Mars. Essential Points 1.Mars is about half the size of Earth 2.Mars has a thin carbon dioxide atmosphere 3.Mars has volcanoes and faults but no plate.

Slides:



Advertisements
Similar presentations
The Terrestrial Planets
Advertisements

© 2005 Pearson Prentice Hall This work is protected by United States copyright laws and is provided solely for the use of instructors in teaching their.
Red Planet Mars Chapter Thirteen.
ASTR100 (Spring 2008) Introduction to Astronomy Earth as a Planet Prof. D.C. Richardson Sections
Lecture Outlines Astronomy Today 8th Edition Chaisson/McMillan © 2014 Pearson Education, Inc. Chapter 10.
Mars Astronomy 311 Professor Lee Carkner Lecture 14.
Mars Astronomy 311 Professor Lee Carkner Lecture 14.
Physics 202: Introduction to Astronomy – Lecture 10 Carsten Denker Physics Department Center for Solar–Terrestrial Research.
Mercury = 5.4 g/cm 3 (Earth 5.5 g/cm 3 ) = 0.38 that of Earth Mass Radius Density Gravity = 3.3 x g = M Earth  = 2439 km = 0.38 R Earth Semimajor.
Earth Diameter 12756km Rotation Period 24 hours Orbital Period days Distance from Sun150 x 10 6 km Orbit Eccentricity/Tilt 0.02 / 23.3 degrees Temperature14C.
Astronomy Picture of the Day. Mercury Mass = M Earth Radius = 0.38 R Earth  Surface Temp: K Average distance from Sun =.39 AU Moonlike:
15 February 2005AST 2010: Chapter 9 1 Venus & Mars.
Made by Vlad Stegariu and Stefan Popovici National College, Iasi, Romania.
Looking at the Geology of Planets and Moons in Our Solar System PSC 121 Follow-up to Activity “Exploring the Geology of Several Worlds from Space”
The Inner Planets  The inner planets are the 4 planets closest to the sun:  Mercury  Venus  Earth  Mars  The four inner planets are small and dense.
Mars Basics. Size & Distance Smaller than Earth (0.532x) Mars diam ~ 6779 km (4212 miles) Earth diam ~ 12,742 km (7918 miles) 8 Mars would fit inside.
Red Planet Mars Chapter Thirteen. Guiding Questions 1.When is it possible to see Mars in the night sky? 2.Why was it once thought that there are canals.
The Terrestrial Planets, Part III Mars. MARS The God of War.
The Solar System.
The Inner Planets Mercury Closest planet to the sun Surface has many craters and looks like the moon Cliffs that may have formed from the iron rich.
© 2011 Pearson Education, Inc. Venus and Mars. © 2011 Pearson Education, Inc. Venus.
By Kathleen Romero. Name Size Location Atmosphere Climate Surface Satellites (Moons) Movement Key Explorations Life on Mars? Works Cited.
Astronomy 1. Weekly Quiz  In place of a quiz this week, you must be able to identify each inner planet and give several facts for each.  So pay attention!!!!
By: John Yentzer And Corey Bollinger. Mercury 1. Distance From Sun-57,910,000 km (0.38 AU) 2. 1 Mercury Year equals 58.7 Earth Days 3. Mercury is about.
The Inner Planets. Mercury Small Weak gravitational force No atmosphere Many craters.
Mars. Moons of Mars Exploration of Mars ~1800: Herschel and others discover ice caps and clouds 1877: Phobos and Deimos discovered; also Schiaparelli.
 Small, have rocky surfaces  Terrestrial Planets: meaning earth.
SNC 1D. The Inner Planets  Terrestrial  Rocky iron core  High temperatures  Closer to the Sun  Closer to each other  Smaller than the outer planets.
Handout 27-3 The Inner Planets.
Innri Reikistjörnur Hvað heldur þú? Er hitastig á Merkúr, reikistjörnunni sem er næst sól, hærra en á jörðinni? Hver er samsetning skýja sem umlykja.
A Journey to Our Planetary Neighbors
The Sun Solar Wind Our Solar System’s Star Current Age- 5 Billions years old Life Time Expectancy- 10 Billions years 99.8 % of our solar systems total.
1 Inner or Terrestrial Planets All the inner planets formed at the same time. Their composition is also very similar. They lack the huge atmospheres of.
MARS By: Charanjit, Richard & Cesar.
Bell Work: What is the name of the man who first invented the rocket? What are the names of the first four planets? What is the special name given to these.
Planetary Geology. Should Humans Be in Space? It’s Not Like We Have a Choice.
The Inner Planets 20.3.
In your table of contents…
The Solar System Terrestrial Planets Mercury Venus Earth Mars.
Chapter 9 The Terrestrial Planets. Mercury: The Messenger.
The Inner Planets Chapter Terrestrial Planets Mercury, Venus, Earth, Mars Mostly solid rock with metallic cores Impact craters.
Image Courtesy of NASA/JPL-Caltech.  Known to Babylonians 3,600 years ago as “Star that Wandered”  The Greeks referred to it as “Ares” the god of War.
The Inner Planets. The Inner Planets are:  Small: Compared to the Outer Planets  Rocky: Rocky surface – thin atmosphere  Dense: Heavy for their size.
The Inner Planets Mercury Venus Earth Mars. Four closest planets to the sun All have rocky surfaces Known as terrestrial planets.
MARS. Where is Mars? 4 th planet in our solar system. Last of the rocky planets. Our solar system is in the Orion arm of the Milky Way Galaxy. Our sun.
Mars Monroe. Mons Olympus. Bigger than most states.
Before we begin… A.U. = Astronomical Unit 1 AU = the distance from Earth to the Sun This is how we measure distances from the planets to the Sun.
Chapter 10 Mars. Mars’s orbit is fairly eccentric which affects amount of sunlight reaching it 10.1 Orbital Properties.
Chapter 9 The Terrestrial Planets. Mercury: The Messenger.
MARS By: Luke Balmer and Clark Matthews. MARS Mars is named after (Greek: Ares) is the god of War. The planet probably got this name due to its red color.
INNER PLANETS Terrestrial Planets are the Four planets closest to the sun. These planets have rocky terrain, and have higher temperatures due to receiving.
The Inner planets Section 28.2.
MARS.
Happy Halloween!. Homework #6 Due 6:00 pm today Exam #2 on Wednesday.
Mercury Venus Earth Mars. Mercury -has a surface much like our moon: cratered, but with HUGE volcanoes -no atmosphere -most extreme temperatures in solar.
Mars. When and where can you see it? Can be seen all night long. Sometimes undergoes apparent retrograde motion.
Mars Images How We Know What We Know Current Spacecraft Mars Odyssey (’01-present) Mars Express (’03-present) Mars Exploration Rovers (’04-present) Mars.
Sept 29, 2003Astronomy 100 Fall 2003 Last Homework before Exam (HW#4) is due Friday at 11:50am. Nighttime observing has 8 more nights. Check the webpage.
Unit 11 Mars. Physical Properties Radius: 3400 km Moons: Deimos, Phobos Mass: 6.4 × kg Density: 3900 kg/m 3 Length of Day: 24.6 hours.
Mars Monroe. Retrograde Motion Apparent backwards motion, compared to background stars.
Topic: The Inner Planets PSSA: D/S8.D.3.1. Objective: TLW explain how distance is measured in our solar system. TLW compare the characteristics.
Our Solar System How it Formed & the Inner Planets Chapter 19 & 20.
Created By: Jared CraCraft – Gabby Smith
Mars.
The Inner Planets.
The Inner Solar System.
Chapter 8.2 “The Inner Planets”
The Solar System.
The Inner Planets of Our Solar System
Walter S. Kiefer Lunar and Planetary Institute
Presentation transcript:

