Astronomy 101: The Solar SystemThe Final Exam Details• Final exam date: December 15, 10:30 AM• Location: Hasbrouck 20• The final exam has two parts:• Part 1 is the 3rd midterm. This will focus on thematerial presented in lecture after the second midterm,i.e., this will cover material presented in lecturesbetween Nov. 13 and Dec. 11.• Part 2 is a cumulative final.• The final exam does not have a take-home part. 100%of the grade on the final exam is based on the in-classexam score.Outline of course subject matterOverview and Scale of the UniverseMath reviewPowers of 10Scientific notationUnits of measurementLight yearSize and scale of the UniverseAge of the UniverseOrigin of elements in the cores of starsThe work of Einstein and Edwin HubbleExpansion of the UniverseGravitational lensingMotion of the Earth & SunThe speed of light and the "observable" universeLooking back in time by observing distant objectsObserving the Sky and the Celestial SphereThe Solar System, star clusters, galaxiesThe Scientific MethodConstellationsThe Celestial SphereDiurnal (daily) motion & impact on observing the skyAnnual motion & impact on observing the skyAngles & angular measurementsPrevalence in astronomyUnits of angle measurementAngular diameter vs. linear diameterThe Milky WayHistorical evolution of our understanding of the Milky Way (an exampleof the scientific method at work)Current understandingMapping the skyAltitude & azimuthLatitude & longitudeAltitude of Polaris (the "North Star"): a navigation tool!Right Ascension and DeclinationCelestial motions & cycles of our livesThe definition of days, weeks, months, & years have astronomical originsPhases of the Moon & motion of the MoonSolar & lunar eclipsesCause of eclipsesTypes of eclipsesReasons that eclipses are rarely viewedThe seasons on EarthCause of the seasonsSolstices & equinoxesReason Venus & Mercury are "evening (or morning) stars"Retrograde motion of the planetsPrecession (e.g., precession of the Earth's axis of rotation)Astronomy Through the AgesAchievements and motivations of ancient cultures in astronomyStonehenge, Mayan astronomy, Anasazi astronomyAgricultural & religious purposesGreek astronomical concepts & achievementsLogical arguments of the Greek philosophersFeatures of the Ptolemaic model of the Solar SystemFlaws of the Greek modelParallaxCopernicus, Brahe, Kepler, & GalileoKepler's LawsGalileo's observations and arguments against the Greek modelEnergy & MatterBasic types of energyConservation of energyKinetic energyPotential energy (e.g., gravitational, chemical)Thermal energyHeat vs. temperatureTemperature scalesPhases and properties of matterSolid, liquid, gas, and "plasma"Electric chargeProperties of atomsThe size of the atom and the nature of mattter at the microscopic levelElectrons, protons, & neutronsAtomic number & atomic mass number (also known as atomic weight)IsotopesIonsMoleculesEnergy levelsMatter-energy: E = mc2Two types of nuclear reactions: fission & fusionElectric chargeFour fundamental forces of natureLaws of MotionSpeed, velocity, & accelerationScalar vs. vector quantities and addition of vectorsAcceleration due to gravityMomentum & ForceConservation of (linear) momentumMass vs. weightNewton's laws of motionNewton's universal law of gravitationAngular quantities, e.g., angular momentum & torqueConservation of angular momentumUseful applications of angular momentum (e.g., gyroscopes, pointing the HubbleSpace Telescope)Orbital motionBalance of orbital velocity vs. gravityEscape velocityTypes of orbits (ellipse, parabola, hyperbola)Orbital energyChanging orbits by gravitational encounters or atmospheric dragKepler's laws as explained by NewtonTidesThe cause of effects of tidal forcesTides on EarthTidal frictionSynchronous rotationExamples of tidal effects throughout the Solar System (e.g., Io, Europa,Enceladus, the Earth-Moon system)Physics of LightLight carries energy & informationBasic characteristicsWavelength, frequency, energy, speed, amplitudeTransverse vs. longitudinal wavesResonanceDual natureParticle-like characteristicsWave-like characteristicsThe connection between light and electric and magnetic fields(the nature of an "electromagnetic" wave)The electromagnetic spectrumTypes of lightWhite lightSpectroscopyEmission vs. absorption vs. continuum spectraSpectra of atoms and moleculesThermal radiation (aka blackbody radiation)Basic explanation and characteristicsStephan-Boltzmann lawWien lawSound waves vs. light wavesInteraction of light and matterEmission, absorption, transmission, reflectionReflection: specular vs. diffuseRefraction and diffractionAddition of waves and "beats"The Doppler effectHubble's use of the Doppler effectOther applications (e.g., detecting rotation and measuring rotation speed)Flux and luminosityPower from the Sun delivered to various planetsHubble's use of Cepheid starsTelescopesThe human eye vs. telescopesRefracting telescopes vs. reflecting telescopesFundamental properties and purposes of telescopesFocusing of lightLight-collecting areaAngular resolutionMagnification: not important for professional telescopes. Why?A simple explanation of how refraction occursObservations of the Solar SystemLayout & observed motionsTerrestrial vs. jovian planetsAsteroids & cometsCharacteristicsDistribution in the Solar System (asteroid belt, Kuiper Belt, Oort Cloud)Odd cases & exceptionsNotable features of all planetsThe "habitable zone"Craters on Mercury and the MoonEvidence of the period of "heavy bombardment"Formation of the Solar SystemKey observational constraintsEvidence of interstellar clouds from which stars can form (e.g., giant clouds ofmolecules in the Orion constellation)Basic governing physicsGravity, conservation of energy, angular momentum, & linear momentumProcesses that occur when a cloud collapses under the force of gravityEvidence supporting the nebular theory of planetary system formationDisks observed around young stars in our galaxyRecent observations of disks and planets orbiting Fomalhaut and BetaPictorisBuilding the Solar SystemCondensation, accretion, & planetesimal collisionsKey role of temperature in how matter condensesThe "frost line"Explanation of terrestrial vs. jovian planetsReason that jovian planets acquire large amounts of gas andterrestrial planets do notJovian moons and evidence that jovian planets are "miniature" solarsystemsImportance and impact of the solar windTransfer of the Sun's angular momentumMagnetic fields generated by the