 19.3
... 19.3 Types of Galaxies Astronomers classify galaxies according to their shape. 1. Spiral galaxies consist of a central, dense area surrounded by spiraling arms. 2. Barred spiral galaxies have a bar-shaped structure in the center. 3. Elliptical galaxies look like the central portion of a spiral gal ...
... 19.3 Types of Galaxies Astronomers classify galaxies according to their shape. 1. Spiral galaxies consist of a central, dense area surrounded by spiraling arms. 2. Barred spiral galaxies have a bar-shaped structure in the center. 3. Elliptical galaxies look like the central portion of a spiral gal ...
Evolution Cycle of Stars
... grains of dust in a nebula. • Dark Nebula are dense clouds of molecular hydrogen which partially or completely absorb the light from stars behind them. • Planetary Nebula are the outer layers of a star that are lost when the star changes from a red giant to a white dwarf. ...
... grains of dust in a nebula. • Dark Nebula are dense clouds of molecular hydrogen which partially or completely absorb the light from stars behind them. • Planetary Nebula are the outer layers of a star that are lost when the star changes from a red giant to a white dwarf. ...
Old Final
... A) the star vibrates B) the star spins and beams of radio waves cross the Earth periodically C) the star accretes matter causing periodic runaway fusion that we observe as pulses D) the star's binary companion periodically blocks the pulsar's constant radio emission E) a black hole near the star abs ...
... A) the star vibrates B) the star spins and beams of radio waves cross the Earth periodically C) the star accretes matter causing periodic runaway fusion that we observe as pulses D) the star's binary companion periodically blocks the pulsar's constant radio emission E) a black hole near the star abs ...
Integrative Studies 410 Our Place in the Universe
... – Estimate distances to galaxies where they occur ...
... – Estimate distances to galaxies where they occur ...
Due: January 15, 2014 Name
... 12. Which effect has been useful (and successful) in the search for and identification of black holes in the universe? a. their magnetic fields and their influence on nearby matter. b. the effect of their angular momentum or spin on nearby matter. c. the influence of their intense gravitational fiel ...
... 12. Which effect has been useful (and successful) in the search for and identification of black holes in the universe? a. their magnetic fields and their influence on nearby matter. b. the effect of their angular momentum or spin on nearby matter. c. the influence of their intense gravitational fiel ...
stars - Chatt
... that can last for weeks and reach 40,000 km high. • Solar Flare: Like a solar prominence, but the gases travel into the corona, and last only a few minutes. ...
... that can last for weeks and reach 40,000 km high. • Solar Flare: Like a solar prominence, but the gases travel into the corona, and last only a few minutes. ...
Life Cycle of a Star
... Step Five Stars bigger than our sun will collapse so quickly they explode into a __________________. The core that is leftover after a supernova may form a ______________ star. If the leftover core was above a certain mass, it will continue to collapse in on itself and form a _______ _________. Its ...
... Step Five Stars bigger than our sun will collapse so quickly they explode into a __________________. The core that is leftover after a supernova may form a ______________ star. If the leftover core was above a certain mass, it will continue to collapse in on itself and form a _______ _________. Its ...
Document
... • Burns or converts H He via theromonuclear fusion in core • When hydrogen in the core is exhausted, converted into helium, the H-burning shell moves outward and the star expands • H-burning phase for another 5 billion years; inert He-core • Stars in H-burning phase are said to be Main Sequence st ...
... • Burns or converts H He via theromonuclear fusion in core • When hydrogen in the core is exhausted, converted into helium, the H-burning shell moves outward and the star expands • H-burning phase for another 5 billion years; inert He-core • Stars in H-burning phase are said to be Main Sequence st ...
Lifecycle of the stars.
... Small proto star-a brown dwarf that was too small to generate enough heat to start fusion. ...
... Small proto star-a brown dwarf that was too small to generate enough heat to start fusion. ...
PHY 150
... blown off after leaving the main sequence, probably becoming a planetary nebula. The white dwarf will probably be about 0.8 MSun. ...
... blown off after leaving the main sequence, probably becoming a planetary nebula. The white dwarf will probably be about 0.8 MSun. ...
The Milky Way Galaxy
... Spiral Structure We know that other galaxies have spiral structure, but it is harder to see the Milky Way’s We find spiral arms by tracing: ...
... Spiral Structure We know that other galaxies have spiral structure, but it is harder to see the Milky Way’s We find spiral arms by tracing: ...
