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3 Pages

### Exercise2c

Course: PHY 3, Fall 2009
School: University of Dayton
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Word Count: 429

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2c Exercise Estimate of Angular Diameters Page 1 Names of members of lab group (alphabetical please) Group Number: Determine the angular width of the fingers or between the knuckles for each member of your group using techniques described in class. Group Member Name: What is being used for the angular measure? Angular width appropriate for this person: Group Member Name: What is being used for the angular...

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2c Exercise Estimate of Angular Diameters Page 1 Names of members of lab group (alphabetical please) Group Number: Determine the angular width of the fingers or between the knuckles for each member of your group using techniques described in class. Group Member Name: What is being used for the angular measure? Angular width appropriate for this person: Group Member Name: What is being used for the angular measure? Angular width appropriate for this person: Group Member Name: What is being used for the angular measure? Angular width appropriate for this person: Group Member Name: What is being used for the angular measure? Angular width appropriate for this person: Group Member Name: What is being used for the angular measure? Angular width appropriate for this person: Exercise 2c Estimate of Angular Diameters Page 2 Group Number: 1. Estimate the angular diameter of 3 objects on campus. You can use the "knuckle" or "finger" rule that you learned in class. Fill in the following information for each object. Brief Description of Object and it's location (ex: Door at main entrance to science center) Your location when you made the measurement Angular Diameter: Brief Description of Object and it's location (ex: Door at main entrance to science center) Your location when you made the measurement Angular Description Diameter: Brief of Object and it's location (ex: Door at main entrance to science center) Your location when you made the measurement Angular Diameter: Exercise 2c Estimate of Angular Diameters Page 3 Check of your abilities. Group Number: 2. Stand at double doors in the FRONT of the Science Center, looking down the hall past SC128 (our class room) and look at the double doors at the BACK of the Science Center. Estimate the angular diameter of the double doors at the back of the Science Center. Next, measure the distance from the double doors to where you are standing, and measure the actual width of the double doors. Using the trigonometry you learned in class, determine the actual angular diameter of the double doors from your position. Here is some information you might fin...

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University of Dayton - PHY - 2
Exercise 2b Estimate of Angular Diameters Page 1Names of members of lab group (alphabetical please)Group Number:Determine the angular width of the fingers or between the knuckles for each member of your group using techniques described in class.
University of Dayton - PHY - 250
Exercise 2b Estimate of Angular Diameters Page 1Names of members of lab group (alphabetical please)Group Number:Determine the angular width of the fingers or between the knuckles for each member of your group using techniques described in class.
University of Dayton - PHY - 250
Exercise 4a Estimate of Distance Using Parallax Page 1Names of members of lab group (alphabetical please)Group Number:The following exercise is a VERY crude estimate of a distance using parallax. Calculate the distance indicated in the picture b
University of Dayton - PHY - 250
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University of Dayton - PHY - 6
View from outside of the boxPhoton injected into the boxClick left mouse button to continueView from outside of the boxPhoton injected into the boxView from outside of the boxPhoton injected into the boxView from outside of the boxPho
University of Dayton - PHY - 250
Black Holes in Other GalaxiesBlack Holes in Other GalaxiesThe giant elliptical galaxy M87 is located 50 million light-years away in the constellation Virgo. By measuring the rotational properties of the central core of the galaxy and in the obser
University of Dayton - PHY - 6
Black Holes in Other GalaxiesBlack Holes in Other GalaxiesThe giant elliptical galaxy M87 is located 50 million light-years away in the constellation Virgo. By measuring the rotational properties of the central core of the galaxy and in the obser
University of Dayton - PHY - 250
