Unit 11 Guide: Concepts of Earth Science Stars, Galaxies, and the
... Milky Way galaxy? 2. What evidence do scientists use to support the Big Bang Theory? Explain the sequence of events predicted by the Big Bang Theory. 3. Explain Hubble’s Law. 4. Compare and contrast the apparent and actual motion of stars. How can scientists know if a star or galaxy is moving toward ...
... Milky Way galaxy? 2. What evidence do scientists use to support the Big Bang Theory? Explain the sequence of events predicted by the Big Bang Theory. 3. Explain Hubble’s Law. 4. Compare and contrast the apparent and actual motion of stars. How can scientists know if a star or galaxy is moving toward ...
Astronomy Objectives
... Evolution of low mass (red dwarf) stars, medium mass main sequence stars, massive stars, all from nebulae to their final phases ...
... Evolution of low mass (red dwarf) stars, medium mass main sequence stars, massive stars, all from nebulae to their final phases ...
Life cycle of a star
... star) is now in its final stages. The core becomes a White Dwarf the star eventually cools and dims. When it stops shining, the now dead star is called a Black Dwarf. ...
... star) is now in its final stages. The core becomes a White Dwarf the star eventually cools and dims. When it stops shining, the now dead star is called a Black Dwarf. ...
Where Stars Are Born
... 1. What is the composition of interstellar gas? Of interstellar dust? 2. If space is a near-perfect vacuum, how can there be enough dust in it to block light? 3. What is an emission nebula? 4. How is interstellar dust detected? 5. Why is dust found in the neighborhood of some stars (as in the Pleiad ...
... 1. What is the composition of interstellar gas? Of interstellar dust? 2. If space is a near-perfect vacuum, how can there be enough dust in it to block light? 3. What is an emission nebula? 4. How is interstellar dust detected? 5. Why is dust found in the neighborhood of some stars (as in the Pleiad ...
1. a. Collisionless Boltzmann—particles moving in smooth potential
... photographic standards. In blue light the spiral arms stand out more (why?). a. Clusters of galaxies are dominated by early type galaxies, E & S0 classes, with few spirals. This is thought to be the result of environmental processes including ram pressure stripping of gas and tidal disruption/thicke ...
... photographic standards. In blue light the spiral arms stand out more (why?). a. Clusters of galaxies are dominated by early type galaxies, E & S0 classes, with few spirals. This is thought to be the result of environmental processes including ram pressure stripping of gas and tidal disruption/thicke ...
Astronomy - The-A-List
... Stellar evolution, including spectral features and chemical composition, luminosity, blackbody radiation, color index (B-V), and HR Diagram transitions, stellar nurseries and star formation, protostars, main sequence stars ...
... Stellar evolution, including spectral features and chemical composition, luminosity, blackbody radiation, color index (B-V), and HR Diagram transitions, stellar nurseries and star formation, protostars, main sequence stars ...
Name: Period : ______ The Universe – Life and Death of a Star How
... 26. While our Sun is a cosmic loner, more than half of all stars are part of _______________________. 27. When a white dwarf pulls in enough material from its companion star and explodes, it is known as a Type 1-A _________________________. 28. Although a supernova is very bright, the visible light ...
... 26. While our Sun is a cosmic loner, more than half of all stars are part of _______________________. 27. When a white dwarf pulls in enough material from its companion star and explodes, it is known as a Type 1-A _________________________. 28. Although a supernova is very bright, the visible light ...
The Evolution of Massive Stars
... of “metal-rich” debris from a supernova in about 1680: today the brightest radio source in the sky ...
... of “metal-rich” debris from a supernova in about 1680: today the brightest radio source in the sky ...
PHYSICS 1500 ASTRONOMY Sample Exam Solutions Section B
... (a) It seems that all Type I supernovae have about the same intrinsic luminosity at their peak. Therefore, if we observe one in a distant galaxy, we can compare its apparent brightness with its expected intrinsic brightness to estimate its distance. This will also be the distance to the galaxy in wh ...
... (a) It seems that all Type I supernovae have about the same intrinsic luminosity at their peak. Therefore, if we observe one in a distant galaxy, we can compare its apparent brightness with its expected intrinsic brightness to estimate its distance. This will also be the distance to the galaxy in wh ...
Stellar_Evol
... • Not all stars fuse H into He • Helium can be fused to Carbon, Carbon to nitrogen and more… • All to produce enough energy to fight ...
... • Not all stars fuse H into He • Helium can be fused to Carbon, Carbon to nitrogen and more… • All to produce enough energy to fight ...
Chapter 7 Review Answers
... at the beginning of the universe (BBT) went. That extra radiation should be present throughout the universe if the BBT was to be true. We believe now that the cosmic background radiation is that extra energy/radiation. The CBR found fits with the predictions consistent with the BBT, supporting the B ...
... at the beginning of the universe (BBT) went. That extra radiation should be present throughout the universe if the BBT was to be true. We believe now that the cosmic background radiation is that extra energy/radiation. The CBR found fits with the predictions consistent with the BBT, supporting the B ...
stars and galaxies – study guide
... 21. Hydrogen is the “fuel” of the sun. 22. By using a tool called a spectroscope astronomers can identify the elements in a star. 23. On an H-R Diagram, stars are classified by temperature and absolute magnitude. 24. What is the next stage of the sun? Red Giant 25. An example of a winter constellat ...
