Astronomy 328 Midterm Exam - Department of Physics and Astronomy
... Exam rules: You may consult your sheet of formulas during the exam. This sheet can contain any formulas or values for constants that you think you need but it cannot contain worked out problems or concepts. You must turn in your formula sheet with the exam. Calculators are permitted. Good luck. ...
... Exam rules: You may consult your sheet of formulas during the exam. This sheet can contain any formulas or values for constants that you think you need but it cannot contain worked out problems or concepts. You must turn in your formula sheet with the exam. Calculators are permitted. Good luck. ...
The Role of the Galaxy in the Dynamical Evolution of
... 1) Mass of protoplanetary disk may have been low ( as current migration theory suggest it was - Gomes et al 2004). If so, is Standard Model too inefficient, especially since stripping by Giant Molecular Clouds was not included? Then again, mass of typical comet is unknown, so estimates of mass vary ...
... 1) Mass of protoplanetary disk may have been low ( as current migration theory suggest it was - Gomes et al 2004). If so, is Standard Model too inefficient, especially since stripping by Giant Molecular Clouds was not included? Then again, mass of typical comet is unknown, so estimates of mass vary ...
Astronomy 112: The Physics of Stars Class 17 Notes: Core Collapse
... begins to occur spontaneously. Each such reaction requires 1.3 MeV of energy, and even further reduces the degeneracy pressure of the electrons. Electron capture by heavy elements earlier on in the collapse occurs for very similar reasons. The collapse is only halted once another source of pressure ...
... begins to occur spontaneously. Each such reaction requires 1.3 MeV of energy, and even further reduces the degeneracy pressure of the electrons. Electron capture by heavy elements earlier on in the collapse occurs for very similar reasons. The collapse is only halted once another source of pressure ...
What is remote sensing?
... along successive lines over finite time called scanning systems. The size of scene which is determined by the aperture and optics called field of view (FOV). ...
... along successive lines over finite time called scanning systems. The size of scene which is determined by the aperture and optics called field of view (FOV). ...
Star Finder
... aspect of the stars daily and yearly permits us to use the locator for any day or hour of the year. D: CIRCUMPOLAR CONSTELLATIONS: Rotate the dial and note the constellations near the pole(brass pin) just go in circles about the pole and some never disappear (or set behind a horizon ie. Never set!). ...
... aspect of the stars daily and yearly permits us to use the locator for any day or hour of the year. D: CIRCUMPOLAR CONSTELLATIONS: Rotate the dial and note the constellations near the pole(brass pin) just go in circles about the pole and some never disappear (or set behind a horizon ie. Never set!). ...
A deep look at the nuclear region of UGC 5101 through high angular
... this scenario, these mergers first go through a luminous starburst phase, followed by a dust-enshrouded active galactic nucleus (AGN) phase, and finally evolve into an optically bright, naked quasar once they either consume or shed their shells of gas and dust (Sanders et al. 1988a). The target of i ...
... this scenario, these mergers first go through a luminous starburst phase, followed by a dust-enshrouded active galactic nucleus (AGN) phase, and finally evolve into an optically bright, naked quasar once they either consume or shed their shells of gas and dust (Sanders et al. 1988a). The target of i ...
Chapter 3 - People @ EECS at UC Berkeley
... the phase change upon reflection varies in sign depending on the sequence of high and low refractive index materials. (d) What is the required bi-layer periodicity (d-spacing) required for positive interference? Note that this problem will be considered computationally, including absorption, in Chap ...
... the phase change upon reflection varies in sign depending on the sequence of high and low refractive index materials. (d) What is the required bi-layer periodicity (d-spacing) required for positive interference? Note that this problem will be considered computationally, including absorption, in Chap ...
1 Dark matter and dark energy comprise over 90% of the Universe
... Universe is flat, with Ω0 = 1. The search for dark matter using gravitational lensing provides the backdrop to explanations to what dark matter is and why it is important. Among the myriad of particle candidates for dark matter, two stand out: the WIMP and the axion. Gravitational lensing as a tool ...
... Universe is flat, with Ω0 = 1. The search for dark matter using gravitational lensing provides the backdrop to explanations to what dark matter is and why it is important. Among the myriad of particle candidates for dark matter, two stand out: the WIMP and the axion. Gravitational lensing as a tool ...
Ch. 21
... the use of instructors in teaching their courses and assessing student learning. Dissemination or sale of any part of this work (including on the World Wide Web) will destroy the integrity of the work and is not permitted. The work and materials from it should never be made available to students exc ...
... the use of instructors in teaching their courses and assessing student learning. Dissemination or sale of any part of this work (including on the World Wide Web) will destroy the integrity of the work and is not permitted. The work and materials from it should never be made available to students exc ...
Exploring Compton Scattering Using the Spectrum
... electron volt is equal to 1.602×10−19 J. The energy E of a photon is related to its wavelength λ or its frequency f through Planck’s formula E hf ...
... electron volt is equal to 1.602×10−19 J. The energy E of a photon is related to its wavelength λ or its frequency f through Planck’s formula E hf ...
Gravitational Lensing Abstract
... was the first to derive the correct formula for the deflection angle α̃ of a light passing at a distance r from an object with mass M as α̃ = ...
... was the first to derive the correct formula for the deflection angle α̃ of a light passing at a distance r from an object with mass M as α̃ = ...
Zeeman observations: Measuring magnetic fields in the atomic and
... In Astrophysics, the only way to directly measure magnetic fields is through polarimetric observations. In the case of interstellar medium (ISM) studies, the polarization can be detected from the following mechanisms (see [27] for a description of these mechanisms): synchrotron radiation, thermal du ...