The Solar System MissionsComparative Planetology* The study of the similarities and dissimilarities of the constituents of the solar system. * Provides a basis for understanding how the solar system might have formed and how it evolved.planets n
University of Dayton - PHY - 6
The Solar System MissionsComparative Planetology* The study of the similarities and dissimilarities of the constituents of the solar system. * Provides a basis for understanding how the solar system might have formed and how it evolved.planets n
University of Dayton - PHY - 250
Telescopes !We have learned how the EM waves are produced by objects of interest.NOWWe have to learn how the information is collectedNaked Eye AstronomyConstellations Motions of Planets Moon Observations Eclipses Comets Meteor Showers Identifi
University of Dayton - PHY - 3
Telescopes !We have learned how the EM waves are produced by objects of interest.NOWWe have to learn how the information is collectedNaked Eye AstronomyConstellations Motions of Planets Moon Observations Eclipses Comets Meteor Showers Identifi
University of Dayton - PHY - 250
Supernova Type 1 SupernovaProduced in a binary system containing a white dwarf. The mechanism is the same (?) as what produces the nova event.NovaNova Rapid increase in luminosity of a white dwarf in a binary systemRotationAccretion disc ma
University of Dayton - PHY - 6
Supernova Type 1 SupernovaProduced in a binary system containing a white dwarf. The mechanism is the same (?) as what produces the nova event.NovaNova Rapid increase in luminosity of a white dwarf in a binary systemRotationAccretion disc ma
University of Dayton - PHY - 250
Supernova 1987aSupernova 1987aOn February 23, 1987, a Canadian astronomer named Ian Shelton took a photo of the Large Magellanic Cloud. Upon development of the film, he discovered a bright star which had not been seen before. It became clear that
University of Dayton - PHY - 6
Supernova 1987aSupernova 1987aOn February 23, 1987, a Canadian astronomer named Ian Shelton took a photo of the Large Magellanic Cloud. Upon development of the film, he discovered a bright star which had not been seen before. It became clear that
University of Dayton - PHY - 250
University of Dayton Flyer Observatory UFOFunded: Fall 2006 Through the University of Dayton LTC Innovation Grant ProgramUFOMeade LX200R 12 inch telescope w/ UHTC Ritchey-Chretien Cassegrain f = 3048 mm D = 305.8 mmUFOSony GPS Receiver Sensor
University of Dayton - PHY - 3
University of Dayton Flyer Observatory UFOFunded: Fall 2006 Through the University of Dayton LTC Innovation Grant ProgramUFOMeade LX200R 12 inch telescope w/ UHTC Ritchey-Chretien Cassegrain f = 3048 mm D = 305.8 mmUFOSony GPS Receiver Sensor
University of Dayton - PHY - 250
Wave BasicsWavesBasicTerminology.pptEquilibriumAmplitude
University of Dayton - PHY - 3
Wave BasicsWavesBasicTerminology.pptEquilibriumAmplitude
University of Dayton - PHY - 250
Nucleosynthesis WoodstockWell I came across a child of God, he was walking along the road and I asked him tell where are you going, this he told me: Well, I'm going down to Yasgur's farm, going to join in a rock and roll band. Got to get back to the
University of Dayton - PHY - 6
Nucleosynthesis WoodstockWell I came across a child of God, he was walking along the road and I asked him tell where are you going, this he told me: Well, I'm going down to Yasgur's farm, going to join in a rock and roll band. Got to get back to the
University of Dayton - PHY - 250
Neutron Stars PulsarsNeutron StarsIn 1967, it was believed (by some) that the first intelligent signal from outer space had been discovered. A graduate student by the name of Jocelyn Bell observed highly periodic, well defined pulsations of electr
University of Dayton - PHY - 6
Neutron Stars PulsarsNeutron StarsIn 1967, it was believed (by some) that the first intelligent signal from outer space had been discovered. A graduate student by the name of Jocelyn Bell observed highly periodic, well defined pulsations of electr
University of Dayton - PHY - 250
Black Holes - ObservationHow do you see something you can't see ?How do objects emit em waves?When an charged object accelerates, it must change it's energy if the acceleration causes a change in speed.If the acceleration of the charged object
University of Dayton - PHY - 6
Black Holes - ObservationHow do you see something you can't see ?How do objects emit em waves?When an charged object accelerates, it must change it's energy if the acceleration causes a change in speed.If the acceleration of the charged object
University of Dayton - PHY - 250
EMWavesElectric Charge and Field BasicsFundamental charges are carried by electrons (negative) and protons (positive). Charge on the electron is 1.6 x 10-19 C Charge on the proton is + 1.6 x 10-19 C Like sign charges repel, opposite sign charges
