The astronomy glossary aims to help you understand some of the terms used in this website. It is by no means a comprehensive astronomy dictionary.
The Andromeda Galaxy or MESSIER 31 (M31) is the closest large galaxy to the MILKY WAY. It is 2.5 million LIGHT YEARS away and gets its name from the CONSTELLATION in which it appears in our night sky (see picture below). The star Alpheratz is also used to form the square shape in the constellation Pegasus, even though it is now assigned exclusively to Andromeda and not Pegasus.
The Andromeda Galaxy is one of the brightest MESSIER objects with an apparent MAGNITUDE of 3.4 and is the farthest object that can be seen with the unaided eye. We only see the very bright central region, if we could see the whole of the galaxy it would stretch 6 full Moon widths across the sky (3 degrees).
It is a spiral galaxy 260,000 LIGHT YEARS in diameter containing 1 trillion stars so over twice the size of our own Milky Way galaxy. It is the most massive of the galaxies in the LOCAL CLUSTER which contains the MILKY WAY, the Triangulum galaxy (M33) and 44 other smaller galaxies. It has a double nucleus with at least one supermassive BLACK HOLE hidden at its core. There are at least 450 GLOBULAR CLUSTERS orbiting around the galaxy and some of these are the most densely populated globulars ever seen.
The Andromeda Galaxy is approaching the Milky Way at approximately 100-140 km/s and in about 3.75 billion years the galaxies will collide, merging and evolving into a new type of galaxy, an ELLIPTICAL GALAXY or a LARGE DISC GALAXY.
Finding the Andromeda Galaxy
Asteroid 3200 Phaethon was discovered in October 1983. This unusual Near Earth Asteroid (NEA) may be an extinct comet. It measures 5.1 Km in diameter and its orbit crosses the orbits of Mars, Earth, Venus and Mercury. It was the first asteroid to be discovered by a spacecraft. Its orbit is tilted at an angle of 22.2 degrees to the ECLIPTIC. It also has a highly elongated orbit; with an ECCENTRICITY of 0.88, which is more like a comet than an asteroid.
Phaethon's (pronounced FAY-a-thon) most remarkable distinction is that it approaches the Sun closer than any other numbered asteroid and comes even closer to the Sun than Mercury; it gets within 20.9 million km [13 million miles]. The surface temperature at its closest (perihelion) could reach approximately 1025 Kelvin. This is why it was named after the Greek myth of Phaëton, son of the Sun god Helios. As Phaethon approaches the Sun the dust is literally cooked off its surface. It then makes its way back to far beyond the orbit of Mars some 223 million miles from the Sun (359 million Km) in just 262 days. This far away from the Sun Phaethon cools down to very low temperatures. This constant periodical cooling and heating cycle cracks its mineralogical surface into small dusty particles. Each December, when Earth passes close to the orbit of Phaethon, the small grains swept from Phaethon by the radiation pressure (of sunlight) enter our atmosphere as the GEMINIDS METEOR SHOWER.
The Geminids meteor shower is observed between the 4th-17th December (maximum is usually December 14th). Along with the Quadrantids, observed between 1st-6th January, they are the only meteor showers originating from an asteroid rather than a comet. It will approach relatively close to the Earth on December 14, 2093, passing within 0.0198 AU (Astronomical Units).
3200 Phaethon is a rocky object with a strange blue hue (artist impression).
Astronomical twilight is defined to begin in the morning, and to end in the evening when the centre of the Sun is geometrically 18 degrees below the horizon. From the end of astronomical twilight in the evening to the beginning of astronomical twilight in the morning, the sky (away from urban light pollution) is dark enough for all astronomical observations. Most casual observers would consider the entire sky fully dark even when astronomical twilight is just beginning in the evening or just ending in the morning, and astronomers can easily make observations of point sources such as stars, but faint diffuse items such as nebulae and galaxies can be properly observed only beyond the limit of astronomical twilight. In some places, especially those with sky glow, astronomical twilight may be almost indistinguishable from night.
