PPT-Is it a meteorite? In-Class Activity 1_Meteorite & Impact Craters

. Francis Nimmo. Last Week - Volcanism. How and why are melts generated?. Increase in mantle potential temperature; or. Reduction in solidus temperature (e.g. water); or. Thinning of the lithosphere. How do melts ascend towards the surface?. Characterizing LROC NAC Images. Created by: . Belfry High School. Participants. Taylor Runyon. Mickayla Walters. Sarah Compton. Staci Coleman. Brianna Sullivan. Our Purpose. Our purpose of doing this project is to understand morphology and the composition of the Tycho . Houle. 11:00 E. 10:00 C. Red. RB. Bank. High. School. Lunar-tics!. Scientific Research. Southeastern Imbrium Crater Age Dating and Ejecting Data. March 30, 2011. . Objectives Covered. What we covered for Phase II. & Meteors. Lectures will be available at: . homework.uoregon.edu. /pub/. elsa. /. haydock. / . Asteroid Belt Basic . Characteristics. Estimated 1 million are ~1km or larger; millions more are . smaller. In-Class Activity 1_Meteorite & Impact Craters. Introduction to methods. Identification and classification. EL YAZIDI . Mayssa. . Le 31/03/2016 – . Kélibia. . Plan . Introduction. Terminology. Origin. Identification . criteria. Classification. Meteors. Meteorites. Impacts. Meteors, Meteorites and Impacts. I. . Small . Solar System Bodies. Small Solar System Bodies. (SSSB, as defined by the IAU) are objects in the Solar System that are neither . Tungsten isotope abundances for iron meteorites fall into two distinct groups that also include carbonaceous chondrites (CC) and non-carbonaceous chondrites (NC) plus Mars, Earth, and the Moon. The higher . Asteroids. Over 100,000 asteroids.. Vesta is the largest – 330 miles. in diameter.. Size range – 330 miles to about. 100 yards.. Irregular-shaped rocky bodies.. Some asteroids have moon(s).. The . Isheyevo. carbonaceous chondrite . has millimeter- . to centimeter-thick laminations . composed of different amounts of silicate versus Fe-Ni metal grains. . These remarkable laminations are a permanent record of a . on. The early history of the Solar System is recorded by meteorites falling now, but also by those that fell hundreds of millions to billions of years ago, preserved in lunar samples, sedimentary layers on Earth, and even sitting on the surface of Mars. . Prentice Hall Earth Science. 22.3 Objectives. Describe . how the physical features of the lunar surface were created. Explain . the history of the moon . 22.3 Vocabulary. crater. ray. mare. rille. lunar regolith. on. The early history of the Solar System is recorded by meteorites falling now, but also by those that fell hundreds of millions to billions of years ago, preserved in lunar samples, sedimentary layers on Earth, and even sitting on the surface of Mars. . Formation of the Moon Before visit to the Observatory Overview Introduction to the Formation of the Moon Video about the Evolution of the Moon Classroom demonstrations on distances to the Moon Classroom activity – Craters on the Moon