Astronomy 1001/1005 Final Exam (250 points)
... You will NOT get your bubble sheet back One page of notes is allowed Use a #2 pencil on the bubble sheet. Make your bubbles dark and neat. There are 50 multiple choice problems and your choice of 5 short answer questions with point values given for each. ...
... You will NOT get your bubble sheet back One page of notes is allowed Use a #2 pencil on the bubble sheet. Make your bubbles dark and neat. There are 50 multiple choice problems and your choice of 5 short answer questions with point values given for each. ...
Charterhouse2-gelletly-elements
... Recoilling nuclei from the target are separated from the beam particles and from each other by mass as they pass through the crossed electric and magnetic fields of the spectrometer. The reactions of interest are where the two nuclei fuse gently and so there is little internal energy. As a result on ...
... Recoilling nuclei from the target are separated from the beam particles and from each other by mass as they pass through the crossed electric and magnetic fields of the spectrometer. The reactions of interest are where the two nuclei fuse gently and so there is little internal energy. As a result on ...
gelletly-Charterhouse2-elements
... Recoilling nuclei from the target are separated from the beam particles and from each other by mass as they pass through the crossed electric and magnetic fields of the spectrometer. The reactions of interest are where the two nuclei fuse gently and so there is little internal energy. As a result on ...
... Recoilling nuclei from the target are separated from the beam particles and from each other by mass as they pass through the crossed electric and magnetic fields of the spectrometer. The reactions of interest are where the two nuclei fuse gently and so there is little internal energy. As a result on ...
It all began with a Big Bang!
... about 14 billion years ago The Big Bang The Universe began in a Big Bang about 14 billion years ago. At that time, the entire Universe was inside a bubble that was thousands of times smaller than a pinhead. It was hotter and denser than anything we can imagine. Then it suddenly exploded. The Univers ...
... about 14 billion years ago The Big Bang The Universe began in a Big Bang about 14 billion years ago. At that time, the entire Universe was inside a bubble that was thousands of times smaller than a pinhead. It was hotter and denser than anything we can imagine. Then it suddenly exploded. The Univers ...
M - UC Berkeley Astronomy w
... A classic problem in astronomy in the context of the mass distribution of molecular cloud core masses. Measurements of the absolute magnitude of the stars in the solar neighborhood revealed a preponderance of large magnitudes, I.e., faint low-mass stars. This is due to the long main-sequence lifetim ...
... A classic problem in astronomy in the context of the mass distribution of molecular cloud core masses. Measurements of the absolute magnitude of the stars in the solar neighborhood revealed a preponderance of large magnitudes, I.e., faint low-mass stars. This is due to the long main-sequence lifetim ...
five minute episode script
... DISTINCTIVE BELT OF THREE STARS. IF YOU LOOK A LITTLE CLOSER YOU'LL SEE STARS OF DIFFERENT BRIGHTNESS AND COLOR. DEAN: STAR COLOR IS AN INDICATION OF ITS TEMPERATURE - BLUE STARS BEING THE HOTTEST AND RED STARS BEING THE COLDEST. YOU CAN REALLY SEE THE COLORS OF THE BRIGHTEST STARS LIKE THOSE IN ORI ...
... DISTINCTIVE BELT OF THREE STARS. IF YOU LOOK A LITTLE CLOSER YOU'LL SEE STARS OF DIFFERENT BRIGHTNESS AND COLOR. DEAN: STAR COLOR IS AN INDICATION OF ITS TEMPERATURE - BLUE STARS BEING THE HOTTEST AND RED STARS BEING THE COLDEST. YOU CAN REALLY SEE THE COLORS OF THE BRIGHTEST STARS LIKE THOSE IN ORI ...
Physics 111 HW 23 - University of St. Thomas
... AP03. Under some circumstances, a star can collapse into an extremely dense object made mostly of neutrons and called a neutron star. The density of a neutron star is roughly 10 14 times as great as that of ordinary solid matter. Suppose we represent the star as a uniform, solid, rigid sphere, both ...
... AP03. Under some circumstances, a star can collapse into an extremely dense object made mostly of neutrons and called a neutron star. The density of a neutron star is roughly 10 14 times as great as that of ordinary solid matter. Suppose we represent the star as a uniform, solid, rigid sphere, both ...
Topic/Objective: ______ _____ Full Name: __________ Class: __
... Example - 4.2 light-years means that the light we see has been traveling for 4.2 years before we can see it (4.2 X 9.5 trillion km) Parallax change in an object’s direction due to a change in the observer’s position Parsec short for “parallax second” equal to 3.258 light-years. ...
