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... that star is made of. • Prisms can be used to separate the colors of white light. The various wavelengths making up white light bend at different angles when they pass through the prism. They separate from each other and the colors of the visible light spectrum become visible. • The visible light sp ...
... that star is made of. • Prisms can be used to separate the colors of white light. The various wavelengths making up white light bend at different angles when they pass through the prism. They separate from each other and the colors of the visible light spectrum become visible. • The visible light sp ...
6. 1 Star Distances 6. 2 Apparent Brightness, Intrinsic Brightness
... We see a single point of light, and only by taking a spectrum can we determine that there are two stars. ...
... We see a single point of light, and only by taking a spectrum can we determine that there are two stars. ...
Protostar formation
... on one hand, gravitational force pushes inward, while on the other hand internal pressure due to the nuclear reactions pushes outward. ...
... on one hand, gravitational force pushes inward, while on the other hand internal pressure due to the nuclear reactions pushes outward. ...
Study Guide for the Comprehensive Final Exam
... Interpret stellar apparent magnitudes and their relationship to brightness. Interpret stellar absolute magnitudes and their relationship to luminosity. Solve problems relating to the relative brightness or luminosity of two stars given their m or M values. Determine the hottest and coolest stars fro ...
... Interpret stellar apparent magnitudes and their relationship to brightness. Interpret stellar absolute magnitudes and their relationship to luminosity. Solve problems relating to the relative brightness or luminosity of two stars given their m or M values. Determine the hottest and coolest stars fro ...
Astronomy Homework - Life
... have enough mass to allow temperatures high enough for carbon fusion. 19. The temperature at which carbon will fuse is (100,000,000°°K/600,000,000°°K). 20. The carbon core of a star becomes degenerate which means (it cannot be squeezed any further/its about to do a bad thing). 20. Stars that begin t ...
... have enough mass to allow temperatures high enough for carbon fusion. 19. The temperature at which carbon will fuse is (100,000,000°°K/600,000,000°°K). 20. The carbon core of a star becomes degenerate which means (it cannot be squeezed any further/its about to do a bad thing). 20. Stars that begin t ...
Chapter 5 Galaxies and Star Systems
... between the stars. Because there is little gas or dust, stars are no longer forming. Most elliptical galaxies contain only old stars. Some galaxies do not have regular shapes, thus they are called irregular galaxies. These galaxies are typically smaller than other types of galaxies and generally hav ...
... between the stars. Because there is little gas or dust, stars are no longer forming. Most elliptical galaxies contain only old stars. Some galaxies do not have regular shapes, thus they are called irregular galaxies. These galaxies are typically smaller than other types of galaxies and generally hav ...
Lecture 2+3 - University of Texas Astronomy Home Page
... When the high mass star dies - its core becomes a neutron star or black hole, - its central and outer layers of gas containing H, He, C, and N, O, Sulfur, Silicon, Iron are blown out by a supernova (SN) explosion, and form a SN remnant, made of hot glowing gas. The remnant enriches surrounding gas w ...
... When the high mass star dies - its core becomes a neutron star or black hole, - its central and outer layers of gas containing H, He, C, and N, O, Sulfur, Silicon, Iron are blown out by a supernova (SN) explosion, and form a SN remnant, made of hot glowing gas. The remnant enriches surrounding gas w ...
Spectra of stars
... The continuous spectrum originates from the surface of the star and the absorption lines are produced when light passes upwards and outwards through the tenuous upper layers of the star. By looking at the spectrum of a star astronomers can determine: (a) the temperature of the star (b) the velocity ...
... The continuous spectrum originates from the surface of the star and the absorption lines are produced when light passes upwards and outwards through the tenuous upper layers of the star. By looking at the spectrum of a star astronomers can determine: (a) the temperature of the star (b) the velocity ...
Homework #3 10 points Question #1 (2 pts) The brightest star in the
... iron? You can think the following way: let’s imagine that in a region of space A we found one massive star that exploded as a core collapse supernova, and in a region of space B we found several white dwarfs that all exploded as thermonuclear supernovae. The number of white dwarfs in the region B is ...
... iron? You can think the following way: let’s imagine that in a region of space A we found one massive star that exploded as a core collapse supernova, and in a region of space B we found several white dwarfs that all exploded as thermonuclear supernovae. The number of white dwarfs in the region B is ...
M13 – The Great Hercules Cluster
... a warm June night and look up at the stars. Everything you see is just a small part of the much larger collection of stars called the Milky Way Galaxy. Our star, the Sun, is only one of more than a hundred billion other stars in the Milky Way. This galaxy of ours is shaped like a flat, circular disk ...
... a warm June night and look up at the stars. Everything you see is just a small part of the much larger collection of stars called the Milky Way Galaxy. Our star, the Sun, is only one of more than a hundred billion other stars in the Milky Way. This galaxy of ours is shaped like a flat, circular disk ...
stellar_explosions - UT Austin (Astronomy)
... A.D. SN? Observed radial velocities of a few thousand km/sec gives age, which comes out to be about 950 years as it should. See Discovery 21-2 on p. 566. From the observed number of SNe (supernovae) in our own and other galaxies, we expect about 1 SN per 100 years in our Galaxy. But the last one was ...
... A.D. SN? Observed radial velocities of a few thousand km/sec gives age, which comes out to be about 950 years as it should. See Discovery 21-2 on p. 566. From the observed number of SNe (supernovae) in our own and other galaxies, we expect about 1 SN per 100 years in our Galaxy. But the last one was ...
