Study Guide - Universe Exam key 2014-15 v2
... 1. Describe the model that was used in the activity titled “Our Expanding Universe.” We used a balloon and put dots on it to represent galaxies. a) How was this model useful? Showed us how galaxies move away from each other as it expands. b) Name 2 limitations of this model. It has boundaries and wi ...
... 1. Describe the model that was used in the activity titled “Our Expanding Universe.” We used a balloon and put dots on it to represent galaxies. a) How was this model useful? Showed us how galaxies move away from each other as it expands. b) Name 2 limitations of this model. It has boundaries and wi ...
Worksheet: Stars and the HR Diagram
... Background: The Hertzsprung-Russell diagram is actually a graph that illustrates the relationship that exists between the average surface temperature of stars and their absolute magnitude, which is how bright they would appear to be if they were al the same distance away. Rather than speak of the br ...
... Background: The Hertzsprung-Russell diagram is actually a graph that illustrates the relationship that exists between the average surface temperature of stars and their absolute magnitude, which is how bright they would appear to be if they were al the same distance away. Rather than speak of the br ...
Stellar Explosions
... High Mass Stars can continue to fuse elements in its core right up to iron (after which the fusion reaction is energetically unfavored) As heavier elements are fused, the reactions go faster and the stage is over more quickly 20-solar-mass star will burn carbon for about 10,000 years, but its iron c ...
... High Mass Stars can continue to fuse elements in its core right up to iron (after which the fusion reaction is energetically unfavored) As heavier elements are fused, the reactions go faster and the stage is over more quickly 20-solar-mass star will burn carbon for about 10,000 years, but its iron c ...
Wednesday, November 7, 2007
... million years, an extremely short time by stellar standards. • They have not had time to move away from their birthplaces. • If stars were being born a few million years ago, they probably still are. • Stars are now being born in their vicinity; these stars are signposts for regions of star formatio ...
... million years, an extremely short time by stellar standards. • They have not had time to move away from their birthplaces. • If stars were being born a few million years ago, they probably still are. • Stars are now being born in their vicinity; these stars are signposts for regions of star formatio ...
Old Final
... There are 10 T/F questions each worth 2 pts., 40 multiple choice questions each worth 5 pts. and your choice of 5 (out of 8 ) long answer questions worth 16 pts. each. True/False ( True = A, False = B , worth 2 pts each) 1. Increasing the density of a cloud makes it easier to form stars there ...
... There are 10 T/F questions each worth 2 pts., 40 multiple choice questions each worth 5 pts. and your choice of 5 (out of 8 ) long answer questions worth 16 pts. each. True/False ( True = A, False = B , worth 2 pts each) 1. Increasing the density of a cloud makes it easier to form stars there ...
1 - Pitt County Schools
... 4. The H-R diagram shows the relationship between what two factors? ___________________________________________________________________________ ___________________________________________________________________________ 5. At what point is a star born? _______________________________________________ ...
... 4. The H-R diagram shows the relationship between what two factors? ___________________________________________________________________________ ___________________________________________________________________________ 5. At what point is a star born? _______________________________________________ ...
The Sun . . .
... H-R Diagram: Diagram that classifies stars according to their luminosity/absolute magnitude, and spectral class based on color and surface temperature. Luminosity: The brightness of a star compared to the Sun. Absolute Magnitude: Compares the brightness of stars from a standard distance ...
... H-R Diagram: Diagram that classifies stars according to their luminosity/absolute magnitude, and spectral class based on color and surface temperature. Luminosity: The brightness of a star compared to the Sun. Absolute Magnitude: Compares the brightness of stars from a standard distance ...
stars - allenscience
... 2. Large stars form a neutron star. 3.The largest of the large will collapse to a point called a black hole. ...
... 2. Large stars form a neutron star. 3.The largest of the large will collapse to a point called a black hole. ...
Slide 1 - cosmos.esa.int
... • But the most likely detection is through the diffuse neutrino background. If they occur at low redshift, they will fit directly in the GADZOOKS energy band. ...
... • But the most likely detection is through the diffuse neutrino background. If they occur at low redshift, they will fit directly in the GADZOOKS energy band. ...
The Universe Constellations
... 13. What percent of stars belong to a multiple star system? 14. The constellation of Centaurus in the Southern Hemisphere contains Omega Centauri, the largest globular star cluster in the Milky Way Galaxy. Describe how globular clusters may have formed. ...
... 13. What percent of stars belong to a multiple star system? 14. The constellation of Centaurus in the Southern Hemisphere contains Omega Centauri, the largest globular star cluster in the Milky Way Galaxy. Describe how globular clusters may have formed. ...
Chapter 13 Practice Questions
... excess energy and therefore will not produce the additional gas pressure to halt the collapse. D) Iron nuclei are so large that they occupy all remaining space and so the collapse ...
... excess energy and therefore will not produce the additional gas pressure to halt the collapse. D) Iron nuclei are so large that they occupy all remaining space and so the collapse ...
Notes - Michigan State University
... • core shrinks until degeneracy pressure sets in and halts collapse star is HOT (gravitational energy !) star is small WD M-R relation Hamada-Salpeter Ap.J. 134 (1961) 683 ...
... • core shrinks until degeneracy pressure sets in and halts collapse star is HOT (gravitational energy !) star is small WD M-R relation Hamada-Salpeter Ap.J. 134 (1961) 683 ...
