**Glossary of terms used on the Project Pluto WWW site**

Italian version

This portion of the Web site is obviously quite incomplete... as the need arises, phrases will be added to this section.

** Delta-T. **
Delta-T is the difference, in seconds, between
Dynamical Time and Universal Time. It's
therefore also known as "TD-UT".

Delta-T basically reflects the difference between an "ideal" Earth that spins at a constant rate of exactly once per day relative to the Sun, and the "real" Earth that spins somewhat more erratically due to irregular tidal effects from the Moon. The major result of that tidal effect is that the Earth's rotation slows down gradually, so that the length of a day is gradually increasing. However, there are a lot of unpredictable speedups and slowdowns on top of that gradual increase, which makes the amount of Delta-T uncertain in the distant past and future.

** Dynamical Time (TD). **
TD is the successor to the older "Ephemeris Time". In this time
system, a "second" is a unit of constant length, so we have a uniform
time scale. (In the Universal Time scale, in
contrast, we're willing to adjust the length of a day so it will
match the somewhat irregular motion of the earth.)

Various flavors of TD are of great importance in astronomical calculations. In these, it's essential that a "second" at one time match the length of a "second" at another time.

** Julian Day (JD). ** The "traditional" calendrical systems,
with uneven units such as months, days, and years, and months and
years of unequal lengths, is not very handy for astronomical
computations. Therefore, astronomers commonly reckon time according
to the Julian Day system, which simply counts the elapsed days (and
decimal fraction of a day) since noon, 1 January -4712,
Universal Time. Based on this system, noon at 1 January 2000 was
JD 2451545.0.

For astronomers, this system offers several advantages. If you want to know the number of days elapsed between two different dates, you can just subtract the JD of one instant from that of another. You'll very rarely deal with dates before the year -4712, so the JD value will almost always be positive. Conversion between "day, month, year" and JD values is a little cumbersome, but is explained in many reference works (in fact, it is part of the basic astronomical function library available on this Web site.) Time zones are no longer a worry.

**Universal Time (UT), Coordinated Universal Time (UTC).**
The time system usually used for timing astronomical
events is Universal Time, also known as UT. There are several
"versions" of UT, but the one you normally encounter is UTC.
This is essentially the civil time used at Greenwich; corrected
for time zones, it is used throughout the world.

To convert from UTC to your local time zone (in the US), subtract five hours to get EST, six to get CST, seven for MST, and eight for PST. For Daylight Savings time, subtract one hour less than this.

Originally, "Universal Time" referred to a time scale that matched, as closely as could be determined, the actual rotation of the earth. There are some problems with this, because the earth's rotation speeds up and slows down irregularly. There are sudden jumps due to earthquakes, for example, and a seasonal adjustment as ice caps freeze and thaw. (Think of an ice skater twirling and speeding up as she pulls her arm in. Similarly, if ice melts at the poles and flows toward the equator, the earth will slow down a bit. And there's a long-term slowdown due to tides from the sun and moon.)

This is not a big effect, and it wasn't until a century or so ago that astronomers could even notice it. Now, of course, with atomic clocks, it's much more noticeable.

The end result is that one "real" rotation of the Earth is not going to be exactly 24 hours, or 1440 minutes, or 86400 seconds, long. In general, it will be a little more than this (and getting a little longer, on average, over the decades), and the amount of "extra" time will vary somewhat erratically. (In contrast, the Ephemeris Time scale disregards the rotation of the earth, so each day and second is of constant length.)

A little thought provides two possible solutions to the problem of irregular "days". You can re-define a "second" to be a little longer, so there will be exactly 86400 of them in a rotation of the earth. In this case, the length of a "second" will vary from one day to the next. This sort of Universal Time is called UT1.

The second solution is to leave the "second" as defined by atomic clocks: one "second" is the duration of 9 192 631 770 oscillations of a particular state of a cesium atom. In this case, since a particular rotation of the earth is going to be a little more than 86400 seconds, you will sometimes have to insert an extra second at the end of a day: a "leap second". This is exactly analogous to the way in which, since a year is a little over 365 days, we sometimes have to insert a "leap day" into the calendar. This sort of Universal Time is called UTC or Coordinated Universal Time, and is the "normal" sort of civil UT.

"Leap seconds" are always inserted at either 30 June 23:59:59 or on 31 December 23:59:59. Those days can therefore be 86401 seconds long instead of 86400 seconds long. Since the earth's rotation is irregular, the insertion of leap seconds is also irregular.