March  2021

Updated:   1 March 2021

 

Welcome to the night skies of Autumn, featuring Eridanus, Taurus, Gemini, Cancer, Leo, Hydra, Orion, Canis Major, Carina, Crux, Centaurus and Mars

 

Note:  Some parts of this webpage may be formatted incorrectly by older browsers.

 

The Alluna RC-20 Ritchey Chrétien telescope was installed in March, 2016.

The 20-inch telescope is able to locate and track any sky object (including Earth satellites and the International Space Station) with software called TheSkyX Professional, into which is embedded a unique T-Point model created for our site with the telescope itself.

 

Explanatory Notes:  

 

Times for transient sky phenomena are given using a 24 hour clock, i.e. 20:30 hrs = 8.30 pm. Times are in Australian Eastern Standard Time (AEST), which equals Universal Time (UT) + 10 hours. Daylight saving is not observed in Queensland. Observers in other time zones will need to make their own corrections where appropriate. With conjunctions of the Moon, planets and stars, timings indicate the closest approach. Directions (north or south) are approximate. The Moon’s diameter is given in arcminutes ( ’ ). The Moon is usually about 30’ or half a degree across. The 'limb' of the Moon is its edge as projected against the sky background.

Rise and set times are given for the theoretical horizon, which is a flat horizon all the way round the compass, with no mountains, hills, trees or buildings to obscure the view. Observers will have to make allowance for their own actual horizon. 

Transient phenomena are provided for the current month and the next. Geocentric phenomena are calculated as if the Earth were fixed in space as the ancient Greeks believed. This viewpoint is useful, as otherwise rising and setting times would be meaningless. In the list of geocentric events, the nearer object is given first.

When a planet is referred to as ‘stationary’, it means that its movement across the stellar background appears to have ceased, not that the planet itself has stopped. With inferior planets (those inside the Earth’s orbit, Mercury and Venus), this is caused by the planet heading either directly towards or directly away from the Earth. With superior planets (Mars out to Pluto), this phenomenon is caused by the planet either beginning or ending its retrograde loop due to the Earth’s overtaking it.

Apogee and perigee:   Maximum and minimum distances of the Moon or artificial satellite from the Earth.

Aphelion and perihelion:  Maximum and minimum distances of a planet, asteroid or comet from the Sun.

The zenith is the point in the sky directly overhead from the observer.

Eclipses always occur in pairs, a lunar and a solar but not necessarily in that order, two weeks apart.

The meridian is a semicircle starting from a point on the horizon that is exactly due north from the observer, and arching up into the sky to the zenith and continuing down to a point on the horizon that is exactly due south. On the way down it passes through the South Celestial Pole which is 26.6 degrees above the horizon at Nambour. The elevation of the South Celestial Pole is exactly the same as the observer's latitude, e.g. from Cairns it is 16.9 degrees above the horizon, and from Melbourne it is 37.8 degrees. The Earth's axis points to this point in the sky in the southern hemisphere, and to an equivalent point in the northern hemisphere, near the star Polaris, which from Australia is always below the northern horizon.

All astronomical objects rise until they reach the meridian, then they begin to set. The act of crossing or 'transitting' the meridian is called 'culmination'. Objects closer to the South Celestial Pole than its altitude above the southern horizon do not rise or set, but are always above the horizon, constantly circling once each sidereal day. They are called 'circumpolar'. The brightest circumpolar star from Nambour is Miaplacidus (Beta Carinae, magnitude = 1.67).  

A handspan at arm's length with fingers spread covers an angle of approximately 18 - 20 degrees. Your closed fist at arm's length is 10 degrees across. The tip of your index finger at arm's length is 1 degree across. These figures are constant for most people, whatever their age. The Southern Cross is 6 degrees high and 4 degrees wide, and Orion's Belt is 2.7 degrees long. The Sun and Moon average half-a-degree (30 arcminutes) across.   

mv = visual magnitude or brightness. Magnitude 1 stars are very bright, magnitude 2 less so, and magnitude 6 stars are so faint that the unaided eye can only just detect them under good, dark conditions. Binoculars will allow us to see down to magnitude 8, and the Observatory telescope can reach visual magnitude 17 or 22 photographically. The world's biggest telescopes have detected stars and galaxies as faint as magnitude 30. The sixteen very brightest stars are assigned magnitudes of 0 or even -1. The brightest star, Sirius, has a magnitude of -1.44. Jupiter can reach -2.4, and Venus can be more than 6 times brighter at magnitude -4.7, bright enough to cast shadows. The Full Moon can reach magnitude -12 and the overhead Sun is magnitude -26.5. Each magnitude step is 2.51 times brighter or fainter than the next one, i.e. a magnitude 3.0 star is 2.51 times brighter than a magnitude 4.0. Magnitude 1.0 stars are exactly 100 times brighter than magnitude 6.0 (5 steps each of 2.51 times, 2.51x2.51x2.51x2.51x2.51  =  2.51=  99.625   ..... close enough to100).