University of Dayton - PHY - 3
EMWavesElectric Charge and Field BasicsFundamental charges are carried by electrons (negative) and protons (positive). Charge on the electron is 1.6 x 10-19 C Charge on the proton is + 1.6 x 10-19 C Like sign charges repel, opposite sign charges
University of Dayton - PHY - 20
The Helium Flash and Stages 10 and 11 M &lt; 8 MhThe Helium Flash and Stage 10 M &lt; 8 MhElectron degeneracy pressure: the pressure exerted by electrons caused by the confinement in the small core of a star that has left the main sequence.The Helium
University of Dayton - PHY - 250
The Helium Flash and Stages 10 and 11 M &lt; 8 MhThe Helium Flash and Stage 10 M &lt; 8 MhElectron degeneracy pressure: the pressure exerted by electrons caused by the confinement in the small core of a star that has left the main sequence.The Helium
University of Dayton - PHY - 5
The Helium Flash and Stages 10 and 11 M &lt; 8 MhThe Helium Flash and Stage 10 M &lt; 8 MhElectron degeneracy pressure: the pressure exerted by electrons caused by the confinement in the small core of a star that has left the main sequence.The Helium
University of Dayton - PHY - 250
Cygnus X1 The FirstCygnus X1In the early Seventies scientists found an intensive X-Ray source in the Cygnus Constellation. They believe that this X-Ray source is a black hole. Cygnus X-1 is an X-ray binary in the constellation Cygnus, the swan, t
University of Dayton - PHY - 6
Cygnus X1 The FirstCygnus X1In the early Seventies scientists found an intensive X-Ray source in the Cygnus Constellation. They believe that this X-Ray source is a black hole. Cygnus X-1 is an X-ray binary in the constellation Cygnus, the swan, t
University of Dayton - PHY - 250
Space WarpsSpace WarpsLight is believed to travel the shortest distance between two pointsBut. the path of light is curved in the presence of a gravitational fieldEinstein realized that the characteristics of gravity could be explained without
University of Dayton - PHY - 6
Space WarpsSpace WarpsLight is believed to travel the shortest distance between two pointsBut. the path of light is curved in the presence of a gravitational fieldEinstein realized that the characteristics of gravity could be explained without
University of Dayton - PHY - 250
The Solar SystemThe Solar SystemNebula is very hot, and generally is made of gas that is rotating.The Solar SystemHot, rotating nebula RotationSolar NebulaSmall amount of rotation about the axisLarge amount of rotation near the equator
University of Dayton - PHY - 6
The Solar SystemThe Solar SystemNebula is very hot, and generally is made of gas that is rotating.The Solar SystemHot, rotating nebula RotationSolar NebulaSmall amount of rotation about the axisLarge amount of rotation near the equator
University of Dayton - PHY - 250
NovaNovaNova Rapid increase in luminosity of a white dwarf in a binary systemRotationThe Roche lobe is the region of space around a star in a binary system within which orbiting material is gravitationally bound to that star.NovaNova Rapi
University of Dayton - PHY - 6
NovaNovaNova Rapid increase in luminosity of a white dwarf in a binary systemRotationThe Roche lobe is the region of space around a star in a binary system within which orbiting material is gravitationally bound to that star.NovaNova Rapi
University of Dayton - PHY - 250
Line SpectraWhen the particles in the solid, liquid, or gas accelerate, they will produce EM waves.Electron orbit to orbit transitions in atoms (gasses)Applicable to the study of stars (gaseous objects)Line SpectraAtomic StructureShell mode
University of Dayton - PHY - 4
Line SpectraWhen the particles in the solid, liquid, or gas accelerate, they will produce EM waves.Electron orbit to orbit transitions in atoms (gasses)Applicable to the study of stars (gaseous objects)Line SpectraAtomic StructureShell mode
University of Dayton - PHY - 20
Quantum Mechanics - Confinement The Heisenberg Uncertainty PrincipleThe Heisenberg Uncertainty Principle: The position and momentum of a particle cannot be precisely specified simultaneously.&quot;Classical physics seemed the limiting case of visualiza
University of Dayton - PHY - 5
Quantum Mechanics - Confinement The Heisenberg Uncertainty PrincipleThe Heisenberg Uncertainty Principle: The position and momentum of a particle cannot be precisely specified simultaneously.&quot;Classical physics seemed the limiting case of visualiza
University of Dayton - PHY - 250
Line SpectraWhen the particles in the solid, liquid, or gas accelerate, they will produce EM waves.Electron orbit to orbit transitions in atoms (gasses)Applicable to the study of stars (gaseous objects)Line SpectraEmission SpectrumIn accord
