Mars Characteristics Quiz

General Characteristics

• Mars appears red due to iron oxide (rust) on its surface, reflecting sunlight.
• Mars has about half the diameter of Earth and approximately one-tenth the mass.
• Mars is about 15% of Earth's volume and 11% of Earth's surface area.
• A Martian day (sol) is roughly 24 hours and 37 minutes.
• A Martian year lasts for 687 Earth days.
• Mars is colder than Earth due to its greater distance from the sun and thin atmosphere.
• Both Mars and Earth have polar ice caps, seasons, and similar day lengths.
• Mars has a thinner atmosphere, colder temperatures, no liquid water on the surface, and a smaller size compared to Earth.
• Polar ice caps on Mars are comprised of water ice and carbon dioxide (dry ice).
• Early astronomers observed features on Mars resembling canals, polar ice caps, and seasonal changes, associating them with Earth's features.
• "Earth and Mars at opposition" occurs when Mars is on the opposite side of Earth from the Sun, making it appear brightest and closest in the night sky.
• Seasonal changes are caused by Mars' axial tilt (25.2 degrees, similar to Earth's) and its elliptical orbit around the Sun.
• Seasonal changes on Mars include growth and shrinking of polar ice caps and sometimes planet-wide dust storms.

Martian Atmosphere

• The primary atmospheric gas on Mars is carbon dioxide (CO2), making up about 95% of the atmosphere.
• Martian atmospheric pressure is less than 1% of Earth's, making it extremely thin.

Exploration of Mars

• Scientists explore Mars to study potential past or present life, geology, and climate.
• Exploration also aims to prepare for possible human colonization.

Geologic History of Mars

• Scientists determine the relative ages of different areas on Mars by counting the number and size of impact craters.
• The three main geological periods on Mars are: Noachian (4.1-3.7 billion years ago): Heavy cratering and potential liquid water; Hesperian (3.7-3 billion years ago): Volcanic activity and declining water; Amazonian (3 billion years ago-present): Dry, cold conditions with minimal surface changes.

Moons of Mars

• Mars has two moons, Phobos and Deimos.
• Both moons are much smaller than Earth’s Moon.
• They are irregularly shaped objects.

Hemispheric Dichotomy

• Mars displays a striking difference between the northern lowlands (smooth, flat, and younger terrain) and southern highlands (heavily cratered, elevated, and older terrain), this is called the hemispheric dichotomy.

Martian Basin

• The Borealis Basin, likely a giant impact basin, may have been formed early in Mars' history.

Noachian Period

• Characteristics of the Noachian period include heavy cratering; evidence of flowing water, such as valley networks; formation of the planet's oldest surfaces.

River Valleys

• Potential liquid water might have flowed across the surface, creating river valleys.

Loss of Mars' Magnetic Field

• Without a magnetic field, Mars' atmosphere was stripped away by solar wind.

Tharsis Plateau

• A huge volcanic region on Mars that houses some of the largest volcanoes in the solar system.

Hesperian Period

• Mars transitioned from a wet environment to a cold, dry planet during this period, and volcanic activity decreased.

Maps and Surface Features

• Elevation maps colour Mars based on height, and lower elevations are typically represented by blue-coloured maps, while orange or red elevations represent higher ones.
• Olympus Mons is a volcano shown on the Mars map and is located in a volcanic region.
• Heavily cratered areas are Noachian terrain.
• Large impact basin on the map labelled Hellas Basin is an example of one.
• The Northern Lowlands are smooth and blue coloured on the Mars map.
• The boundary between northern lowlands and southern highlands is marked by a white wavy line.
• Shield volcanoes with broad, dome structures formed by lava flows.
• Surface features such as valley networks hint at past liquid water on Mars.

Significance of Atmospheric Pressure

• Low atmospheric pressure prevents liquid water from existing on the surface—water either freezes or evaporates.

Loss of Liquid Water

• Loss of magnetic fields and atmosphere are primary reasons for Mars' loss of liquid water.
• Cooling of the planet from warm temperatures to freezing led to liquid water loss.

Amazonian Period

• During the Amazonian period, wind erosion and dust storms were primary forces of change.

Current Martian Conditions

• Mars' current conditions include cold, dry, thin atmosphere and occasional dust storms.

Current Ice Caps

• Polar ice caps, subsurface ice discovered by radar, and frost in shaded areas are the primary indicators of ice on Mars currently.

Starbucks on Mars

• Currently there are no Starbucks on Mars.