 

The Four Minute Rule

How long does it take the Earth to complete one rotation? No, it's not 24 hours - that is the time taken for the Sun to cross the meridian on successive days. This 24 hours is a little longer than one complete rotation, as the curve in the Earth's orbit means that it needs to turn a fraction more (~1 degree of angle) in order for the Sun to cross the meridian again. It is called a 'solar day'. The stars, clusters, nebulae and galaxies are so distant that most appear to have fixed positions in the night sky on a human time-scale, and for a star to return to the same point in the sky relative to a fixed observer takes 23 hours 56 minutes 4.0916 seconds. This is the time taken for the Earth to complete exactly one rotation, and is called a 'sidereal day'.

As our clocks and lives are organised to run on solar days of 24 hours, and the stars circulate in 23 hours 56 minutes approximately, there is a four minute difference between the movement of the Sun and the movement of the stars. This causes the following phenomena:

    1.    The Sun slowly moves in the sky relative to the stars by four minutes of time or one degree of angle per day. Over the course of a year it moves ~4 minutes X 365 days = 24 hours, and ~1 degree X 365 = 360 degrees or a complete circle. Together, both these facts mean that after the course of a year the Sun returns to exactly the same position relative to the stars, ready for the whole process to begin again.

    2.    For a given clock time, say 8:00 pm, the stars on consecutive evenings are ~4 minutes or ~1 degree further on than they were the previous night. This means that the stars, as well as their nightly movement caused by the Earth's rotation, also drift further west for a given time as the weeks pass. The stars of autumn, such as Orion are lost below the western horizon by mid-June, and new constellations, such as Sagittarius, have appeared in the east.  The stars change with the seasons, and after a year, they are all back where they started, thanks to the Earth's having completed a revolution of the Sun and returned to its theoretical starting point.

We can therefore say that the star patterns we see in the sky at 11:00 pm tonight will be identical to those we see at 10:32 pm this day next week (4 minutes X 7 = 28 minutes earlier), and will be identical to those of 9:00 pm this date next month or 7:00 pm the month after. All the above also includes the Moon and planets, but their movements are made more complicated, for as well as the Four Minute Drift  with the stars, they also drift at different rates against the starry background, the closest ones drifting the fastest (such as the Moon or Venus), and the most distant ones (such as Saturn or Neptune) moving the slowest.

 

 

 Solar System

 

Sun:   The Sun begins the month in the constellation of Aquarius, the Water-bearer. It leaves Aquarius and passes into Pisces, the Fishes on March 12.   

 

 

Moon: 


The Moon keeps one of its hemispheres facing the Earth due to tidal locking caused by the Earth's gravity. The far side remained unseen until the Russian probe Luna 3 went around the Moon and photographed it on October 7, 1959. Now the whole Moon has been photographed in very fine detail by orbiting satellites. The Moon circles the Earth once in a month (originally 'moonth'), the exact period being 27 days 7 hours 43 minutes 11.5 seconds. Its speed is about 1 kilometre per second or 3679 kilometres per hour. The Moon's average distance from the Earth is 384 400 kilometres, but the orbit is not perfectly circular. It is slightly elliptical, with an eccentricity of 5.5%. This means that each month, the Moon's distance from Earth varies between an apogee (furthest distance) of 406 600 kilometres, and a perigee (closest distance) of 356 400 kilometres. These apogee and perigee distances vary slightly from moth to month.  In the early 17th century, the first lunar observers to use telescopes found that the Moon had a monthly 'wobble', which enabled us to observe features which were brought into view by the wobble and then taken out of sight again. The wobble, called 'libration', amounted to 7º 54' in longitude and 6º 50' in latitude  The 'libration zone' on the Moon is the area around the edge of the Moon that comes into and out of view each month, due to libration. This effect means that, instead of only seeing 50% of the Moon from Earth, we can see up to 59%.