How are galaxies classified
... Q: Fill in the blanks: Most average stars will blow away their outer atmospheres to form a ________. Their cores remain behind and burn as a ______ until they cool down. What is left is a dark ball of matter known as a ______. ...
... Q: Fill in the blanks: Most average stars will blow away their outer atmospheres to form a ________. Their cores remain behind and burn as a ______ until they cool down. What is left is a dark ball of matter known as a ______. ...
Stellar Evolution
... When the hydrogen starts to run out in the core, the explosive energy production of nuclear fusion no longer can balance the gravitational tendency to collapse, and so the core of the star will again start to collapse while hydrogen is still burning on the outside of the core. This gravity collapse ...
... When the hydrogen starts to run out in the core, the explosive energy production of nuclear fusion no longer can balance the gravitational tendency to collapse, and so the core of the star will again start to collapse while hydrogen is still burning on the outside of the core. This gravity collapse ...
The Life of a Star
... life of a low-mass star and that of a star 10 times the Sun’s mass. Low-mass stars cool down and swell up into a red giant. Outer layers drift away and the star shrinks to become a white dwarf which will cool and fade away. High-mass stars swells into a red supergiant which undergoes a supernova. Th ...
... life of a low-mass star and that of a star 10 times the Sun’s mass. Low-mass stars cool down and swell up into a red giant. Outer layers drift away and the star shrinks to become a white dwarf which will cool and fade away. High-mass stars swells into a red supergiant which undergoes a supernova. Th ...
Maybe We Are Alone in the Universe, After All
... civilizations are likely to be scattered among the stars like grains of sand, isolated from one another by the emptiness of interstellar space. Just for Earth's own galaxy, the Milky Way, experts have estimated that there might be up to one million advanced societies. Now, two prominent scientists s ...
... civilizations are likely to be scattered among the stars like grains of sand, isolated from one another by the emptiness of interstellar space. Just for Earth's own galaxy, the Milky Way, experts have estimated that there might be up to one million advanced societies. Now, two prominent scientists s ...
Sample final exam
... 19. On page 184, the text states “Understand the fact that we [the Milky Way] are moving toward M31 and that the Large Magellenic Cloud [LMC] is moving toward us.” First, explain what we observe about these galaxies (M31, the LMC) that shows they are moving in the directions the text states. I thoug ...
... 19. On page 184, the text states “Understand the fact that we [the Milky Way] are moving toward M31 and that the Large Magellenic Cloud [LMC] is moving toward us.” First, explain what we observe about these galaxies (M31, the LMC) that shows they are moving in the directions the text states. I thoug ...
20140319_J.Gan
... The fragile disks of late-type (Sc-Sd) spiral galaxies can be almost entirely destroyed by harassment. The disks lose very substantial amounts of mass. The bound stars are also heated, which transforms the disk into spheroidal component. Dwarf ellipticals are ubiquitous in clusters. For more c ...
... The fragile disks of late-type (Sc-Sd) spiral galaxies can be almost entirely destroyed by harassment. The disks lose very substantial amounts of mass. The bound stars are also heated, which transforms the disk into spheroidal component. Dwarf ellipticals are ubiquitous in clusters. For more c ...
Media Alert A new spin on star-forming galaxies
... He said the majority of stars in the sky today, including our five billion-year-old Sun, were probably born inside these clumpy formations. “The clumpy galaxies produce stars at phenomenal rates,” Dr Obreschkow said. “A new star pops up about once a week, whereas spiral galaxies like our Milky Way o ...
... He said the majority of stars in the sky today, including our five billion-year-old Sun, were probably born inside these clumpy formations. “The clumpy galaxies produce stars at phenomenal rates,” Dr Obreschkow said. “A new star pops up about once a week, whereas spiral galaxies like our Milky Way o ...
Study Guide for the 4TH Astronomy Exam
... Stellar Evolution The successful student will be able to… 1. Star Formation a. Describe the physical characteristics of a giant molecular cloud b. Identify the source of heating (energy production) in protostars c. Explain why more low-mass K & M main sequence stars form rather than the high-mass O ...
... Stellar Evolution The successful student will be able to… 1. Star Formation a. Describe the physical characteristics of a giant molecular cloud b. Identify the source of heating (energy production) in protostars c. Explain why more low-mass K & M main sequence stars form rather than the high-mass O ...
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.