Galaxy Powerpoint
... a) “Nucleus with Arms” b) The center is full of many yellow stars, which makes it look like a nucleus. c) Many spiral arms come out of the nucleus. ...
... a) “Nucleus with Arms” b) The center is full of many yellow stars, which makes it look like a nucleus. c) Many spiral arms come out of the nucleus. ...
Document
... superwinds are not very well understood. However, we know that they exist from observational evidence (the rate of mass loss can be observed). ...
... superwinds are not very well understood. However, we know that they exist from observational evidence (the rate of mass loss can be observed). ...
E5 stellar processes and stellar evolution (HL only)
... • If the core is above 1.4 solar masses (the Chandrasekhar limit) Electrons are forced into protons producing neutrons. • The core is only made of neutrons and contracting rapidly. ...
... • If the core is above 1.4 solar masses (the Chandrasekhar limit) Electrons are forced into protons producing neutrons. • The core is only made of neutrons and contracting rapidly. ...
Exercise 9
... star chart printed on a page, we often forget about the three-dimensional nature of the universe. In this exercise, you will construct (with welding rods and Styrofoam balls) a model of nearby space including many of the nearest stars. Of course, you will need information on where to place the stars ...
... star chart printed on a page, we often forget about the three-dimensional nature of the universe. In this exercise, you will construct (with welding rods and Styrofoam balls) a model of nearby space including many of the nearest stars. Of course, you will need information on where to place the stars ...
lecture2_3
... •Study their motions, measure their speeds •Fundamental to understand the evolution of the sources and how their interact with each other (e.g. merging, collisions) •Measure their redshift, determine their distance from us •Fundamental to chart the large-scale structure of the Universe and to study ...
... •Study their motions, measure their speeds •Fundamental to understand the evolution of the sources and how their interact with each other (e.g. merging, collisions) •Measure their redshift, determine their distance from us •Fundamental to chart the large-scale structure of the Universe and to study ...
The Sun: Not An Average Yellow Star
... The Sun is Above Average Most stars in the Universe are small, cool, low-mass dwarfs. The Sun is larger, hotter, and more massive than these. There are stars that are much larger, very hot, and many times more massive than the Sun. But these stars are quite rare compared to the Sun or the lowmass s ...
... The Sun is Above Average Most stars in the Universe are small, cool, low-mass dwarfs. The Sun is larger, hotter, and more massive than these. There are stars that are much larger, very hot, and many times more massive than the Sun. But these stars are quite rare compared to the Sun or the lowmass s ...
Why is there a main sequence?
... Mmax ~ 100 solar masses a) More massive clouds fragment into smaller pieces during star formation ...
... Mmax ~ 100 solar masses a) More massive clouds fragment into smaller pieces during star formation ...
How Stars and Planets are Born
... due to gravity and shock waves Often other stars forming at same time from other parts of the nebula ...
... due to gravity and shock waves Often other stars forming at same time from other parts of the nebula ...
The Mass-Luminosity Relationship and Stellar Lifetimes
... • Our intuition would seem to say that since big stars have a lot more fuel to consume, they should last a lot longer than smaller stars. • It doesn’t work this way, however. If the luminosity of a star increases with the 4th power of the mass, that means that the star is producing energy and using ...
... • Our intuition would seem to say that since big stars have a lot more fuel to consume, they should last a lot longer than smaller stars. • It doesn’t work this way, however. If the luminosity of a star increases with the 4th power of the mass, that means that the star is producing energy and using ...
Stellar Evolution
... are very large, cool and quite bright. Ex. Betelgeuse is 100,000 times more luminous than the Sun but is only 3,500K on the surface. It’s radius is 1,000 times that of the Sun. ...
... are very large, cool and quite bright. Ex. Betelgeuse is 100,000 times more luminous than the Sun but is only 3,500K on the surface. It’s radius is 1,000 times that of the Sun. ...
PPT - McMaster Physics and Astronomy
... high L, low T); and white dwarfs (lower left: low L, high T). Red giants burn hydrogen in a shell White dwarfs hard to detect – very faint Sun will go through red-giant phase and end up as a cooling white dwarf. Red giant will swell to orbit beyond ...
... high L, low T); and white dwarfs (lower left: low L, high T). Red giants burn hydrogen in a shell White dwarfs hard to detect – very faint Sun will go through red-giant phase and end up as a cooling white dwarf. Red giant will swell to orbit beyond ...
ISP 205 Review Questions, Week 13
... than the Sun? Refer to Fig. 15.12 in the textbook. It is about 3000 times more luminous than the Sun. Once you know the star’s luminosity L, you can calculate its distance r from the measured apparent brightness (or flux) F, using the equations L F 4r 2 L r 4F ...
... than the Sun? Refer to Fig. 15.12 in the textbook. It is about 3000 times more luminous than the Sun. Once you know the star’s luminosity L, you can calculate its distance r from the measured apparent brightness (or flux) F, using the equations L F 4r 2 L r 4F ...
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 ...
