PHY 102 1st EditionOutline of Last LectureI. Einsteina. Equation for spacetimeII. Shape of the UniverseIII. Einstein, GTR, and the Universea. Einstein’s equation of general relativityIV. Friedmann’s Universea. Total Energyb. Einstein’s Equationsc. E = mc2V. Atomic Emission SpectraVI. Hubble’s Relationshipa. Distance of nebulasb. Hubble’s law for GalaxiesVII. Abbe Georges LamaitreOutline of Current Lecturei. Individual Star Organizationii. Aging of Starsiii. Variable Starsiv. ClustersThese notes represent a detailed interpretation of the professor’s lecture. GradeBuddy is best used as a supplement to your own notes, not as a substitute.v. Nebulaevi. SNR, Neutron Stars, Black HolesCurrent LectureI. Individual Stars are organized:a. By massb. By lifetimei. Stars range in efficiency in use of gas – can have the same amount of gas but use it in a different time periodc. AgeII. When stars age:a. They can literally explodeb. Some will become white dwarves, neutron stars, and othersc. Which one they will become is dependent on the massIII. Binary/Singular Starsa. Both are equally as commonb. Two stars that orbit around each other instead of one being the “center” of a galaxyc. Some people believe that our sun has a companion star that passes every 30 million years (linked to extinction patterns)IV. Variable Starsa. Large magellanic cloudb. From the southern hemisphere, the milky way looks like two ‘chunks’As the period of variability gets longer, the brightness increasesluminosityThe difference between absolute brightness and apparent brightness has to do with distancePeriod of variabilityV. Clusters – two types:a. Open: loose clusters of stars (leftover from formation of clouds & dust)b. Globular: closely grouped stars – gravitational pull is extremely strongi. 13.8 billion years oldcluster starsbrightturnoff blue redii. Younger stars will be on the main sequenciii. Older the stars are, the more likely they are to peel off of the curvec. We know how much fuel they have and how fast they use it so we can trace it back to age the starsVI. Nebulaea. Emission – sword of Orion contain the Great Nebulab. Dark – horsehead nebula – more perfect vacuum than we can createc. Reflection – seven sisters – dusty gas that surrounds each nebulad. Planetar – the star casts off a shell of material i. Swell so large that the outer layer is cast off and the white dwarf dense core in leftVII. SNRs, Neuton Stars, and Black Holdsa. SNR with Neutron starsi. When they explode, they do it from the inside outii. Gravity in the core will increase until the Helium nucleus crashes togetherto create carbon, oxygen which collapses into Nitrogen. Once Iron is converted into the next element, the next step takes energy and uses the energy from the star. The core collapses on itself, the protons are crushed into electrons and become neutrons.b. Black Hole Modeli. No known force within the nucleus that can stop the collapseii. Closer you get to a black hole, escape velocity is SO greatc. Nuclear Fusioni. The sun is essentially a controlled nuclear blastii. 90% of the original material was Hydrogen by massiii. Proton-neutron will crash into another pair and create Helium and releaseantimatteriv. Light form the sun results from nuclear collisions in the sun’s corev. Can take a million years to start its