University of Dayton - PHY - 250
Measurements of LuminosityFor a refresher on Stefan's Law, upon which this tutorial is based, please consult the Tutorial on Continuous SpectraLuminosity (brightness) of a StarLuminosity is the amount of energy per second (Watts) emitted by the
University of Dayton - PHY - 250
Doppler Shift Astrophysics and CosmologyLonger , lower f Shorter , higher fThe Wavelengths get &quot;squished&quot; in the direction of motion, and &quot;stretched&quot; in the opposite direction.Doppler Shift Astrophysics and CosmologyLonger , lower f Shorter
University of Dayton - PHY - 250
Sun Nuclear ReactionsSunNuclear PhysicsThe work of Einstein A new view of mass:2E=mc Conceptual Implication: Mass is a highly concentrated form of energy.Therefore mass can be converted to other formsSunNuclear PhysicsHow much mass wou
University of Dayton - PHY - 250
Issues with the use of telescopes MagnificationMagnification determines how much larger the image is as compared to the size of the source of the light (the object)oMagnification = fWhere fo is the focal length of the objective fe is the focal
University of Dayton - PHY - 250
Line BroadeningLine broadening - Effect of Doppler Shifts.Spread in Wavelength True Wavelength H= H==2 x Average Velocity of Particles in the Gas Wave SpeedH=H=WavelengthLine BroadeningThe figure shows the spectrum of the sun. It is d
University of Dayton - PHY - 250
Two Body Systems Based on Keplers First LawTwo Body Systems Based on Keplers First LawXFocusClose window to end programTwo Body Systems Based on Keplers First LawXFocusClose window to end programTwo Body Systems Based on Keplers
University of Dayton - PHY - 250
Hertzsprung Russell DiagramA plot of the luminosity as a function of the surface temperature for different radii stars.Hertzsprung Russell DiagramShow all the steps, including the non-dimensionalization process, to demonstrate that a plot of th
University of Dayton - PHY - 250
Spectral Types Continuous SpectraStellar SpectraSince for a photonE=hfThe energy carried by the photon determines the position of the electromagnetic wave on in the electromagnetic spectrum. If the resulting frequency is within the visible win
University of Dayton - PHY - 250
Measurements of Star PropertiesFor a refresher on Trigonometry, please consult the Tutorial on Measurement BasicsCommon Name SunScientific NameDistance (light years) -Apparent Magnitude -26.72Absolute Magnitude 4.8Spectral Type G2VPro
University of Dayton - PHY - 250
Keplers Laws 1. The orbits of the planets are ellipses, with the sun at one focus of the ellipse. 2. The line joining the planet to the sun sweeps out equal areas in equal times as the plates travels around the ellipse. 3. The ratio of the squares of
University of Dayton - PHY - 250
Trigonometry Tutorial* Right Triangles * Tangents * Small Angle Approximation * Triangulation * Parallax Trianglesr OppositeTrianglesWr Trianglesrd Adjacent TriangleswrdTan = Opposite/Adjacent = w/d
University of Dayton - PHY - 250
Comparative Planetology Determining Planet CharacteristicsMost of what is in this tutorial is a review of information contained in past tutorialsPlease refer to the previous tutorials to reinforce the information contained in this tutorialThe A
University of Dayton - SCI - 190
John E. ErdeiINTEGRATED NATURAL SCIENCE SEQUENCE (INSS) SCI190 Fall 2008 Science Center 101B 92318 John.Erdei@notes.udayton.edu Mon Thrs 9:00 am 10:30 am 1:00 pm 2:30 pm Office of the Dean: O'Reilly Hall 104A 92604Physics:Office Hours:Web P
University of Dayton - SCI - 190
John E. ErdeiINTEGRATED NATURAL SCIENCE SEQUENCE (INSS) SCI190 Fall 2007 Science Center 101B 92318 John.Erdei@notes.udayton.edu Mon Thrs 9:00 am 10:30 am 1:00 pm 2:30 pm Office of the Dean: O'Reilly Hall 104A 92604Physics:Office Hours:Web P
University of Dayton - SCI - 190
Part 2, B: MOTION Newton's Laws Fnet2Net force is the vector sum of the individual forces7N2N5NPart 2, B: MOTION Newton's Laws2Part 2, B: MOTION Newton's Laws2Part 2, B: MOTION Newton's Laws2Example: An object sits at rest on
University of Dayton - SCI - 190
123456Destructive Interference Active Noise Reduction (ANR)Koss Noise Reduction Headphones7Destructive Interference Active Noise Reduction (ANR)Koss Noise Reduction HeadphonesThis revolutionary Active Noise Reduction (ANR) ste
University of Dayton - SCI - 190
University of Dayton - SCI - 190
1234Part 2, B: MOTION Newton's Laws Fnet2Net force is the vector sum of the individual forces7N2N5N5Part 2, B: MOTION Newton's Laws26Part 2, B: MOTION Newton's Laws27Part 2, B: MOTION Newton's Laws2Example: An ob