PH109 Exploring the Universe, Test#4, Spring 2005 Please indicate
... 14. Why is the energy source of active galaxies thought to be extremely compact? a) Their energy is totally no stellar in origin. b) Their spectra are like those produced by ordinary stars. c) They vary on rapid time scales. d) They can be seen clearly; we can see that the energy source is compact. ...
... 14. Why is the energy source of active galaxies thought to be extremely compact? a) Their energy is totally no stellar in origin. b) Their spectra are like those produced by ordinary stars. c) They vary on rapid time scales. d) They can be seen clearly; we can see that the energy source is compact. ...
Chapter 25.2 - Planet Earth
... Degenerate matter uses electrical repulsion instead of molecular motion to support itself from total collapse. Although atomic particles in degenerate matter are much closer together than in normal Earth matter, they still are not packed as tightly as possible. Stars made of matter that has an even ...
... Degenerate matter uses electrical repulsion instead of molecular motion to support itself from total collapse. Although atomic particles in degenerate matter are much closer together than in normal Earth matter, they still are not packed as tightly as possible. Stars made of matter that has an even ...
New light on our Sun`s fate - Space Telescope Science Institute
... what happens in the middle remains one of the biggest mysteries in stellar astrophysics. It is during these years that stars undergo dramatic changes and can rapidly transform over size scales of tens of thousands. This evolution begins when a star, depleted of hydrogen in its core, begins to burn h ...
... what happens in the middle remains one of the biggest mysteries in stellar astrophysics. It is during these years that stars undergo dramatic changes and can rapidly transform over size scales of tens of thousands. This evolution begins when a star, depleted of hydrogen in its core, begins to burn h ...
17_LectureOutline
... Apparent luminosity is measured using a magnitude scale, which is related to our perception. It is a logarithmic scale; a change of 5 in magnitude corresponds to a change of a factor of 100 in apparent ...
... Apparent luminosity is measured using a magnitude scale, which is related to our perception. It is a logarithmic scale; a change of 5 in magnitude corresponds to a change of a factor of 100 in apparent ...
Slide 1
... Apparent luminosity is measured using a magnitude scale, which is related to our perception. It is a logarithmic scale; a change of 5 in magnitude corresponds to a change of a factor of 100 in apparent ...
... Apparent luminosity is measured using a magnitude scale, which is related to our perception. It is a logarithmic scale; a change of 5 in magnitude corresponds to a change of a factor of 100 in apparent ...
Transcript_Forbidden Planets
... still manage to deliver lethal doses of high energy radiation onto the planet – and probably generate enough solar wind to blow away the atmosphere – and they would only last of few million years before going supernova, which would be insufficient time for the indigenous Tatooine life-forms to have ...
... still manage to deliver lethal doses of high energy radiation onto the planet – and probably generate enough solar wind to blow away the atmosphere – and they would only last of few million years before going supernova, which would be insufficient time for the indigenous Tatooine life-forms to have ...
Astrophysics by Daniel Yang
... wavelengths. The frequencies absorbed are identical to the frequencies it would emit when incandescent. - Describe the technology needed to measure astronomical spectra To measure spectra, light from the source must be collected then dispersed to form a spectrum. Afterwards, the spectrum can be reco ...
... wavelengths. The frequencies absorbed are identical to the frequencies it would emit when incandescent. - Describe the technology needed to measure astronomical spectra To measure spectra, light from the source must be collected then dispersed to form a spectrum. Afterwards, the spectrum can be reco ...
Unit 11: Stellar Evolution
... the neutrinos being radiated away from the core. In a fraction of a second, the earthsized iron core is transformed into a neutron core about 10 miles across. The unsupported outer regions are now free-falling toward the neutron core. The implosion is converted into an explosion by a combination of ...
... the neutrinos being radiated away from the core. In a fraction of a second, the earthsized iron core is transformed into a neutron core about 10 miles across. The unsupported outer regions are now free-falling toward the neutron core. The implosion is converted into an explosion by a combination of ...
Ch. 20
... all the same age but have different masses. • Stars in binary systems can evolve quite differently due to interactions with each other. ...
... all the same age but have different masses. • Stars in binary systems can evolve quite differently due to interactions with each other. ...
Asymptotic Giant Branch
... • Most AGB stars (see later) and obviously also a large fraction of the RGB stars are variable • Variations in brightness, colour, velocity and extension observed • Possibility to „look“ into the stellar interior ...