Mars

Essential Points 1.Mars is about half the size of Earth 2.Mars has a thin carbon dioxide atmosphere 3.Mars has volcanoes and faults but no plate tectonics 4.Mars had liquid water early in its history 5.Evidence for life on Mars is debatable

Mars About half the size of Earth Rotates in 24.5 hours Ranges from 207 to 249 million km (129 to 155 million miles) from Sun Period: 687 days Two tiny satellites

Mars and Earth

The Surface of Mars Thin carbon dioxide atmosphere about 1/150 as dense as Earth’s Surface temperatures -20 to -200 C Polar caps of ice and frozen carbon dioxide Large rift valley (Vallis Marineris) Huge Shield Volcanoes (Olympus Mons) Evidence for former liquid water

Mars as Lowell Knew It

Lowell’s Mars

Lowell’s Venus

Modern Imaging Technology Improves Earth-Based Views of Mars Greatly

Mars from Mariner 9

Mars Viking Mosaic

Mars Topography

Vallis Marineris

Huge Landslide in Vallis Marineris

Layered Deposits in Vallis Marineris

Active Landslide on Mars

Olympus Mons

Summit of Olympus Mons

Phobos over Olympus Mons

Mars’ Polar Caps

Polar Cliffs on Mars

Dunes on Mars

Water on Mars

Channels on Mars

Floods on Mars

Where’s the Water Now?

Recent Water on Mars?

How to Lose an Ocean If water is exposed to solar UV and particles, it breaks down to H + O (photo- dissociation) Happens if water gets into upper atmosphere – Planet gets hot (Venus) – Planet loses atmosphere (Mars) Oxygen combines with iron and other elements, on Mars may also have escaped

Landing on Mars

Mars as Seen by Viking

Mars from Pathfinder

Martian Winter

Martian Sunset

Layered Rocks on Mars

Cape St. Vincent

Opportunity’s Shadow

Spirit Makes Tracks

Digging Out

Hole on Mars

Wind Erosion on Mars

Ice in Martian Crater

Martian Glacier?

Martian Dust Devil

Dust Devil Tracks

Phobos and Deimos

Phobos and its Shadow

Martian Solar Eclipses

Earth From Mars

Jupiter From Mars

The Face on Mars

Martian Meteorite

Martian Fossils ?

Essential Points 1.Mars is about half the size of Earth 2.Mars has a thin carbon dioxide atmosphere 3.Mars has volcanoes and faults but no plate tectonics 4.Mars had liquid water early in its history 5.Evidence for life on Mars is debatable

Feedback: Privacy Policy Feedback
Do Not Sell My Personal Information
About project: SlidePlayer Terms of Service

© 2024 SlidePlayer.com. Inc. All rights reserved.