Astronomy 1010 Planetary Astronomy Fall_2015 Day-29.

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Presentation transcript:

Astronomy 1010 Planetary Astronomy Fall_2015 Day-29

Course Announcements SW-chapter 8 posted: due Wed. Nov. 4 Exam-3 Wed. Nov. 4: Ch. 6, 7, 8 I will collect the L-T books on Monday, Nov. 23 Dark Night Observing (last 2 of semester): Thursday Nov. 5 Monday Nov. 9 1 st Quarter Obs. (last one of semester): Thurs. Nov. 19 Reports Due: Monday Nov. 23 – AT CLASS TIME!

Useful Information for Next Lab Habitable Zones NAAP Lab Print the instructions BEFORE you come to class!

Take more astronomy! Registration for the Spring semester starts soon so think about taking more astronomy. ASTR-1010/1011: Planetary Astro & lab (Tell your friends) ASTR-1020/1021: Stellar Astronomy & lab (Reg. + Honors) ASTR-2020: Problems in Stellar Astronomy ASTR-3010: History of Astronomy ASTR-3040: Intro. To AstroBiology PHYS-2468: Intro. To Physics Research ASTR-3030/3031: Instrumentation & Techniques

 Volcanism is related to tectonism and is a sign of geologic activity.  The movement of the tectonic plates generates a lot of thermal energy from friction.  This energy combines with heat from convection cells in the mantle to heat portions of the lower crust and upper mantle as magma.

 Volcanoes form (mostly) at hot spots and plate boundaries.  Very fluid lava forms shield volcanoes.  Thick lava forms composite volcanoes.

 The Moon does not have any volcanoes, but lava flows smoothed out parts of its surface.  Mercury also has smooth surfaces from past volcanism, and a few inactive volcanoes have been identified.

 The volcanoes on Mars are the largest mountains in the Solar System, and are shield volcanoes (largest = Olympus Mons).  Venus has the largest amount of volcanoes in the Solar System.

 Erosion includes processes that wear down the high spots and fill in the low.  On Earth, wind and water strongly erode features.  Wind also modifies the surfaces of Venus and Mars, especially on Mars with its loose dust.

Water  While Earth is the only planet with liquid water, there is much evidence that Mars was once wetter than it is today.  Canyons, dry riverbeds, layered rock.

Water  Large deposits of subsurface ice have been detected beneath Mars’ surface, deep under craters as well as just beneath the soil.  Water ice could exist on Mercury and was observed on the Moon after NASA crashed a vehicle into a crater.

Water  Impacts have far-reaching consequences.  The mass extinction of the dinosaurs marked in the Cretaceous-Tertiary boundary could be evidence of a very large impact.

Recent Collisions

Earth’s Surface

Torino Scale

Impact Energies and these are the small ones

Earth’s Changing Surface Lecture Tutorial pg. 101 Work with a partner! Read the instructions and questions carefully. Discuss the concepts and your answers with one another. Take time to understand it now!!!! Come to a consensus answer you both agree on and write complete thoughts into your LT. If you get stuck or are not sure of your answer, ask another group.

i_Clicker Question Terrestrial Planets: Mercury’s Scarps Venus Rotation Moon Altimeter

Exam – 3 To Here