Classification and structure of galaxies
... • Stars and star clusters – microwaves generated by water from H II regions (called the MASER technique) traces the Milky Way’s spiral arms • Nebulae – infrared light (detected by the Spitzer Space Telescope) shows the outline of the heat generated by the bar • Other galaxies (analogous structure as ...
... • Stars and star clusters – microwaves generated by water from H II regions (called the MASER technique) traces the Milky Way’s spiral arms • Nebulae – infrared light (detected by the Spitzer Space Telescope) shows the outline of the heat generated by the bar • Other galaxies (analogous structure as ...
HNRS 227 Lecture #2 Chapters 2 and 3
... Young star clusters give insight into star formation and evolution Newborn stars may form an open or galactic cluster Stars are held together in such a cluster by gravity Occasionally a star moving more rapidly than average will escape, or leave the cluster A stellar association is a group ...
... Young star clusters give insight into star formation and evolution Newborn stars may form an open or galactic cluster Stars are held together in such a cluster by gravity Occasionally a star moving more rapidly than average will escape, or leave the cluster A stellar association is a group ...
doc - University of Texas Astronomy
... intermediate mass BH in center of globular cluster. Now plenty are known. At the centers of galaxies: Stars and gas very near the centers of galaxies (including our own) are moving very rapidly, orbiting some unseen object. Masses inferred from Newton’s laws are millions to billions of solar masses! ...
... intermediate mass BH in center of globular cluster. Now plenty are known. At the centers of galaxies: Stars and gas very near the centers of galaxies (including our own) are moving very rapidly, orbiting some unseen object. Masses inferred from Newton’s laws are millions to billions of solar masses! ...
Life Cycle of Stars
... 4. The star then switches on and begins to shine. 5. Inside every newborn star, hydrogen atoms are fused together to make helium, this process is called fusion, and it creates the energy of every star. 6. What happens to a star during the rest of its life depends on how massive it is at its birth. 7 ...
... 4. The star then switches on and begins to shine. 5. Inside every newborn star, hydrogen atoms are fused together to make helium, this process is called fusion, and it creates the energy of every star. 6. What happens to a star during the rest of its life depends on how massive it is at its birth. 7 ...
A105 Stars and Galaxies
... What about Massive Stars? • Massive stars continue to generate energy by nuclear reactions until they have converted all the hydrogen and helium in their cores into iron. • Once the core is iron, no more energy can be generated • The core collapses and the star explodes ...
... What about Massive Stars? • Massive stars continue to generate energy by nuclear reactions until they have converted all the hydrogen and helium in their cores into iron. • Once the core is iron, no more energy can be generated • The core collapses and the star explodes ...
Spectroscopy – the study of the colors of light (the spectrum) given
... Second , the luminosity must be found. Finding the luminosity is either: easy, if the distance to the star and the apparent brightness are known they can be used to find the luminosity from the inverse square law; or it is impossible, if the distance isn’t known. ...
... Second , the luminosity must be found. Finding the luminosity is either: easy, if the distance to the star and the apparent brightness are known they can be used to find the luminosity from the inverse square law; or it is impossible, if the distance isn’t known. ...
Chapter 8 - TeacherWeb
... or spheres. Usually have bright centers with very little dust and gas. Contain mostly old stars---b/c little to no gas to form new stars. Two types: giant elliptical galaxies and dwarf elliptical galaxies. Irregular Galaxies: galaxies that don’t fit into any certain category or class. Their shape is ...
... or spheres. Usually have bright centers with very little dust and gas. Contain mostly old stars---b/c little to no gas to form new stars. Two types: giant elliptical galaxies and dwarf elliptical galaxies. Irregular Galaxies: galaxies that don’t fit into any certain category or class. Their shape is ...
I CAN SEE THE STARS IN YOUR EYES
... Your space craft begins to travel at the speed of light, taking you towards the sun. Traveling at this speed, the trip from Earth to the sun, a distance of 93 million miles, would take about 8 minutes, not very long for such a long trip! Yet, to get to the next closest star, Proxima Centauri, would ...
... Your space craft begins to travel at the speed of light, taking you towards the sun. Traveling at this speed, the trip from Earth to the sun, a distance of 93 million miles, would take about 8 minutes, not very long for such a long trip! Yet, to get to the next closest star, Proxima Centauri, would ...
15 - Edmodo
... The purpose of this activity will be to use the star chart (Page 551 of your textbook) to determine the location and appearance of well known stars, constellations, and asterisms visible in the ...
... The purpose of this activity will be to use the star chart (Page 551 of your textbook) to determine the location and appearance of well known stars, constellations, and asterisms visible in the ...
Stellar kinematics
Stellar kinematics is the study of the movement of stars without needing to understand how they acquired their motion. This differs from stellar dynamics, which takes into account gravitational effects. The motion of a star relative to the Sun can provide useful information about the origin and age of a star, as well as the structure and evolution of the surrounding part of the Milky Way.In astronomy, it is widely accepted that most stars are born within molecular clouds known as stellar nurseries. The stars formed within such a cloud compose open clusters containing dozens to thousands of members. These clusters dissociate over time. Stars that separate themselves from the cluster's core are designated as members of the cluster's stellar association. If the remnant later drifts through the Milky Way as a coherent assemblage, then it is termed a moving group.