... • Most AGB stars (see later) and obviously also a large fraction of the RGB stars are variable • Variations in brightness, colour, velocity and extension observed • Possibility to „look“ into the stellar interior ...
![Chapter Zero Section 0.2 [reprint from Jesperson 7th] Supernovas](http://s1.studyres.com/store/data/009810478_1-e5fd9db32afbb84e749a32319c4308af-300x300.png)
Chapter Zero Section 0.2 [reprint from Jesperson 7th] Supernovas
... causes a cataclysmic collapse of the star, and as the nuclei rush toward the core the increase in pressure and density do two things. 1. The speeding nuclei destroy many of the iron nuclei, creating a rich mixture of smaller particles such as helium nuclei and neutrons. 2. The temperature of the col ...
... causes a cataclysmic collapse of the star, and as the nuclei rush toward the core the increase in pressure and density do two things. 1. The speeding nuclei destroy many of the iron nuclei, creating a rich mixture of smaller particles such as helium nuclei and neutrons. 2. The temperature of the col ...
21_LectureOutline
... The last nucleus in the alpha-particle chain is nickel-56, which is unstable and quickly decays to cobalt-56 and then to iron-56. Iron-56 is the most stable nucleus, so it neither fuses nor decays. However, within the cores of the most massive stars, neutron capture can create heavier elements, all ...
... The last nucleus in the alpha-particle chain is nickel-56, which is unstable and quickly decays to cobalt-56 and then to iron-56. Iron-56 is the most stable nucleus, so it neither fuses nor decays. However, within the cores of the most massive stars, neutron capture can create heavier elements, all ...
Document
... Globular cluster – tight groups of hundreds of thousands of very old stars Open cluster - contain less than a few hundred members, and are often very young - may eventually become disrupted over time and no longer gravitational bound – move in broadly same direction in space – referred to as ste ...
... Globular cluster – tight groups of hundreds of thousands of very old stars Open cluster - contain less than a few hundred members, and are often very young - may eventually become disrupted over time and no longer gravitational bound – move in broadly same direction in space – referred to as ste ...
Lecture Notes - NMSU Astronomy
... • Photosphere is dense enough to radiate light but not too dense so that photons can escape; thus it is where spectrum of star is emitted and where the absorption lines arise. • Chromosphere is active, hotter and lower density than photosphere is where emission occurs (hot, low density gas). This ...
... • Photosphere is dense enough to radiate light but not too dense so that photons can escape; thus it is where spectrum of star is emitted and where the absorption lines arise. • Chromosphere is active, hotter and lower density than photosphere is where emission occurs (hot, low density gas). This ...
Astronomy 114 Problem Set # 6 Due: 11 Apr 2007 SOLUTIONS 1
... Recall that the temperature of a gas reflects the average speed of the particles. Only the fastest particles at any given temperature will be able overcome the repulsion. Increasing the temperature will then increase the speed of the fastest particles and in turn increase the rate of fusion reaction ...
... Recall that the temperature of a gas reflects the average speed of the particles. Only the fastest particles at any given temperature will be able overcome the repulsion. Increasing the temperature will then increase the speed of the fastest particles and in turn increase the rate of fusion reaction ...
Spiral Elliptical Irregular - SMS 8th Grade Astronomy Unit
... We are __________________ million miles away from the sun This is called an Astronomical Unit (AU) (it would take a jet 17 years to travel this far!) Pluto is 39 AU from the sun…How many miles is that? _____________________ Anything farther than objects in our solar system has to be measured in ligh ...
... We are __________________ million miles away from the sun This is called an Astronomical Unit (AU) (it would take a jet 17 years to travel this far!) Pluto is 39 AU from the sun…How many miles is that? _____________________ Anything farther than objects in our solar system has to be measured in ligh ...
Contemporary Physics - Department of Physics and Astronomy
... apparent magnitude of a star as we see it? Is Proxima Centauri smaller in diameter than the Sun, or larger? ...
... apparent magnitude of a star as we see it? Is Proxima Centauri smaller in diameter than the Sun, or larger? ...
Astronomers Find Extremely Large Planet
... these disks extend many times farther than this local comparison suggests that planets, too, could extend well beyond the relatively close proximity observed in our solar system and others. “That would be good news for astronomers, because planets are notoriously difficult to detect near stars, whic ...
... these disks extend many times farther than this local comparison suggests that planets, too, could extend well beyond the relatively close proximity observed in our solar system and others. “That would be good news for astronomers, because planets are notoriously difficult to detect near stars, whic ...
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.