The first spacecraft to photograph Saturn was Pioneer 11 on September 1, 1979.
Voyagers 1 and 2 also photographed Saturn, but the vast acquisition of knowledge did not really begin until the arrival of the Cassini-Huygens Spacecraft on June 30, 2004.
The dark side of Saturn's rings was photographed by Voyager 1 as it flew by the side opposite the sun. The dense B-ring -- the reddish-brown band --appears dark because it blocks much of the sunlight. It is the brightest ring when viewed from earth.
Image credit: Spinrad, Hyron. "Saturn." World Book Online Reference Center. 2004. World Book, Inc. http://www.worldbookonline.com/wb/Article?id=ar492440)
After its seven-year journey through the Solar System on board the Cassini spacecraft, ESA’s Huygens probe successfully descended through the atmosphere of Titan, Saturn’s largest moon, and safely landed on its surface. The probe started its descent through Titan’s hazy cloud layers from an altitude of about 1270 km at 11:13 CET. During the following three minutes Huygens had to decelerate from 18 000 to 1400 km per hour. A sequence of parachutes then slowed it down to less than 300 km per hour. At a height of about 160 km the probe’s scientific instruments were exposed to Titan’s atmosphere. At about 120 km, the main parachute was replaced by a smaller one to complete the descent. It touched down at 13:34 CET. The probe began transmitting data to Cassini four minutes into its descent and continued to transmit data after landing at least as long as Cassini was above Titan’s horizon. (www.esa.int/esaMI/Cassini-Huygens/SEMQ1QQ3K3E_0.html).
Recently [April 3/10], activity taking place in the rings has scientists buzzing. "According to theory, astronomical discs should be uniform and smooth, with everything moving serenely along, but our observations have shown that life isn't as simple as that," said Burns. Instead, the researchers see particles ranging in size from a few centimeters to many meters in radius. And, according to studies by Hedman and Nicholson, two competing forces -- gravitational attraction that tries to clump ring particles together and tidal forces that pull them apart -- cause particles in the A and B rings (the two main rings) to form self-gravity wakes, or elongated clumps. as they orbit the planet.
Saturn's moons, meanwhile, exert their own influence on the ring particles, causing a scalloped pattern that rotates with the moon and ripples away, with individual particles moving in and out of the ripple, like water molecules moving in and out of a wave in the ocean. These ripples, so-called spiral density waves, push the moons that caused them outward, away from the rings. (www.saturntoday.com)
On 6 October 2009, the discovery was announced of a tenuous outer disk of material that is in the plane of Phoebe's orbit, which is tilted 27 degrees from Saturn's equatorial plane. The ring is from 128 to 207 times the radius of Saturn, and is thought to originate from micrometeoroid impacts on Phoebe. (www.sciencenews.org/view/generic/id/48097/title/Largest_known_planetary_ring_discovered).
Information comes in almost daily about some new discovery about Saturn. For further inquiries and the latest developments log onto one or more of the following web sites:
www.csa.com/discoveryguides/enceladus/review3.php
www.saturntoday.com
http://www.nasa.gov/worldbook/saturn_worldbook.html
www.nasa.gov/mission_pages/cassini/main/index.html
http://solarsystem.nasa.gov/planets/profile.cfm?Object=Saturn
http://nssdc.gsfc.nasa.gov/planetary/factsheet/saturnfact.html
Stan Taylor
This article was first published in Crucible Online, June, 2010 www.stao.org