Lecture 10: The Milky Way
... This gives us the absolute luminosities of low-mass stars, and using binary systems we can calibrate our models to true masses and radii (see earlier). The trouble is that within 100pc we have no massive stars and only 4 giants – how do we calibrate these? To get distances to objects further away we ...
... This gives us the absolute luminosities of low-mass stars, and using binary systems we can calibrate our models to true masses and radii (see earlier). The trouble is that within 100pc we have no massive stars and only 4 giants – how do we calibrate these? To get distances to objects further away we ...
Oct5
... * All the carbon, oxygen, etc on the Earth, (and in humans) was produced in the centers of stars. * Most carbon, oxygen comes from low-mass red giant winds * Most of the heavy elements come from supernovae * New stars form out of interstellar gas which has been enriched with elements by red giant wi ...
... * All the carbon, oxygen, etc on the Earth, (and in humans) was produced in the centers of stars. * Most carbon, oxygen comes from low-mass red giant winds * Most of the heavy elements come from supernovae * New stars form out of interstellar gas which has been enriched with elements by red giant wi ...
S E N S ` 2 0 0 6
... planets in the Universe) has always remained a question to astronomers, because of the large numbers of candidate planets and systems, founded in near past. Till the end of last year they find at least 192 planets around different kind of stars and star systems [1, 2, 3, 4]. Most of them are not alo ...
... planets in the Universe) has always remained a question to astronomers, because of the large numbers of candidate planets and systems, founded in near past. Till the end of last year they find at least 192 planets around different kind of stars and star systems [1, 2, 3, 4]. Most of them are not alo ...
Summation Packet KEY
... 18. The Andromeda galaxy has a blue shift. How will the Andromeda galaxy affect the Milky Way in the near future? It will move closer. If it continues to move closer, it will eventually collide with the milky way galaxy ...
... 18. The Andromeda galaxy has a blue shift. How will the Andromeda galaxy affect the Milky Way in the near future? It will move closer. If it continues to move closer, it will eventually collide with the milky way galaxy ...
HW #8 Stellar Evolution I Solutions
... luminosity, radius and temperature while on the main sequence, because of the natural thermostat mechanism in main sequence stars. The thermostat mechanism acts to return the core fusion rates back to an equilibrium rate in the event of fluctuations in the core fusion rate. This is known as a negati ...
... luminosity, radius and temperature while on the main sequence, because of the natural thermostat mechanism in main sequence stars. The thermostat mechanism acts to return the core fusion rates back to an equilibrium rate in the event of fluctuations in the core fusion rate. This is known as a negati ...
Stellar Classification and Evolution What is a star? A cloud of gas
... from helium fusion _____________ much of their mass The ejected material expands and cools, becoming a planetary ________________ (which actually has nothing to do with planets, but we didn’t know that in the 18th century when Herschel coined the term) The core _____________________ to form a Wh ...
... from helium fusion _____________ much of their mass The ejected material expands and cools, becoming a planetary ________________ (which actually has nothing to do with planets, but we didn’t know that in the 18th century when Herschel coined the term) The core _____________________ to form a Wh ...
The First Stars in the Universe
... sources such as quasars. Future observations of distant objects may help determine when the universe’s helium was ionized. If the first stars were indeed very massive, they would also have had relatively short lifetimes—only a few million years. Some of the stars would have exploded as supernovae at ...
... sources such as quasars. Future observations of distant objects may help determine when the universe’s helium was ionized. If the first stars were indeed very massive, they would also have had relatively short lifetimes—only a few million years. Some of the stars would have exploded as supernovae at ...
Lesson 2 Power Notes Outline
... If an object’s color depends only on temperature, the object is called a blackbody. ...
... If an object’s color depends only on temperature, the object is called a blackbody. ...
The Family of Stars
... Type I: No hydrogen lines in the spectrum Type II: Hydrogen lines in the spectrum ...
... Type I: No hydrogen lines in the spectrum Type II: Hydrogen lines in the spectrum ...
RED GIANTS
... • pressure at core is enormous • hydrogen combines to form helium and releases energy • helium combines to form carbon and releases energy • process continues to produce heavier ...
... • pressure at core is enormous • hydrogen combines to form helium and releases energy • helium combines to form carbon and releases energy • process continues to produce heavier ...
PHYSICS 1500 - ASTRONOMY TOTAL
... Neither Mars nor Venus have conditions to support a rich biosphere. Which of the following is not a contributing factor to this situation? (a) Mars is close to the asteroid belt, which resulted in widespread cratering in the heavy bombardment period. (b) Venus is a little close to the sun, resulting ...
... Neither Mars nor Venus have conditions to support a rich biosphere. Which of the following is not a contributing factor to this situation? (a) Mars is close to the asteroid belt, which resulted in widespread cratering in the heavy bombardment period. (b) Venus is a little close to the sun, resulting ...
Powerpoint of lecture 3
... and constant volume, we can find (see blackboard) an integral expression for the total internal energy, U. • Using Theorem II, if is constant throughout the star, we can then prove the Virial Theorem: ...
... and constant volume, we can find (see blackboard) an integral expression for the total internal energy, U. • Using Theorem II, if is constant throughout the star, we can then prove the Virial Theorem: ...
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.