... 21. Hydrogen is the “fuel” of the sun. 22. By using a tool called a spectroscope astronomers can identify the elements in a star. 23. On an H-R Diagram, stars are classified by temperature and absolute magnitude. 24. What is the next stage of the sun? Red Giant 25. An example of a winter constellat ...
Homework 1 - Course Pages of Physics Department
... t1/2 (235) = 0.704 × 109 a ja t1/2 (238) = 4.47 × 109 a. The ratio of their abundances on earth is 235 U/238 U = 0.00725. When were they equal in abundance? The heavy elements were created in supernova explosions and mixed with the interstellar gas and dust, from which the earth was formed. Accordin ...
... t1/2 (235) = 0.704 × 109 a ja t1/2 (238) = 4.47 × 109 a. The ratio of their abundances on earth is 235 U/238 U = 0.00725. When were they equal in abundance? The heavy elements were created in supernova explosions and mixed with the interstellar gas and dust, from which the earth was formed. Accordin ...
Sample exam 2
... 11. The Sun started off its trajectory on the Hertzsprung-Russell diagram by initially moving down and to the left as it organized into a protostar. Explain this behavior in terms of temperature and luminosity, and give a reason for this behavior, given what we know about stars. 12. What are the con ...
... 11. The Sun started off its trajectory on the Hertzsprung-Russell diagram by initially moving down and to the left as it organized into a protostar. Explain this behavior in terms of temperature and luminosity, and give a reason for this behavior, given what we know about stars. 12. What are the con ...
General Astrophysical Concepts: Astronomical length scales
... nucleus of a quasar is about five million times the mass of our Sun The light-emitting region of a typical quasar is comparable in size to our Solar System Quasars and AGNs can be 100 to 1000 times more luminous than our Milky Way galaxy Most galaxies have massive black holes at their centers ...
... nucleus of a quasar is about five million times the mass of our Sun The light-emitting region of a typical quasar is comparable in size to our Solar System Quasars and AGNs can be 100 to 1000 times more luminous than our Milky Way galaxy Most galaxies have massive black holes at their centers ...
Stellar Nucleosynthesis
... • These reactions created the heavier elements from fusing together lighter elements. • When the outer layers of a star are thrown back into space (supernovae), the processed material can be incorporated into gas clouds that will later form stars and planets. • The material that formed our solar sys ...
... • These reactions created the heavier elements from fusing together lighter elements. • When the outer layers of a star are thrown back into space (supernovae), the processed material can be incorporated into gas clouds that will later form stars and planets. • The material that formed our solar sys ...
Ch.21 Stars, Galaxies, and the Universe Section 3: Lives of Stars
... o A Star is Born Nebula: is a large cloud of gas and dust spread out in an immense volume Protostar: earliest stage of a star’s life A star is born when the contracting gas and dust from a nebula become so dense and hot that nuclear fusion starts o Lifetimes of Stars How long a star lives de ...
... o A Star is Born Nebula: is a large cloud of gas and dust spread out in an immense volume Protostar: earliest stage of a star’s life A star is born when the contracting gas and dust from a nebula become so dense and hot that nuclear fusion starts o Lifetimes of Stars How long a star lives de ...
Characteristics of Stars
... Measuring distances to stars • Measure parallax – the apparent shift in the position of an object when viewed from two different positions. • Knowing the angle that the star’s position changes and the size of Earth’s orbit, astronomers can calculate the distance of the star from earth. ...
... Measuring distances to stars • Measure parallax – the apparent shift in the position of an object when viewed from two different positions. • Knowing the angle that the star’s position changes and the size of Earth’s orbit, astronomers can calculate the distance of the star from earth. ...
CH27.2 Stellar Evolution
... NONE are yet known to exist…..our universe isn’t thought to be old enough for this to happen yet! ...
... NONE are yet known to exist…..our universe isn’t thought to be old enough for this to happen yet! ...
Stars and Their Characteristics
... measure star distance • The nearest stars have the largest parallax angles, while those of distant stars are too small to measure ...
... measure star distance • The nearest stars have the largest parallax angles, while those of distant stars are too small to measure ...
Fusion in the Sun
... During NUCLEAR FUSION the sun converts matter (elements) into energy (radiation) in the CORE of the star. The sun fuses 4 HYDROGEN nucleus/atoms into 1 HELIUM nucleus/atom. A result of this is the creation of massive amounts of RADIATION ENERGY. ...
... During NUCLEAR FUSION the sun converts matter (elements) into energy (radiation) in the CORE of the star. The sun fuses 4 HYDROGEN nucleus/atoms into 1 HELIUM nucleus/atom. A result of this is the creation of massive amounts of RADIATION ENERGY. ...
Solar System
... Solar System Notes – Part 1 Universe: all of space and ________________________________________________ Galaxy: A large group of __________________________________, solar systems, and associated gas and dust in space that is bound by _____________________________ Solar System: Composed of one ...
... Solar System Notes – Part 1 Universe: all of space and ________________________________________________ Galaxy: A large group of __________________________________, solar systems, and associated gas and dust in space that is bound by _____________________________ Solar System: Composed of one ...
Astronomy 1001
... • Our solar system is about halfway out in Milky Way Galaxy • Milky Way is part of the Local Group • Local Group is part of the Local Supercluster ...
... • Our solar system is about halfway out in Milky Way Galaxy • Milky Way is part of the Local Group • Local Group is part of the Local Supercluster ...
ASTR2050 Spring 2005 • In this class we will ...
... of individual stellar radii See Studio Laboratory this Friday ...
... of individual stellar radii See Studio Laboratory this Friday ...
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.