It takes 29.53 days for one lunation i.e. the time taken to go from, for example, New Moon back to New Moon. There are 365.24 days in a year so there are usually 12.37 lunations in one year which equates to roughly 11 days more than the number of days in 12 lunar cycles. The extra days accumulate so every 2-3 years there is an 'extra' 13th full moon. This extra full moon means that one of the seasons ends up having 4 full moons and not 3. Originally the 3rd full moon in the season with 4 full moons was called a Blue Moon. In 1946 an article was printed which misinterpreted this traditional definition; it stated that if there is a second full moon in one month then this second full moon is called a Blue Moon. This misinterpretation seems to have been widely adopted as a current description.
The Moon of course is not blue. This would be a rare event indeed and only occurs in certain atmospheric conditions; e.g., when there are volcanic eruptions or when exceptionally large fires leave particles in the atmosphere. The image you see here has been taken using a blue filter.
In this example conjunction is the position of the outer planet (in orange) in relation to the Earth when the outer planet is at the opposite side of the Sun to the Earth. At this point in the orbits of the 2 bodies the outer planet is the furthest it will be from the Earth. However because of the elliptical nature of planetary orbits the actual distance between the Earth and the outer planet will be different at each conjunction.
The diagram is simplified to show opposition and conjunction. The elliptical orbits are very exagerated.
A constellation is a group of stars that forms an imaginary outline or meaningful pattern on the CELESTIAL SPHERE. Imagine the night sky as a huge dot to dot puzzle. If you joined some of the stars by imaginary lines you would make patterns.
In ancient times poets, farmers and astronomers began to pick out patterns in the stars and named them after heroes and fabled animals. In Ptolemy's time 48 constellations were recognised by the Eastern Mediteraneans and many mythological stories were associated with them. Nowadays because we have included the whole of the celestial sphere and not just the ones that Ptolemy could see, the tally has gone up to 88.
The origins of some constellations extend back to prehistory, while others have changed. While the patterns of old seem quite specific to the brightest stars, the constellations of today make up a block of sky encompassing not only the recognised pattern of stars but all the stars within that block which are not necessarily visible to the unaided eye. Each block forms a border with another block much like the county boundaries in the UK. These specific boundaries were put in place by the International Astronomical Union in 1922 and the 88 constellations have remained since then.
We still recognise the patterns that the brighter stars make within the whole of the constellation but assigning a region of sky to one constellation has helped us to locate specific deep sky objects. For example Messier object M13 is located in the constellation Hercules (see below). The green line marks the constellation boundary.
There are three different types of double stars:
Optical doubles are unrelated stars that appear close together through chance alignment with Earth. An example of an optical double are the two stars Mizar and Alcor in the constellation Ursa Major. Look at the tail of the bear, Mizar and Alcor are the second stars in from the tip of the tail (see constellation).
Visual binaries are in mutual orbit and gravitationally bound to each other. They are seen as one star with the unaided eye but can be resolved into two with a telescope.
Non-visual binaries cannot be resolved through a telescope but they can be split into their respective components by spectroscopy (spectroscopic binaries), or more esoteric means, such as occultation (eclipsing binaries), or anomalies in proper motion (astrometric binaries).
Multiple star systems also exist but these are more complex than binary stars.
Improvements in telescopes can shift previously non-visual binaries into visual binaries, as happened with Polaris A in 2006. It is only the inability to telescopically observe two separate stars that distinguish non-visual and visual binaries.
A globular cluster is a nearly symetrical, spherical collection of hundreds of thousands of very old stars held tightly together by gravity. The stars are probably some of the first stars that formed in our Milky Way galaxy. The highest concentration of stars is in the central region making it look like a glowing almost 3 dimensional ball through a telescope.
The name is derived from the Latin globulus meaning a small sphere and there are currently about 158 known globular clusters in the Milky Way. In larger galaxies there may be many more. In fact every galaxy of sufficient mass has an associated group of globular clusters.
Several globular clusters with extremely massive cores may even have a black hole lurking at their centre but there is no scientific evidence to prove this yet.
Magnitude is a measure of how bright a celestial object looks. Those objects that can be seen with the naked eye are ranked in 6 magnitudes from first to sixth magnitude. First magnitude is the brightest and 6th magnitude the faintest, which always seems a little odd! Anyway a sixth magnitude object is exactly 100 times less bright than a first magnitude object. This means that the difference between a first and second magnitude object is approximately 2.51 times. To get the difference between a first and second magnitude object all you do is multiply 2.51 x 2.51 = 6.3.This means that a third magnitude object is about 6.3 times less bright than a first magnitude object.
