Jupiter - PowerPoint Presentation

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JupiterSlide2
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Jupiter

Largest and most massive planet in the solar system

Contains almost ¾ of all planetary matter in the solar system.

Explored in detail by several space probes:

Pioneer 10, Pioneer 11, Voyager 1, Voyager 2,

Galileo,

Juno

Most striking features visible from Earth: Multi-colored cloud belts

Visual image

Infrared false-color image

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Exploration of Jupiter

Previous Missions

Pioneer 10 & 11

Voyager 1 & 2Slide5

Jupiter Mission

Galileo (1995 - 2003)Slide6

Galileo Probe

What did it tell us?

What did we expect?Slide7

Juno

NASA's Juno mission to Jupiter has been in orbit around the gas giant since July 4, 2016Slide8

Juno

Juno has successfully orbited Jupiter four times since arriving at the giant planet, with the most recent orbit completed on Feb. 2, 2017.

During each orbit, Juno soars low over Jupiter's cloud tops -- as close as about 2,600 miles (4,100 kilometers). During these flybys, Juno probes beneath the obscuring cloud cover and studies Jupiter's auroras to learn more about the planet's origins, structure, atmosphere and magnetosphere.

JunoCamSlide9

Jupiter’s Rotation

Jupiter is the most rapidly rotating planet in the solar system

Rotation period slightly less than 10 hr.

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Centrifugal forces stretch Jupiter into a markedly oblate shape.Slide10

Jupiter’s Atmosphere

Jupiter’s liquid hydrogen ocean has no surface:

Gradual transition from gaseous to liquid phases.

Only very thin atmosphere above cloud layers;

transition to liquid hydrogen zone ~ 1000 km below clouds.Slide11

Jupiter’s Cloud layers

Haze (at the top)

Ammonia

Ammonium Hydrosulfide

Water (lowest observed layer)

What did the Probe find?Slide12

At depth of 1 bar (Earth Sea level):

T = 130 K (-225 F), P=1 bar

Survived to a depth of 150 km:

T = 425 K (305 F), P=22 bars

Hotter and denser than expected

Ammonia and water layers were not detected

Wind velocities much greater (435 mph)

Chemically like Sun in terms of H, He, but a bit off in other elementsSlide13

Jupiter’s Atmosphere

Three layers of clouds:

1. Ammonia (NH

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) crystals

2. Ammonia hydrosulfide (NH

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SH)

3. Water crystals

Heating mostly from latent, internal heatSlide14

Observations of Jupiter from the Earth reveal clouds and atmospheric structures

Belts

ZonesSlide15

The Cloud Belts of Jupiter

Dark belts and bright zones.

Zones higher and cooler than belts; high-pressure regions of rising gas.Slide16

The Cloud Belts on Jupiter

Just like on Earth, high-and low-pressure zones are bounded by high-pressure winds.

Jupiter’s Cloud belt structure has remained unchanged since humans began mapping them.

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Clouds, clouds, clouds

Rotation rate is about 10 hours

Differential Rotation

(different parts rotate at different rates)

Produces turbulence, and storms

© Calvin HamiltonSlide18

Cloud DetailsSlide19

South Pole StormsSlide20

The Great Red Spot

8-year sequence of images of the Great Red Spot on Jupiter

Has been visible for over 400 years

Giant storm system similar to Hurricanes on Earth: Wind speeds of 430 km/h (= 270 miles/h)

Changes appearance gradually over time

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Seems to be decreasing in size – may be gone in 10 to 20 yearsSlide21

The Great Red SpotSlide22

The History of Jupiter

Formed from cold gas in the outer solar nebula, where ices were able to condense.

Rapid growth

Soon able to trap gas directly through gravity

Heavy materials sink to the center

In the interior, hydrogen becomes metallic (very good electrical conductor)

Rapid rotation → strong magnetic field

Rapid rotation and large size

→ belt-zone cloud pattern

Dust from meteorite impacts onto inner moons trapped to form ring

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Jupiter’s Magnetic Field

Magnetic field at least 10 times stronger than Earth’s magnetic field.

