Jupiter: An Overview- Remote Sensing Application - Completely Remote Sensing, GPS, and GPS Tutorial
Jupiter: An Overview

Our tour begins with Jupiter, shown here in full disk images taken by Voyager 1 (top), enhanced to bring out various color tones and (bottom) taken from the Galileo spacecraft that reached the planet 18 years later which affords a closer approximation to the true color of this planet's atmospheric exterior. This, and other imagery, are shown in the Wikepedia website overview of Jupiter.

Color Voyager 1 full-disk image of Jupiter.



Color Galileo full-disk image of Jupiter.

In one sense, Jupiter is the most important of the solar planets in that its size and mass have played a major role in the development and survival of the inner (terrestrial) planets. It does two vital things: its gravitational action on these planets have slowed their inward progression towards the Sun and it helps to keep most large asteroids from continually bombarding the inner planets.

The jovian atmosphere is approximately 75% hydrogen and 24% helium by mass, with the remaining 1% of the mass consisting of other elements. The interior contains denser materials such that the distribution is roughly 71% hydrogen, 24% helium and 5% other elements by mass. The atmosphere contains trace amounts of methane, water vapor, ammonia, and silicon-based compounds. There are also traces of carbon, ethane, hydrogen sulfide, neon, oxygen, phosphine, and sulfur. The outermost layer of the atmosphere contains crystals of frozen ammonia. Through infrared and ultraviolet measurements, trace amounts of benzene and other hydrocarbons have also been found.

The most obvious features of Jupiter's gaseous surface are the colored bands (from chemical reactions), in which the darker reddish-browns are called belts (low pressure atmospheric motion) (temperatures around -147° C) and the lighter, more bluish are zones (higher pressure) (temperatures about -154° C). Belts (atmosphere rises) and zones (atmosphere sinks) also move in opposite directions. The orange, red, and brown coloration in the clouds of Jupiter are caused by upwelling compounds that change color when they are exposed to ultraviolet light from the Sun. The exact makeup remains uncertain, but the substances are believed to be phosphorus, sulfur or possibly hydrocarbons. Nomenclature for the belts and zones are given in this illustration (from Wikipedia).

Belts and zones in the jovian atmosphere; N and S = North and South; E = Equatorial; T = Temperate; P = Polar.

These belts and zones are not stable and permanent - they can change rather abruptly but usually are restored over time. In May of 2010, the large Southern Equatorial Belt almost vanished, as seen in the comparison images below. The cause is uncertain but one hypothesis is that whitish clouds form from time to time, obscuring the dark belt below. Another is that the color fades owing to chemical changes.

The disappearance of the SEB as noted by comparing a 2009 and a 2010 image.

In Jupiter's northern hemisphere, jet winds at velocities up to 600 km/hr (420 mph) blow westward south of zones and north of belts and eastward north of zones and south of belts; this is reversed in the southern hemisphere. Global cloud decks include an outer layer of ammonia ice crystals, above a layer containing small amounts of ammonium hydrosulphide (NH4SH), and possibly a water ice crystal layer beneath. Upwelling in the belts may convert the NH4SH (perhaps including also phosphorus compounds) into the darker reds by photochemical reactions with sunlight. This profile diagram describes the pressure-temperature-composition relations in the jovian atmosphere:

Diagram showing variations of pressure and temperature with altitude (depth) within the outer jovian atmosphere; composition of layers at different altitudes also shown.

A hallmark of Jupiter's atmosphere is the prominent Great Red Spot (GRS), an oval feature (25000 x 12000 km [15500 x 750 miles]) that has persisted at least since its discovery by telescope in the 17th century. The GRS is a high pressure disturbance caused by thermal convection that carries gases up to 8 km (5 miles) higher than its surroundings, thus cooling them; its anticyclonic winds move counterclockwise (in the southern hemisphere) as it drifts through the bands. The GRS experiences a complete rotation in about 6 days. The false color view below is a Voyager close-up of the GRS in which images made by the red and blue filters are enhanced relative to green which also helps to emphasize some of the swirls and plumes peripheral to it. Red areas are higher than blue above the level of the jovian atmosphere that appears as a quasi-surface. Theories supported by laboratory experiments suppose that the GRS's color may be caused by any of "complex organic molecules, red phosphorus, or yet another sulfur compound", but a consensus has not been reached.

False color Voyager image closeup of the Great Red Spot on Jupiter.

The GRS has existed much as is since first observed by Galileo. More recent are two more Red Spots as seen here (the one at the same latitude as the GRS first appeared in the spring of 2008):

Three Red Spots on Jupiter.

The Red Spot at a more southern latitude has been around since the 1940s (it developed from the merger of several storms). Named the Little Red Spot (LRS)(it does not appear red in the image below) because different wavelengths are involved), the swirling patterns of individual curve cloud streaks indicate fast motion of the gases; a maximum wind speed of 524 kph (385 mph) has been measured:

The Little Red Spot.

But other cyclonic storms can have much shorter durations. Sometimes two storm spots within a band will close the gap between them and even merge, as shown in this sequence:

Merger of Cyclonic Storms in one of the Compositional Bands of Jupiter's Atmosphere.

Here is a color version of two of the circulating features known as White Ovals:

White Ovals.

The Galileo spacecraft has returned numerous images showing details in the circulation patterns of individual bands. Here is one typical example:

Circulation patterns in jovian atmosphere bands.

