Characteristics of Stars
... f. shines brightly in the center of a distant galaxy because of the friction of material spiraling around it ...
... f. shines brightly in the center of a distant galaxy because of the friction of material spiraling around it ...
galaxy.
... This does not mean we are at the center of the universe. The entire universe is expanding, so the distance between all galaxies is increasing (except ones close enough to be bound together by gravity). If we lived in another distant galaxy, we would see all ...
... This does not mean we are at the center of the universe. The entire universe is expanding, so the distance between all galaxies is increasing (except ones close enough to be bound together by gravity). If we lived in another distant galaxy, we would see all ...
Astronomy HOMEWORK Chapter 12 - 9th Edition 1. Consider a star
... Answer: Cepheids are stars which pulsate in brightness in a distinctive way due to a thermal instability. A higher-mass star becomes a Cepheid when its evolutionary path takes it across the instability strip. The most important characteristic of Cepheids is that their pulsation period correltates wi ...
... Answer: Cepheids are stars which pulsate in brightness in a distinctive way due to a thermal instability. A higher-mass star becomes a Cepheid when its evolutionary path takes it across the instability strip. The most important characteristic of Cepheids is that their pulsation period correltates wi ...
Mars Project
... All star start their lives as a dense part of a nebula. (A big cloud of gas and dust spread out in space.) in the dense part of the nebula the gas and dust becomes so dense and hot that a star is born. ...
... All star start their lives as a dense part of a nebula. (A big cloud of gas and dust spread out in space.) in the dense part of the nebula the gas and dust becomes so dense and hot that a star is born. ...
Lecture 11 - Stars and Atomic Spectra
... Masses of stars • Spectral lines also allow us to measure the velocities of stars via the Doppler shift that we discussed in searching for extra-solar planets. Doppler shift measurements are ...
... Masses of stars • Spectral lines also allow us to measure the velocities of stars via the Doppler shift that we discussed in searching for extra-solar planets. Doppler shift measurements are ...
PowerPoint Presentation - Super Massive Black Holes
... around black holes that are thought to produce the spectacular jets of high-energy particles rushing away from black holes come from the disk of hot gas around the black hole, not the black ...
... around black holes that are thought to produce the spectacular jets of high-energy particles rushing away from black holes come from the disk of hot gas around the black hole, not the black ...
notes
... Most galaxies are between 3,000 and 400,000 light years in diameter and can contain billions or trillions of stars. The Milky Way, our galaxy, is thought to be between 100,000 and 200,000 light years in diameter and contain between 100 and 400 billion stars, the most ancient of which are 13.7 billio ...
... Most galaxies are between 3,000 and 400,000 light years in diameter and can contain billions or trillions of stars. The Milky Way, our galaxy, is thought to be between 100,000 and 200,000 light years in diameter and contain between 100 and 400 billion stars, the most ancient of which are 13.7 billio ...
14_creationism
... • Birth: collapse of gas cloud forms protostar. • Main sequence: center of star becomes hot ...
... • Birth: collapse of gas cloud forms protostar. • Main sequence: center of star becomes hot ...
UNIT VIII/B: THE EARTH IN SPACE – STARS AND GALAXIES
... * Spiral galaxies, which are typically disk-shaped with a somewhat greater concentration of stars near their centers, often containing arms of stars extending from their central nucleus *Barred spiral galaxies, a type of spiral galaxy that has the stars arranged in the shape of a bar, which rotates ...
... * Spiral galaxies, which are typically disk-shaped with a somewhat greater concentration of stars near their centers, often containing arms of stars extending from their central nucleus *Barred spiral galaxies, a type of spiral galaxy that has the stars arranged in the shape of a bar, which rotates ...
Spectral Classification and the HR Diagram
... Catalogue. Because it was the goal of this project to classify a sufficient number of stars so that it would be years before anyone felt the need to repeat such an undertaking, it was Pickering's goal to classify at least 100,000 stars for the Henry Draper (HD) Catalogue. By World War I, objective p ...
... Catalogue. Because it was the goal of this project to classify a sufficient number of stars so that it would be years before anyone felt the need to repeat such an undertaking, it was Pickering's goal to classify at least 100,000 stars for the Henry Draper (HD) Catalogue. By World War I, objective p ...
Integrative Studies 410 Our Place in the Universe
... • Ellipticals with a bulge and thin disk, but no spiral arms ...
... • Ellipticals with a bulge and thin disk, but no spiral arms ...
Distance to Stars
... km/s – 1 light year = the distance a ray of light travels in 1 year. 9.5 trillion km. Horsehead Nebula is 1,500 light years away) ...
... km/s – 1 light year = the distance a ray of light travels in 1 year. 9.5 trillion km. Horsehead Nebula is 1,500 light years away) ...