The Hertzsprung-Russell Diagram
... We see that the H-R Diagram is an extremely useful way to follow the changes that take place as a star evolves. Most stars are on the Main Sequence because that is where stars spend most of their lives, burning hydrogen to helium through nuclear reactions. As stars live out their lives, changes in t ...
... We see that the H-R Diagram is an extremely useful way to follow the changes that take place as a star evolves. Most stars are on the Main Sequence because that is where stars spend most of their lives, burning hydrogen to helium through nuclear reactions. As stars live out their lives, changes in t ...
Stars - Red, Blue, Old, New pt.3
... Some Comments on Stellar Middle Age • The Sun (and other stars less than about 10 solar masses) will never be a supergiant. • Stars more massive than about 10 solar masses do get to be supergiants. • The massive stars fuse elements up to iron and they do it fast…timescales 1000s of years. ...
... Some Comments on Stellar Middle Age • The Sun (and other stars less than about 10 solar masses) will never be a supergiant. • Stars more massive than about 10 solar masses do get to be supergiants. • The massive stars fuse elements up to iron and they do it fast…timescales 1000s of years. ...
Stellar Evolution
... • What are the evolutionary stages of a one solar mass star? • How does the evolution of a high mass star differ from that of a low mass star? • How can the age of a cluster of stars, all formed at the same time, be determined? • Why does fusion stop at Iron? ...
... • What are the evolutionary stages of a one solar mass star? • How does the evolution of a high mass star differ from that of a low mass star? • How can the age of a cluster of stars, all formed at the same time, be determined? • Why does fusion stop at Iron? ...
Life Cycle of a Star
... Nuclear fusion is the engine of the star. Hydrogen will convert to helium at the rate it takes to support the stars mass. For bigger stars, nuclear fusion must occur at a very fast rate in order to balance the star’s gravity. Because of this, larger stars go through the stages much faster than small ...
... Nuclear fusion is the engine of the star. Hydrogen will convert to helium at the rate it takes to support the stars mass. For bigger stars, nuclear fusion must occur at a very fast rate in order to balance the star’s gravity. Because of this, larger stars go through the stages much faster than small ...
Polarimetry & Star
... Winds from O stars account for 30% of recylcable input to ISM Supernovae from O stars throw out much of the remaining mass Biggest contribution of (correlated) supernovae is to “collection” ...
... Winds from O stars account for 30% of recylcable input to ISM Supernovae from O stars throw out much of the remaining mass Biggest contribution of (correlated) supernovae is to “collection” ...
Lab 1-2 : Vocabulary
... Big Bang- theory that all matter and energy in the universe was compressed into an extremely small volume that suddenly began expanding in all directions billions of ...
... Big Bang- theory that all matter and energy in the universe was compressed into an extremely small volume that suddenly began expanding in all directions billions of ...
Review for Midterm 1
... How many stars are typically born in a group and how many groups are typically formed at once? Why? How does spin affect the formation of a star? What are stars formed from and how big is that object? How does the mass of a star affect the time it takes to form? 4. Stellar energy: Where does the ene ...
... How many stars are typically born in a group and how many groups are typically formed at once? Why? How does spin affect the formation of a star? What are stars formed from and how big is that object? How does the mass of a star affect the time it takes to form? 4. Stellar energy: Where does the ene ...
More detailed notes - Particle Physics and Particle Astrophysics
... You may notice that the one-solar-mass track doesn’t have this reversal of direction at the end of the main sequence stage. That’s because in stars using the pp chain, the core is radiative rather than convective: the core material is not mixed, and the very centre of the core runs out of hydrogen w ...
... You may notice that the one-solar-mass track doesn’t have this reversal of direction at the end of the main sequence stage. That’s because in stars using the pp chain, the core is radiative rather than convective: the core material is not mixed, and the very centre of the core runs out of hydrogen w ...
Stellar evolution
Stellar evolution is the process by which a star changes during its lifetime. Depending on the mass of the star, this lifetime ranges from a few million years for the most massive to trillions of years for the least massive, which is considerably longer than the age of the universe. The table shows the lifetimes of stars as a function of their masses. All stars are born from collapsing clouds of gas and dust, often called nebulae or molecular clouds. Over the course of millions of years, these protostars settle down into a state of equilibrium, becoming what is known as a main-sequence star.Nuclear fusion powers a star for most of its life. Initially the energy is generated by the fusion of hydrogen atoms at the core of the main-sequence star. Later, as the preponderance of atoms at the core becomes helium, stars like the Sun begin to fuse hydrogen along a spherical shell surrounding the core. This process causes the star to gradually grow in size, passing through the subgiant stage until it reaches the red giant phase. Stars with at least half the mass of the Sun can also begin to generate energy through the fusion of helium at their core, whereas more-massive stars can fuse heavier elements along a series of concentric shells. Once a star like the Sun has exhausted its nuclear fuel, its core collapses into a dense white dwarf and the outer layers are expelled as a planetary nebula. Stars with around ten or more times the mass of the Sun can explode in a supernova as their inert iron cores collapse into an extremely dense neutron star or black hole. Although the universe is not old enough for any of the smallest red dwarfs to have reached the end of their lives, stellar models suggest they will slowly become brighter and hotter before running out of hydrogen fuel and becoming low-mass white dwarfs.Stellar evolution is not studied by observing the life of a single star, as most stellar changes occur too slowly to be detected, even over many centuries. Instead, astrophysicists come to understand how stars evolve by observing numerous stars at various points in their lifetime, and by simulating stellar structure using computer models.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.