Practice Questions for Exam 3
... A. As the Sun was forming, nuclear fusion reactions in the shrinking clouds of gas slowly became stronger and stronger, until the Sun reached its current luminosity. B. The Sun initially began making energy through chemical reactions. These heated the interior enough to allow gravitational contracti ...
... A. As the Sun was forming, nuclear fusion reactions in the shrinking clouds of gas slowly became stronger and stronger, until the Sun reached its current luminosity. B. The Sun initially began making energy through chemical reactions. These heated the interior enough to allow gravitational contracti ...
Earth Science Curriculum Unit 1 Maps and Measurements
... 1. Describe evidence that supports the Big Bang theory. 2. Identify the three main types of galaxies. 3. List several characteristics of the Milky Way Galaxy. Section 3 Radiation from space Time: 2 sessions 1. Explain the electromagnetic spectrum. Section 4 Stars and the Evolution of Stars Time: 3 s ...
... 1. Describe evidence that supports the Big Bang theory. 2. Identify the three main types of galaxies. 3. List several characteristics of the Milky Way Galaxy. Section 3 Radiation from space Time: 2 sessions 1. Explain the electromagnetic spectrum. Section 4 Stars and the Evolution of Stars Time: 3 s ...
EM review
... A Hertzsprung-Russell (HR) diagram is a plot of absolute magnitude (luminosity) against temperature. The majority of stars lie in a band across the middle of the plot, known as the Main Sequence. This is where stars spend most of their lifetime, during their hydrogen-burning phase. ...
... A Hertzsprung-Russell (HR) diagram is a plot of absolute magnitude (luminosity) against temperature. The majority of stars lie in a band across the middle of the plot, known as the Main Sequence. This is where stars spend most of their lifetime, during their hydrogen-burning phase. ...
Question 1 (7-5 thru 7-7 PPT Questions)
... form than the lifespan of the accretion disk around the star. 2. According to the disk-instability model, dense regions forming in the disk accrete more material and suddenly collapse to form one or more planets. However, such instabilities require massive disks, which are not commonly observed. ...
... form than the lifespan of the accretion disk around the star. 2. According to the disk-instability model, dense regions forming in the disk accrete more material and suddenly collapse to form one or more planets. However, such instabilities require massive disks, which are not commonly observed. ...
Tools of Astronomy
... 5. And that’s just what’s in or local neighborhood! Our Galaxy is a collection of about ___ billion stars, and there are at least 300 billion other ________! Our nearest neighboring galaxy is the Andromeda galaxy. It is an incredible ________ light years away! Here is a view looking back with Earth ...
... 5. And that’s just what’s in or local neighborhood! Our Galaxy is a collection of about ___ billion stars, and there are at least 300 billion other ________! Our nearest neighboring galaxy is the Andromeda galaxy. It is an incredible ________ light years away! Here is a view looking back with Earth ...
Supernovae — Oct 21 10/21/2011 • Outline
... stars and expelled by supernovae • Heavier elements were made in supernovae & in giants, where there are free neutrons. Nuclei capture neutrons. ...
... stars and expelled by supernovae • Heavier elements were made in supernovae & in giants, where there are free neutrons. Nuclei capture neutrons. ...
Powerpoint
... • Considered to be a “revised” Big Bang theory • The universe expanded and cooled until about 10-35 second after the big bang when it became so cool that the forces of nature caused the universe to inflate tremendously. • The initial expansion was faster than the speed of light. ...
... • Considered to be a “revised” Big Bang theory • The universe expanded and cooled until about 10-35 second after the big bang when it became so cool that the forces of nature caused the universe to inflate tremendously. • The initial expansion was faster than the speed of light. ...
ASTRONOMY WEBQUEST…… EXPLORE THE UNIVERSE
... Stars and planets are made from gases in a __________________. The Milky Way Galaxy is approximately _______________ light years across. How much longer will our Sun last? _________________________ Lifetimes of stars range from ___________ to ____________ years. Our star orbits the centre of our gal ...
... Stars and planets are made from gases in a __________________. The Milky Way Galaxy is approximately _______________ light years across. How much longer will our Sun last? _________________________ Lifetimes of stars range from ___________ to ____________ years. Our star orbits the centre of our gal ...
The Central Star of A63 – UU Sge Don Pollacco, Ralf
... UU Sge is unique amongst central star in that it is a totally eclipsing binary. Hence physical parameters for the components can be derived, in principle, with great accuracy. The morphology of A63 is extreme, exhibiting an aspect ratio of some 7:1! ...
... UU Sge is unique amongst central star in that it is a totally eclipsing binary. Hence physical parameters for the components can be derived, in principle, with great accuracy. The morphology of A63 is extreme, exhibiting an aspect ratio of some 7:1! ...
STAAR Science Tutorial 35 TEK 8.8B: The Sun
... TEK 8.8B: Recognize that the Sun is a medium-sized star near the edge of a disc-shaped galaxy of stars and that the Sun is many thousands of times closer to Earth than any other star. Our Sun is a star, much like all of the other stars that are visible in the night sky. What makes our Sun different ...
... TEK 8.8B: Recognize that the Sun is a medium-sized star near the edge of a disc-shaped galaxy of stars and that the Sun is many thousands of times closer to Earth than any other star. Our Sun is a star, much like all of the other stars that are visible in the night sky. What makes our Sun different ...
IFU observations of the high-z Universe
... SSA22b results • Assuming shock velocities of several 100 km/s • Shell travels ~100 kpc in a few 108yr • Shell can cool to ~104 K in this time – Implied by the Voigt profile b parameter – Required to be in photoionization equilibrium ...
