ASTR 151 1st Edition Lecture 15 Outline of Last LectureI. Chapter 7 Section 4 Surface Activity ContinuedII. Chapter 7 Section 5 Earth`s MagnetosphereIII. Chapter 7 Section 6 The TideOutline of Current LectureI. Chapter 8 Section 1 Orbital PropertiesII. Chapter 8 Section 2 Physical PropertiesIII. Chapter 8 Section 3 Surface Features of the Moon and MercuryIV. Chapter 8 Section 4 Rotation RatesCurrent LectureI. Chapter 8 Section 1 Orbital Propertiesa. Distance between Earth and Moon measured using Lasersb. Mercury is never far from suni. Has phasesii. Can be seen in it`s max elongation (18 to 28 degrees) between Earth and the SunII. Chapter 8 Section 2 Physical Propertiesa. Mooni. Radius 1738km, Mass 7.3x10^22kg, Density 3300 kg/m3, escape speed 2.4km/sii. No atmosphere or magnetic field1. Due to air molecules move fast due to thermal motion2. Average molecular speed is well below the escape velocitya. Escapes more probable for lighter moleculesiii. Mercury does have a magnet fieldIII. Chapter 8 Section 3 Surface Features of the Moon and MercuryThese 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.a. Moon has dark featuresi. Lava flow is called Maria (was seen as oceans by early astronomers)ii. Maria result of basaltic eruptionsb. Moon has lots of Cratersi. From meteorite impactsii. Far side (dark) of the Moon has craters but no mariac. Mercury has craters too but their impacts are less dense and shallow than the Moon`si. Looks similar to our Moonii. Named after the patron god of financial gain and commerced. Mercury can`t be seen from Earth due to the sun.IV. Chapter 8 Section 4 Rotation Ratesa. Moon is tidally locked onto the Earthb. Arogee (away) and Perogee describes the Moon`s orbitc. Mercury`s day and year are in a 3:2 resonancei. It`s tilt is the smallest tilt of all the planetsii. Equator`s temperature = 700kiii. Poles are cold =
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