The animation loop below shows the appearance of the Moon over one month. The changing phases are obvious, as is the changing size as the Moon comes closer to Earth at perigee, and moves away from the Earth at apogee. The wobble due to libration is the other feature to note, making the Moon appear to sway from side to side and nod up and down.   (Credit: Wikipedia)
 

 

Phases: 


Last Quarter:           March 06         11:31 hrs         diameter = 32.1'
New Moon
:               March 13         20:22 hrs         diameter = 30.2'     Lunation #1215 begins
First Quarter
:           March 22         00:40 hrs         diameter = 30.0'
Full Moon
:                March 29         04:48 hrs         diameter = 33.0'

Last Quarter:           April 04            20:03 hrs         diameter = 31.7'
New Moon
:               April 12            12:31 hrs         diameter = 29.6'     Lunation #1216 begins
First Quarter
:           April 20            16:59 hrs         diameter = 30.5'
Full Moon
:                April 27            13:32 hrs         diameter = 33.4'


 


Lunar Orbital Elements:


March 02:             Moon at perigee (365 432 km) at 15:30 hrs, diameter = 32.7'
March 06:             Moon at descending node at 10:57 hrs, diameter = 32.1'
March 18:             Moon at apogee (405 235 km) at 14:25 hrs, diameter = 29.5'
M
arch 20:             Moon at ascending node at 13:28 hrs, diameter = 29.6'

March 30:             Moon at perigee (360 319 km) at 16:21 hrs, diameter = 33.2'

April 02:                Moon at descending node at 12:44 hrs, diameter = 32.6'
April 15:                Moon at apogee (406 131 km) at 03:16 hrs, diameter 29.4'
April 16:                Moon at ascending node at 15:51 hrs, diameter = 29.5'
April 28:                Moon at perigee (357 389 km) at 01:04 hrs, diameter = 33.4'
April 29:                Moon at descending node at 19:18 hrs, diameter = 33.2'
 

Moon at 8 days after New, as on March 23.

The photograph above shows the Moon when approximately eight days after New, just after First Quarter. A rotatable view of the Moon, with ability to zoom in close to the surface (including the far side), and giving detailed information on each feature, may be downloaded  here.  A professional version of this freeware with excellent pictures from the Lunar Reconnaissance Orbiter and the Chang orbiter (giving a resolution of 50 metres on the Moon's surface) and many other useful features is available on a DVD from the same website for 20 Euros (about AU $ 33) plus postage.

Click here for a photographic animation showing the lunar phases. It also shows the Moon's wobble or libration, and how its apparent size changes as it moves from perigee to apogee each month. It takes a little while to load, but once running is very cool !  All these downloads are freeware, although the authors do accept donations if the user feels inclined to support their work.

 


Lunar Feature for this Month

 

Each month we describe a lunar crater, cluster of craters, valley, mountain range or other object, chosen at random, but one with interesting attributes. A recent photograph from our Alluna RC20 telescope will illustrate the object. As all large lunar objects are named, the origin of the name will be given if it is important. This month we will look at the crater Marius and the hundreds of volcanic hills and domes in its vicinity.



The largest crater in this image is 41 kilometre diameter Marius at bottom centre. it lies on the western margin of the Oceanus Procellarum (Ocean of Storms). Behind it (to the west) is an extensive cluster of small volcanic domes, cones and hills called the Marius Hills. The image was taken at 8:33 pm on June 3, 2020.


Marius crater has a flat floor due to being filled with magma welling up from below until it reached about the same level as the lunar plain outside the crater. A few craterlets are visible on the floor of Marius. The largest is half in shadow, and has a diameter of 3 kilometres. The second largest, near the centre, is 2 kilometres across. The others are less than a kilometre across. The Marius Hills is the highest concentration of volcanic features on the Moon.

West of Marius are more than 200 domes, cones, shield volcanoes, and hills, and they vary between 200 and 500 metres in height. The largest ones average about 10 kilometres across their bases, the smallest between one and two kilometres. Some may be dormant volcanoes, although no activity has yet been detected, but there are quite a few instances in the image above where a dome-like hill has a circular crater about a kilometre across precisely at the summit. Such craters are probably volcanic vents, and larger ones could be calderas. A "wrinkle ridge" (a solidified ripple in the ocean of lava that formed the Oceanus Procellarum) can be seen running from the lower left-hand corner of the image past the upper rim of crater Marius.


Marius

Although Galileo always referred to the Jovian moons he had discovered in late 1609 as Jupiter I, Jupiter II, Jupiter III and Jupiter IV, in 1614 the German astronomer Simon Mayr (Marius) (1573-1624) published a book Mundus Jovialis (The World of Jupiter), in which he claimed to have discovered the four satellites over a week before Galileo. The two men had a history between them as, many years before, Galileo had forced Mayr to leave Padua University. Although Mayr’s claim was possibly true, Galileo responded that he did not believe it, and, in any case, Mayr lived in the Lutheran city of Ansbach which had not yet adopted the Gregorian calendar, and was therefore ten days behind Catholic Padua where Galileo lived. Mayr called the Jovian moons ‘the Brandenburg stars’ after his own patron, and, following a suggestion from Kepler, gave them the individual names of Io, Europa, Callisto and Ganymede.