Multispectral imaging of Jupiter helps to reveal variations in the compositional banding and the appearance of cyclonic spots. In this next view, the three images were made in the Visible Blue (left), the Ultraviolet, and the Near IR (right)

Appearance of Jupiter in Blue, UV, and Near IR spectral bands.

In February, 2007, the New Horizons spacecraft passed Jupiter enroute to Pluto (see page 19-21). It proved the quality of its instrumentation with excellent looks at the planet and its moons. Here is a closeup of the atmosphere; note that a thin visible cross-section of the outer atmosphere shows at the limb.

A close view of part of Jupiter's surface.

One of Voyager's discoveries is that Jupiter has a ring system. It is more nebulous than Saturn's rings, as evident in this image.

Voyager image of the Jovian rings.

The ring's inner edge begins at about 123,000 km (76,432 mi) from the planet's center. Its fine particles, still effective as sunlight reflectors, form a continuous band about 5,200 km (3,231 mi) wide and 30 km (18.6 mi) thick that shows no conspicuous gaps.

After the Voyagers, Jupiter has been revisited in the '90s. The primary objective for the Galileo mission was to penetrate the jovian atmosphere. This spacecraft, launched on October 13, 1989, separated its probe from the Orbiter on December 7, 1995. The probe’s initial velocity on entering was about 106,000 km/hr (65,868 mph), but it then slowed greatly, due to atmospheric friction aided by a deployed parachute. It transmitted data for 57 minutes, as it descended in excess of 150 km (93.2 mi), where the pressure exceeded 24 bars (23.7 atm) at a temperature around 150° C. It encountered no thick, dense clouds, and it detected less sulphur, oxygen, and neon than expected, but found no water. The helium levels were above what was expected. The data overall suggested the probe may have entered at an anomalous hot spot, with abnormal cloud conditions. As it observed Jupiter, the Orbiter saw evidence of large thunderstorms, with rain, and some lightning. The Orbiter also monitored the Galilean satellites, taking close-ups of their surfaces that surpass those of Voyager.

JPL has three brief videos that describe the Galileo mission. Access through the JPL Video Site, then the pathway Format-->Video -->Search to bring up the list that includes "Galileo's Legacy at Jupiter", October 16, 2003, "The Big Spacecraft that Could", February 4, 2003, and "Galileo at Jupiter", May 8, 2002. To start each, once found, click on the blue RealVideo link.

Galileo spent part of its observing time monitoring Jupiter's atmosphere. The bands and convection plumes show temperature differences that broadly correlate with the patterns these atmospheric features assume. This correlation is evident in the Galileo Orbiter view, below, of a segment of bands and spots, in which the temperatures derived from the photopolarimeter divide into warmer (yellow) and somewhat cooler (orange-red to black) zones.

Galileo Orbiter photopolarimeter views of a segment of bands and spots in which the temperatures divide into warmer (yellow) and somewhat cooler (orange-red to black) zones.

The jovian atmosphere is not only dynamic and turbulent but is electrically charged, as is evident from this next view that shows lightning-like discharges, imaged when the Orbiter is looking at the nightside of Jupiter's outer atmosphere. These are the first visible lightning flashes seen on another planet.

Galileo Orbiter image showing lightening flashes in the jovian atmosphere.

This next image associates lightning strikes (bright marks in lower insert) with a specific, localized storm in the atmosphere.

Lightning in a small storm, in this colorized image taken by the Galileo Orbiter.

Jupiter has both the strongest (10x that of Earth) and the largest magnetosphere of any solar planet. The magnetic field extends out to at least 100 jovian radii from the planet (reaching to Saturn). If seen in real size from the Earth, in which Jupiter appears at its normal size, the field would cover space on the celestial sphere equal to almost three times the full Moon. Here are two plots of the magnetosphere: one using radiowaves to visualize the field; the lower one constructed from data gathered by a sensor aboard the Cassini spacecraft:

Two views of Jupiter's magnetosphere.

The Orbiter also observed aurora effects as rings at the north and south magnetic poles. The view below shows a Galileo visible image of the planet, on which are two superimposed insets made with the UV camera on the spacecraft.

Aurora effects at the poles of Jupiter as seen through the UV camera on the Galileo Orbiter.

This is a closer view of the northern aurora in UV light:

The northern aurora.

Ultraviolet auroral light comes from emissions resulting from excited ions and electrons emanating from the innermost satellite, Io, released during volcanic activity (see the next page) that Jupiter’s magnetic field captured and concentrated in the polar regions.

Jupiter is an emitter of strong radio waves (peaking at 10 cm), caused by both thermal and non-thermal processes. These waves come from the Van Allen-like radiation belts around the planet. The belts trap electrons, producing a field of 400000 rad strength (enough to kill any astronaut caught within it). Here is a plot of the detected radiation belt around Jupiter:

Jupiter's Radiation belts

Jupiter continues to be a target of additional imaging and data gathering. The Cassini spacecraft, enroute to Saturn for a rendezvous in 2004, passed by Jupiter on December 30, 2000 and continues to acquire information. Although the images are not much different from those obtained by Galileo, they do extend the monitoring and add more instrumental analysis. Here is a view of part of the jovian surface and the satellite Io; this helps to realize how small are these "moons" relative to the huge size of the planet.

A Cassini image of Jupiter's atmosphere, with the Galilean satellite Io seen in orbit.

Now, on to the four fascinating major satellites of Jupiter, plus a look at some smaller moons.

Source: http://rst.gsfc.nasa.gov