E-mail
The concept of sending electronic text messages between parties in a way analogous to mailing letters or memos predates the formation of the Internet. Today it is an important one to differentiate between Internet and internal e-mail systems. Internet e-mail may travel and even be stored unencrypted on many other machines and networks out of both the sender's and the recipient's control. It is also quite possible for the content to be read and even tampered with by third parties, if anyone considers it important enough during this period.

Purely internal or intranet mail systems, where the information never leaves the corporate or organization's network and servers, is much more protected, although in any organization there will be IT and other personnel whose job may involve monitoring, or at least occasionally accessing, the email of other employees are not been addressed to them. E-mail attachments have increased the usefulness of e-mail in a wide manner. When a file is attached to an email, a text representation of the attached data is actually appended to the e-mail text, later to be reconstituted into a 'file' on the recipient's machine for their use.

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Solar System

The Solar System, is the stellar system comprising the Sun and the retinue of celestial objects gravitationally bound to it: the eight planets, their 162 known moons, three currently identified dwarf planets and their four known moons, and thousands of small bodies. This last category includes asteroids, meteoroids, comets, and interplanetary dust.

The principal component of the Solar System is the Sun ; a main sequence G2 star that contains 99.86% of the system's known mass and dominates it gravitationally. Because of its large mass, the Sun has an interior density high enough to sustain nuclear fusion, releasing enormous amounts of energy, most of which is radiated into space in the form of electromagnetic radiation, including visible light. The Sun's two largest orbiting bodies, Jupiter and Saturn, account for more than 90% of the system's remaining mass.

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