Magnetosphere over 100 times larger than Earth’s magnetosphere

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Aurorae on Jupiter

Just like on Earth, Jupiter’s magnetosphere produces aurorae concentrated in rings around the magnetic poles.

~ 1000 times more powerful than aurorae on Earth.

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Particles producing the aurorae originate mostly from moon Io Slide25

Infrared Southern AuroraSlide26

Aurora requires a magnetic field

What’s Jupiter’s magnetic field like?

How is it produced?Slide27

Rock and Metal

Liquid Metallic

Hydrogen

Liquid Hydrogen

Molecular HydrogenSlide28

Jupiter’s Ring SystemSlide29

Jupiter’s Ring

Not only Saturn, but all four gas giants have rings.

Jupiter’s ring: dark and reddish

; only discovered by Voyager 1 spacecraft.

Galileo spacecraft image of Jupiter’s ring, illuminated from behind

Composed of microscopic particles of rocky material

Location: Inside Roche limit, where larger bodies (moons) would be destroyed by tidal forces.

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Satellites of Jupiter

Currently 60+ known satellites - most

Most small asteroid-like, only a few km in size

4 largest satellites are the Galilean Satellites

Io, Europa, Ganymede, CallistoSlide31

Juno’s Family PortraitSlide32

The Galilean SatellitesSlide33

Io - The Volcanic WorldSlide34
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Io: Bursting Energy

Most active of all Galilean moons; no impact craters visible at all.

Over 100 active volcanoes!

Interior is mostly rock.

Activity powered by tidal interactions with Jupiter.

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Surface features have changed since the Voyager spacecraft visited (1979) and the Galileo spacecraft’s observations (late 1990’s)Slide37

Continual volcanic eruptions

Why?Slide38
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Io has the highest density

Io has the fewest craters - youngest surface

Io is closest to Jupiter

And on the other side are the other 3 large satellites

Io is a victim of a tug of war (tidal heating) due to Jupiter and the other moons!Slide40

Jupiter’s Influence on its Moons

Presence of Jupiter has at least two effects on geology of its moons:

1. Tidal effects: possible source of heat for interior of Ganymede

2. Focusing of meteoroids, exposing nearby satellites to more impacts than those further out.

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Interactions with Jupiter’s Magnetosphere

Io’s volcanoes blow out sulfur-rich gases

→ tenuous atmosphere, but gases can not be retained by Io’s gravity

→ gases escape from Io and form an ion torus in Jupiter’s magnetosphere.

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→ Aurorae on Jupiter are fueled by particles from IoSlide42

Europa - The Ice WorldSlide43

Europa: A Hidden Ocean

Close to Jupiter → should be hit by many meteoroid impacts; but few craters visible.

→ Active surface; impact craters rapidly erased.

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The Surface of Europa

Cracked surface and high albedo (reflectivity) provide further evidence for geological activity.

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Ice features that are slowly changing

Very few craters

Lower density than Io

Slightly older surfaceSlide48
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The Interior of Europa

Europa is too small to retain its internal heat

→ Heating mostly from tidal interaction with Jupiter

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Europa has a liquid water ocean ~ 15 km below the icy surface.

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Ganymede - The Largest MoonSlide51

Ganymede: A Hidden Past

Largest of the 4 Galilean moons.

Rocky core

Ice-rich mantle

Crust of ice

1/3 of surface old, dark, cratered;

rest: bright, young, grooved terrain

Bright terrain probably formed through flooding when surface broke

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Light and Dark Terrain indicates some resurfacingSlide54

Lower Density

More craters, Less resurfacing

Older surface than EuropaSlide55
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Callisto - The Cratered MoonSlide57

Callisto: The Ancient Face

Tidally locked to Jupiter, like all of Jupiter’s moons.

Composition: mixture of ice and rocks

Dark surface, heavily pocked with craters.

No metallic core: Callisto never differentiated to form core and mantle.

→

No magnetic field.

Layer of liquid water, ~ 10 km thick, ~ 100 km below surface, probably heated by radioactive decay.

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Valhalla Impact Basin - rings extend out 1500 kmSlide59
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Lowest Density

Most craters

Very little resurfacing

Oldest surfaceSlide61