To make things a little more complicated, an object 2.51 times brighter than magnitude 1 becomes magnitude 0. An object 6.3 times brighter than magnitude 1 becomes magnitude -1.
Sirius is the brightest STAR in the sky and has a magnitude of -1.44. The full Moon has a magnitude of -12.7 and the Sun has a magnitude of -26.7.
Star clusters form from the same molecular cloud. An open cluster is one that can contain from a few dozen to a few thousand stars all of similar ages. They are much more loosly bound by gravity than a globular cluster and also generally contain younger, hot stars. Because they are more loosely bound they can become disrupted by passing objects such as other clusters or clouds of gas and stars can be lost from the cluster.
Open clusters are commonly found in the disk of a galaxy but only in spiral or irregular galaxies where active star formation is still ongoing. They generally survive for a few hundred million years, with the most massive ones surviving for a few billion years.
The Pleiades or the Seven Sisters in the constellation Taurus is an example of an open cluster. It contains a group of newly formed B-type stars. It is 115 million years old and is easily seen with the unaided eye. when you start to see Pleiades rising over the eastern horizon before midnight then you know the end of summer is nigh and Autumn is on its way. The brightest stars have a surface temperature of 30,000 Kelvin, much hotter than the surface of our Sun which is about 6,000 Kelvin.
Other examples of Open Clusters include the Double Cluster in Perseus and the Coma Star Cluster in Coma Berenices (also known as Melotte 111). More than 1,100 open clusters have been discovered within the Milky Way Galaxy, and many more are thought to exist.
The Orion Nebula is also known as M42. The M refers to Charles Messier an 18th century French astronomer and comet hunter. He compiled a list of deep sky fuzzy looking objects so they would not be mistaken for comets. Not all Messier objects were actually discovered by Charles Messier himself.
Nebula (plural nebulae) is Latin for mist and they are vast areas of cloud and dust between the stars. The Orion Nebula is so huge it is visible to the naked eye even though it is 1,344 light years away. It appears to cover 1 degree of the sky, an area twice the size of the full Moon, it is actually 24 light years across. A light year is roughly equivalent to 9.5 million million Km! It is a region where new stars are formed. These new stars at the centre of the dust cloud light up the surrounding gas making it visible through a telescope.
The Orion Nebula is in the constellation of Orion, which is a very prominent constellation in the winter sky. The nebula is located in the "sword" of Orion which hangs below the 3 stars that depict his belt (see diagram on right)
One of the new stars at the centre of the Orion Nebula is Theta-1 Orionis. It is easy to understand why it is called the Trapezium because, through the telescope, you should see 4 prominent stars in the shape of a trapezium (see Diagram below).
This false colour mosaic was made by combining several exposures from the Hubble Space Telescope Image credit: NASA Picture of the day
The whole of the Moon is only ever half illuminated - the half that faces towards the Sun (inner part of the diagram). However, looking from Earth, we only see a portion of this illuminated face because as the moon orbits the Earth it changes position in space relative to the Sun and Earth. (outer part of the diagram).
New Moon is considered as the beginning of the cycle, hence the term New Moon. However, because the moon is between Earth and the Sun the Sun only illuminates the face that we do not see, the ‘Far Side of the Moon'. The face that we normally look at is in total darkness and therefore we cannot see it.
The next phase is a crescent Moon but because more and more of the illuminated face of the Moon will become visible to observers from Earth in the following days it is called a waxing crescent.
The next phase is called First Quarter. The reason why we call this phase of the moon first quarter is because it is one quarter of the way through the lunar cycle. The lunar cycle is the number of days it takes to go from one New Moon to the next and is 29.53 days. This is one lunation. First quarter is often referred to as half moon. This is because only half of the face of the moon that we see is lit by the Sun. Halfway through the lunar cycle is Full Moon when we can see the whole of the illuminated face because it is opposite the Sun with respect to the Earth.
As the illuminated face becomes less the Moon is said to be waning and when it has orbited three quarters of the way around the Earth it is said to be a Last (or Third) Quarter Moon. The next time the moon is a crescent it is a waning crescent and the edge that is illuminated is the opposite edge that is illuminated when it is a waxing crescent. Remembering this becomes easy by saying "if the Light is coming from the Left the Moon is getting Less."