... In Astrophysics, the only way to directly measure magnetic fields is through polarimetric observations. In the case of interstellar medium (ISM) studies, the polarization can be detected from the following mechanisms (see [27] for a description of these mechanisms): synchrotron radiation, thermal du ...
18. Formation of Stars.
... formation & evolution. ◦ Gravity is constantly trying to pull matter toward the center of mass of a gas cloud or a star. ◦ Since stars do not have an infinite supply of energy, they must readjust their structure in response to the energy supply. Initially, gravitational collapse is the only source ...
... formation & evolution. ◦ Gravity is constantly trying to pull matter toward the center of mass of a gas cloud or a star. ◦ Since stars do not have an infinite supply of energy, they must readjust their structure in response to the energy supply. Initially, gravitational collapse is the only source ...
here - Canadian Institute for Theoretical Astrophysics
... Kepler identifies planets by detecting the slight dimming in a star’s light that occurs when an object passes in front of it. This ‘transit’ method can find planets much smaller than the radialvelocity technique can, giving astronomers a chance to detect other Earths. Kepler has now found 974 exopla ...
... Kepler identifies planets by detecting the slight dimming in a star’s light that occurs when an object passes in front of it. This ‘transit’ method can find planets much smaller than the radialvelocity technique can, giving astronomers a chance to detect other Earths. Kepler has now found 974 exopla ...
planetary standard model
... Kepler identifies planets by detecting the slight dimming in a star’s light that occurs when an object passes in front of it. This ‘transit’ method can find planets much smaller than the radialvelocity technique can, giving astronomers a chance to detect other Earths. Kepler has now found 974 exopla ...
... Kepler identifies planets by detecting the slight dimming in a star’s light that occurs when an object passes in front of it. This ‘transit’ method can find planets much smaller than the radialvelocity technique can, giving astronomers a chance to detect other Earths. Kepler has now found 974 exopla ...
Globular and Open Clusters in our Galaxy
... The overall number of currently known globular clusters in our Galaxy is about 150. They can be find about anywhere in the celestial sphere, but with a significant concentration towards the Milky Way center, which explains why the constellations of Sagittarius, Ophiuchus and Scorpius solely congrega ...
... The overall number of currently known globular clusters in our Galaxy is about 150. They can be find about anywhere in the celestial sphere, but with a significant concentration towards the Milky Way center, which explains why the constellations of Sagittarius, Ophiuchus and Scorpius solely congrega ...
Optical studies of an ultraluminous X-ray source: NGC1313 X-2 Jifeng Liu
... X-ray observations: spectroscopy • light curves ...
... X-ray observations: spectroscopy • light curves ...
printer-friendly sample test questions
... 2nd Item Specification: Recognize the life-cycles of mid-size and massive stars and their stellar remnants. Depth of Knowledge Level 1 8. When fusion of hydrogen ceases in our Sun’s core, the Sun will A. explode as a supernova. B. collapse into white dwarf star. C. contract into a black hole. D. exp ...
... 2nd Item Specification: Recognize the life-cycles of mid-size and massive stars and their stellar remnants. Depth of Knowledge Level 1 8. When fusion of hydrogen ceases in our Sun’s core, the Sun will A. explode as a supernova. B. collapse into white dwarf star. C. contract into a black hole. D. exp ...
The X-ray Bursters Problem and its Implications to the Equation of
... baryon of proton mass mp ) release energies around grav = R p ∼ 200 MeV per nucleon. This energy is liberated in form of kinetic energy, gamma-ray photons (emerging in the Xray burst), and neutrinos. The time that takes for heat transport to cool the deep envelope (thermal time) is around seconds, ...
... baryon of proton mass mp ) release energies around grav = R p ∼ 200 MeV per nucleon. This energy is liberated in form of kinetic energy, gamma-ray photons (emerging in the Xray burst), and neutrinos. The time that takes for heat transport to cool the deep envelope (thermal time) is around seconds, ...
Stellar Distances - Red Hook Central School District
... Ex 1: The nearest star to Earth is Alpha Centauri, which is at a distance of 4.37 ly. Calculate the parallax angle that was measured to obtain that distance. ...
... Ex 1: The nearest star to Earth is Alpha Centauri, which is at a distance of 4.37 ly. Calculate the parallax angle that was measured to obtain that distance. ...
The Primeval Populations of the Ultra
... [Fe/H]= −2.3; blue curve) and the low extreme of the metallicity distribution in these UFDs ([Fe/H]= −3.2; green curve). It is clear from the comparison that the luminosity of the MS turnoff and SGB in each galaxy is consistent with ancient metal-poor stars. The few stars immediately brighter and bl ...
... [Fe/H]= −2.3; blue curve) and the low extreme of the metallicity distribution in these UFDs ([Fe/H]= −3.2; green curve). It is clear from the comparison that the luminosity of the MS turnoff and SGB in each galaxy is consistent with ancient metal-poor stars. The few stars immediately brighter and bl ...
Ch. 22 (NS & BH
... the use of instructors in teaching their courses and assessing student learning. Dissemination or sale of any part of this work (including on the World Wide Web) will destroy the integrity of the work and is not permitted. The work and materials from it should never be made available to students exc ...
... the use of instructors in teaching their courses and assessing student learning. Dissemination or sale of any part of this work (including on the World Wide Web) will destroy the integrity of the work and is not permitted. The work and materials from it should never be made available to students exc ...
Astronomical spectroscopy
Astronomical spectroscopy is the study of astronomy using the techniques of spectroscopy to measure the spectrum of electromagnetic radiation, including visible light, which radiates from stars and other hot celestial objects. Spectroscopy can be used to derive many properties of distant stars and galaxies, such as their chemical composition, temperature, density, mass, distance, luminosity, and relative motion using Doppler shift measurements.