Stellar Evolution Lab
... Stage 1- Stars are born in clouds of gas and dust called Nebulas. Stage 2- The gas and dust spiral together and contract under their own gravity. The gas and dust will begin to heat up and start to glow forming Protostars. Stage 3- If a protostar contains enough matter, the central temperature will ...
... Stage 1- Stars are born in clouds of gas and dust called Nebulas. Stage 2- The gas and dust spiral together and contract under their own gravity. The gas and dust will begin to heat up and start to glow forming Protostars. Stage 3- If a protostar contains enough matter, the central temperature will ...
12.4 Evolution of Stars More Massive than the Sun
... Its path across the H-R diagram is essentially a straight line – it stays as just about the same luminosity as it cools off. Eventually the star dies in a violent explosion called a supernova. ...
... Its path across the H-R diagram is essentially a straight line – it stays as just about the same luminosity as it cools off. Eventually the star dies in a violent explosion called a supernova. ...
ASTRONOMY: WHAT DO YOU NEED TO KNOW
... What is degenerate matter? Where is it found? Degenerate matter is high density matter whose temperature no longer depends on temperature. It is a gas but resists compression. It is found in white dwarfs near the end of a star’s lifetime. Know the characteristics and lifespan characteristics of red ...
... What is degenerate matter? Where is it found? Degenerate matter is high density matter whose temperature no longer depends on temperature. It is a gas but resists compression. It is found in white dwarfs near the end of a star’s lifetime. Know the characteristics and lifespan characteristics of red ...
Understanding Stars
... Extremely dense things (opaque gases, liquids or solids) the atoms are too close – Emit a continuous spectrum • photosphere Stefan-Boltzman Law A dense hot object emits light of all colors – More of one color than others • “peak” color – The peak color is determined by the temperature • Hotter = blu ...
... Extremely dense things (opaque gases, liquids or solids) the atoms are too close – Emit a continuous spectrum • photosphere Stefan-Boltzman Law A dense hot object emits light of all colors – More of one color than others • “peak” color – The peak color is determined by the temperature • Hotter = blu ...
Stars
... Life span of a star depends on its size and mass. – Very large, massive stars burn their fuel much faster than smaller stars – Their main sequence may last only a few hundred thousand years – Smaller stars will live on for billions of years because they burn their fuel much more slowly ...
... Life span of a star depends on its size and mass. – Very large, massive stars burn their fuel much faster than smaller stars – Their main sequence may last only a few hundred thousand years – Smaller stars will live on for billions of years because they burn their fuel much more slowly ...
Living alongside Monsters: Matter around Central Massive Black Holes Q. Daniel Wang
... 39’ (300 light-year) • Distance to the Galactic center: 26,000 light-year • Resolution: 0.025 light-year (0.2”) • 144 HST orbits, taken between Feb and June, 2008 144X4X4=2304 images for each of the two wavelength filters ...
... 39’ (300 light-year) • Distance to the Galactic center: 26,000 light-year • Resolution: 0.025 light-year (0.2”) • 144 HST orbits, taken between Feb and June, 2008 144X4X4=2304 images for each of the two wavelength filters ...
The Inverse Square Law and Surface Area
... Earth is called the intensity (I) of the star’s radiation This is related to the power output per metre squared L of the star’s surface in this way ...
... Earth is called the intensity (I) of the star’s radiation This is related to the power output per metre squared L of the star’s surface in this way ...
November 2013 - Pomona Valley Amateur Astronomers
... unevenness of the background may be caused by photons being shadowed by areas of greater and lesser density of mass. There is a bit of uncertainty which depends on how and when one thinks those photons started out. If this happened many times before the earliest galaxies we have seen, it could expla ...
... unevenness of the background may be caused by photons being shadowed by areas of greater and lesser density of mass. There is a bit of uncertainty which depends on how and when one thinks those photons started out. If this happened many times before the earliest galaxies we have seen, it could expla ...
Galaxy clusters - University of Iowa Astrophysics
... source, we can figure out the total mass in the lens. This provides an independent confirmation of dark matter. • A lense can act as a huge telescope. The deepest images of the most distant galaxies are obtained with clusters acting as gravitational lenses. ...
... source, we can figure out the total mass in the lens. This provides an independent confirmation of dark matter. • A lense can act as a huge telescope. The deepest images of the most distant galaxies are obtained with clusters acting as gravitational lenses. ...
AN INTRODUCTION TO ASTRONOMY Dr. Uri Griv •
... Explanation: How could a galaxy become shaped like a ring? The rim of the blue galaxy pictured on the right is an immense ring-like structure 150,000 light years in diameter composed of newly formed, extremely bright, massive stars. That galaxy, AM 0644-741, is known as a ring galaxy and was caused ...
... Explanation: How could a galaxy become shaped like a ring? The rim of the blue galaxy pictured on the right is an immense ring-like structure 150,000 light years in diameter composed of newly formed, extremely bright, massive stars. That galaxy, AM 0644-741, is known as a ring galaxy and was caused ...
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.