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The largest and most interesting satellite of Saturn is Titan, measuring 5,150 km (3,200 miles) in diameter It is almost as large as Ganymede, Jupiter s largest moon Nevertheless, the gigantic, gaseous planet Saturn dwarfs it (Fig 10-3) Titan is the only planetary moon that has a significant atmosphere As viewed through the most powerful telescopes, and even from space probes flying by, Titan looks something like an orange little sister of Venus The cloud layer is so thick that it hides the surface features from visual view The atmosphere of Titan is comprised mainly of nitrogen and methane and is cold by Earthly standards, far below 0 C at the surface The atmospheric pressure at the surface is about half again as great as the normal atmospheric pressure at the surface of the Earth Thus, although we would not be able to breathe Titan s air, we would at least not have to worry about being crushed to death by its pressure, as would be the case on Venus The main reason scientists find Titan so interesting is that it contains an abundance of organic chemicals The term organic does not mean that these chemicals were produced by or are necessarily indicative of living things in the environment Methane and ethane, hydrocarbons similar to natural gas, are considered organic because they have the potential to give rise to amino acids under the right conditions The impact of a large meteSaturn Titan

OSB administrative server The OSB administrative server stores the OSB catalog You can designate any server as the administrative server, and the best practice is to have it separate from the servers in the backup domain for ensuring high availability You can use the administrative server to house the RMAN catalog database and the Oracle Enterprise Manager repository, and increase the utilization rate of the server

Earth Figure 10-3 The relative size of Saturn s largest moon Titan, the planet Earth,

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Now that you have seen how the tape backup infrastructure fits together, we will look at the process involved in sizing and tuning the individual components The goal is to have an architecture that achieves the best throughput possible while meeting the constraints set by recovery time objective and, of course, the cost Tape Infrastructure Sizing Best Practices Before you start sizing and configuring the backup infrastructure, capture the performance characteristics of each component that is involved with the transfer/processing of the backup data (tape library, network, media servers, and database servers) The next step is to start with one component of the architecture and add more instances of it until you get the scalability benefits and an effective increase in throughput You should repeat this process for all the components, namely, the tape library, network, media servers, and the database servers The trick here is to make sure you do not induce bottlenecks while you perform the scaling exercise and stay focused on making the overall configuration balanced An example of a typical tape backup infrastructure with throughput rates of each component is depicted in Figure 6-4 For illustrating the sizing process, we assume the media servers connect to a full-rack Exadata Database Machine X2-2 using the 40 Gb/s InfiniBand network, and to the tape library using 8 Gb/s SAN links The tape library used is the Oracle

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orite or comet or an electrical discharge caused by a thunderstorm creates the high temperatures necessary for the formation of amino acids, which are the building blocks of life Titan is a candidate for exploration by humans The main problem to be overcome in such a visit, besides the enormous distance that separates the Saturnian system from Earth, is the powerful magnetic field surrounding Saturn, which accelerates subatomic particles from the Sun, producing intense belts of ionizing radiation Although this radiation is less intense than that in the vicinity of Jupiter, it is still much greater than the intensity of the Van Allen radiation belts surrounding the Earth Anyone who lands on Titan also would have to be prepared for the possibility of hitting a turbulent, liquid hydrocarbon surface, perhaps with floating icebergs of frozen methane and heavy methane rain or snow blowing down out of the red sky

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Rhea is 1,530 km (950 mi) in diameter It orbits in an almost perfect circle 530,000 km (330,000 mi) from its parent planet This moon is only a little more dense than water, and this fact has led astronomers to conclude that it must be comprised mainly of ice and very little rocky material Rhea, like most moons, keeps the same face toward Saturn at all times As a result, one side of the moon leads the way through space, whereas the opposite side trails behind There is a considerable difference in the appearance of the leading side of Rhea compared with the trailing side The leading side is as densely packed with craters as any part of Earth s moon, even though the surface of Rhea is mostly water ice The trailing side has far fewer craters This would be expected because the leading side would be more exposed to bombardment by meteorites Most of the rock in Rhea is believed to be contained in a small core The moon s small size and its relatively large distance from Saturn prevent heating from tidal effects, keeping the surface far below 0 C and hardening the ice so that it resembles granite and can maintain crater and mountain formations for a long time Rhea has essentially no atmosphere

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