... SSA22b results • Assuming shock velocities of several 100 km/s • Shell travels ~100 kpc in a few 108yr • Shell can cool to ~104 K in this time – Implied by the Voigt profile b parameter – Required to be in photoionization equilibrium ...
Nature of Stars 2
... Kepler 3rd Law gives us a relationship between the average distance of a planet from the Sun and the amount of time it takes a planet to orbit the Sun once. For objects orbiting the Sun, P2 = a3 (P in years, a in AUs). Kepler’s relation does not work for objects that are not orbiting the Sun, for ex ...
... Kepler 3rd Law gives us a relationship between the average distance of a planet from the Sun and the amount of time it takes a planet to orbit the Sun once. For objects orbiting the Sun, P2 = a3 (P in years, a in AUs). Kepler’s relation does not work for objects that are not orbiting the Sun, for ex ...
Build your own Galaxy - McDonald Observatory
... oven cooks food by emitting strong radio waves, called microwaves, at a 12-centimeter wavelength). Astronomers have detected hydrogen far beyond the luminous stars of our galaxy. In your model, the hydrogen clouds would extend an additional nine centimeters from the edge of the disk. In real space, ...
... oven cooks food by emitting strong radio waves, called microwaves, at a 12-centimeter wavelength). Astronomers have detected hydrogen far beyond the luminous stars of our galaxy. In your model, the hydrogen clouds would extend an additional nine centimeters from the edge of the disk. In real space, ...
Lesson 3 - The DK Foundation
... cannot be a purely intellectual exercise. Knowing the name of our stars is the first step, but it is only a first step. The preparation is part of the process: making time, physically travelling to places where we are able to see the stars clearly, and then locating our ‘own’ stars in order to esta ...
... cannot be a purely intellectual exercise. Knowing the name of our stars is the first step, but it is only a first step. The preparation is part of the process: making time, physically travelling to places where we are able to see the stars clearly, and then locating our ‘own’ stars in order to esta ...
chap18_s05_probs
... = 1.7 10 kilogram per meter3 4/3 R 3 = 1.7 10-24 kilogram per meter3 13.51 (6.4 106 meters)3 = 1.7 10-24 kilogram per meter3 1.1 1021 meters3 = 0.0019 kilograms or 1.9 grams (!) A very small mass. PROBLEM 18-10: To ionize interstellar hydrogen, a photon must have a wavelen ...
... = 1.7 10 kilogram per meter3 4/3 R 3 = 1.7 10-24 kilogram per meter3 13.51 (6.4 106 meters)3 = 1.7 10-24 kilogram per meter3 1.1 1021 meters3 = 0.0019 kilograms or 1.9 grams (!) A very small mass. PROBLEM 18-10: To ionize interstellar hydrogen, a photon must have a wavelen ...
HABITABLE PLANETS For every star with planets, how many of
... split on whether these are a problem. (I’ll explain in class. Your text also has a good discussion of low-mass stars.) These are clearly important points since low mass stars comprise about 70 to 80 percent of all stars: If low-mass stars can have habitable planets with life, then they are the most ...
... split on whether these are a problem. (I’ll explain in class. Your text also has a good discussion of low-mass stars.) These are clearly important points since low mass stars comprise about 70 to 80 percent of all stars: If low-mass stars can have habitable planets with life, then they are the most ...
Neutron Stars and Black Holes
... Probe nearing the event horizon of a black hole will be seen by observers as experiencing a dramatic redshift as it gets closer Time appears to be going more and more slowly as it approaches the event horizon This called a gravitational redshift Not due to motion, but to the large gravitational ...
... Probe nearing the event horizon of a black hole will be seen by observers as experiencing a dramatic redshift as it gets closer Time appears to be going more and more slowly as it approaches the event horizon This called a gravitational redshift Not due to motion, but to the large gravitational ...
A new isolated dSph galaxy near the Local Group
... The gas-poor dwarf spheroidal systems (dSph) with old stellar population are found almost exclusively in the virial domain of groups and clusters. It is generally considered that the concentration of dSph galaxies to the haloes of massive galaxies is due to processes of gas stripping and strangulati ...
... The gas-poor dwarf spheroidal systems (dSph) with old stellar population are found almost exclusively in the virial domain of groups and clusters. It is generally considered that the concentration of dSph galaxies to the haloes of massive galaxies is due to processes of gas stripping and strangulati ...
Topics for this week
... The Sun radiates tremendous amount of energy from its surface. Where does this energy come from? Nuclear fusion inside the Sun generates energy while fusing hydrogen nuclei to make helium nuclei. The reaction chain is referred to as the proton-proton chain because the first reaction is the fusion of ...
... The Sun radiates tremendous amount of energy from its surface. Where does this energy come from? Nuclear fusion inside the Sun generates energy while fusing hydrogen nuclei to make helium nuclei. The reaction chain is referred to as the proton-proton chain because the first reaction is the fusion of ...
The portion of light we detect from a star/blackbody depends on
... Since the discrepancy was greatest at UV wavelengths, this problem was called the: “ultraviolet catastrophe.” ...
... Since the discrepancy was greatest at UV wavelengths, this problem was called the: “ultraviolet catastrophe.” ...
ppt - MIT Haystack Observatory
... Sun is orders of magnitude) large solar flares (as measured in X-rays) have a nearly 100% association with CMEs (Yashiro et al. 2006) If one supposes that this scaling relation also applies to different kinds of stars, it implies a substantially enhanced mass loss rate CME mass loss on Sun is genera ...
... Sun is orders of magnitude) large solar flares (as measured in X-rays) have a nearly 100% association with CMEs (Yashiro et al. 2006) If one supposes that this scaling relation also applies to different kinds of stars, it implies a substantially enhanced mass loss rate CME mass loss on Sun is genera ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.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.