... Example - 4.2 light-years means that the light we see has been traveling for 4.2 years before we can see it (4.2 X 9.5 trillion km) Parallax change in an object’s direction due to a change in the observer’s position Parsec short for “parallax second” equal to 3.258 light-years. ...
Earth`s Motion and Seasons
... Main Sequence Star: hydrogen fueled star Makes up about 90% of stars Our sun is a main sequence Two types ...
... Main Sequence Star: hydrogen fueled star Makes up about 90% of stars Our sun is a main sequence Two types ...
Lecture 7
... • Why is the center of the Sun hot? • What is the source of the Sun’s energy? • What are neutrinos & why do we care • How does energy get from the inside to the outside of a star? ...
... • Why is the center of the Sun hot? • What is the source of the Sun’s energy? • What are neutrinos & why do we care • How does energy get from the inside to the outside of a star? ...
nebula - Harding University
... At the end of that time, the hydrogen fuel in the center of the Sun will become depleted; there is too much helium to efficiently continue the thermonuclear fusion process at the core. When that happens, the radiation pressure from the center of the Sun will be reduced and the core will collapse ...
... At the end of that time, the hydrogen fuel in the center of the Sun will become depleted; there is too much helium to efficiently continue the thermonuclear fusion process at the core. When that happens, the radiation pressure from the center of the Sun will be reduced and the core will collapse ...
Ay 102: Homework 5 (Blast waves, Supernova Remnant) S. R. Kulkarni
... Please come to the class reading either Ch 38-39 of Draine or 16.1-16.3 of Kowk. I would like that each of be prepared to work out successive elements of this “homework” on the board (with constructive help from me). 1. Supernova Remnant. A popular model for a type Ia supernova is one where a C+O wh ...
... Please come to the class reading either Ch 38-39 of Draine or 16.1-16.3 of Kowk. I would like that each of be prepared to work out successive elements of this “homework” on the board (with constructive help from me). 1. Supernova Remnant. A popular model for a type Ia supernova is one where a C+O wh ...
STAR FORMATION (Ch. 19)
... pillars (emission nebulae), followed by circumstellar disks, and progressing to evolved massive stars in the young starburst cluster.To the upper right of center is the evolved blue supergiant called Sher 25. The star has a unique circumstellar ring of glowing gas that is a galactic twin to the famo ...
... pillars (emission nebulae), followed by circumstellar disks, and progressing to evolved massive stars in the young starburst cluster.To the upper right of center is the evolved blue supergiant called Sher 25. The star has a unique circumstellar ring of glowing gas that is a galactic twin to the famo ...
Star Basics
... helium. At these temperatures most of the hydrogen is ionized, so the hydrogen lines are weak. Both HeI and HeII (singly ionized helium) are seen in the higher temperature examples. The radiation from O5 stars is so intense that it can ionize hydrogen over a volume of space 1000 light years across. ...
... helium. At these temperatures most of the hydrogen is ionized, so the hydrogen lines are weak. Both HeI and HeII (singly ionized helium) are seen in the higher temperature examples. The radiation from O5 stars is so intense that it can ionize hydrogen over a volume of space 1000 light years across. ...
Life Cycle of Stars
... Hubble Space Telescope ACS/HRC – NASA, ESA, N.Evans (Harvard-Smithsonian CfA), and H.Bond (S TScl) ...
... Hubble Space Telescope ACS/HRC – NASA, ESA, N.Evans (Harvard-Smithsonian CfA), and H.Bond (S TScl) ...
Earth in the Solar System (Earth Science) 12% 7 Items Test Prep
... Summary: Distances between astronomical objects are enormous. The astronomical unit (AU) is defined to be equal to the average distance from Earth to the Sun: 1 AU=1.496X1011meters. Distances between planets of the solar system are usually expressed in AU. For distances between stars and galaxies, e ...
... Summary: Distances between astronomical objects are enormous. The astronomical unit (AU) is defined to be equal to the average distance from Earth to the Sun: 1 AU=1.496X1011meters. Distances between planets of the solar system are usually expressed in AU. For distances between stars and galaxies, e ...
study guide
... • Jupiter and Saturn are still “collapsing” and releasing heat • All have moons • Some are large, most are captured asteroids ...
... • Jupiter and Saturn are still “collapsing” and releasing heat • All have moons • Some are large, most are captured asteroids ...
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.