These names did not come into official use until the 20th century, after Edward E. Barnard had discovered Jupiter V in 1892. At that time, the French astronomer Nicolas Camille Flammarion suggested naming the new satellite Amalthea, in line with a system of nomenclature suggested by John Herschel for naming the satellites of the other planets. In the 20th century, the International Astronomical Union (IAU, founded in 1919) ratified Herschel’s and Mayr’s names for planetary satellites, and subsequent discoveries were named in like manner.

Mayr had worked with Tycho Brahe in Prague for four months in 1601, and was the first European to observe the Andromeda Galaxy, which he saw with his new ‘Perspicilli Belgici’ (Belgian lenses).



The crater Marius and its hills are located inside the rectangle above.

 

Click  here  for the  Lunar Features of the Month Archive


 

Geocentric Events:



It should be remembered that close approaches of Moon, planets and stars are only perspective effects as seen from the Earth - that is why they are called 'geocentric or Earth-centred phenomena'. The Moon, planets and stars do not really approach and dance around each other as it appears to us from the vantage point of our speeding planet.


March 4:              Mars 2.5º south of the Pleiad Alcyone (Eta Tauri, mv= 2.85) at 2:35 hrs
March 5:              Limb of Moon 22 arcminutes north of the star Graffias (Beta-1 Scorpii, mv= 2.56) at 15:14 hrs
March 5:              Mercury 20 arcminutes north of Jupiter at 15:01 hrs
March 6:              Mercury at Greatest Elongation West (27º 16') at 19:56 hrs  (diameter = 7.1")
March 7:              Jupiter 47 arcminutes north of the star Iota Capricorni (mv= 4.28) at 11:01 hrs
March 7:              Limb of Moon 42 arcminutes north of the star Kaus Borealis (Lambda Sagittarii, mv= 2.82) at 22:38 hrs
March 8:              Moon 1.4º north of the star Nunki (Sigma Sagittarii, mv=2.02) at 12:07 hrs
March 9:              Moon 1.8º south of Pluto at 11:16 hrs
March 10:            Moon 3.6º south of Saturn at 09:13 hrs
March 11:            Moon 3.6º south of Jupiter at 00:40 hrs
March 11:            Neptune in conjunction with the Sun at 10:10 hrs  (diameter = 2.2")
March 11:            Moon 3.3º south of Mercury at 12:40 hrs
March 11:            Mercury 1.4º north of the star Deneb Algedi (Delta Capricorni, mv=2.85) at 13:48 hrs
March 13:            Moon 3.1º south of Venus at 13:32 hrs
March 13:            Moon 3.2º south of Neptune at 15:55 hrs
March 14:            Mercury at aphelion at 11:44 hrs  (diameter = 6.4")
March 14:            Venus 22 arcminutes south of Neptune at 14:05 hrs
March 17:            Moon 2º south of Uranus at 14:02 hrs
March 20:            Moon 1.8º south of Mars at 4:50 hrs
March 22:            Limb of Moon 41 arcminutes north of the star Mebsuta (Epsilon Geminorum (mv= 3.06) at 18:15 hrs
March 26:            Venus in superior conjunction with the Sun at 16:09 hrs
March 26:            Jupiter 1.9º north of the star Nashira (Gamma Capricorni, mv= 3.69) at 18:36 hrs
March 30:            Mercury 1.3º south of Neptune at 13:24 hrs
March 31:            Moon 2.7º north of the star Zuben Elgenubi (Alpha2 Librae, mv= 2.75) at 15:47 hrs

April 1:                Limb of Moon 15 arcminutes north of the star Graffias (Beta-1 Scorpii, mv= 2.56) at 20:28 hrs
April 4:                Moon occults the star Kaus Borealia ((Lambda Sagittarii, mv= 2.82) between 5:03 and 6:30 hrs
April 4:                Moon 2.7º north of the star Nunki (Sigma Sagittarii, mv=2.02) at 16:34 hrs
April 4:                Jupiter 1.9º north of the star Deneb Algedi (Delta Capricorni, mv=2.85) at 9:38 hrs
April 5:                Moon 1.4º south of Pluto at 17:30 hrs
April 6:                Moon 3.2º south of Saturn at 20:07 hrs
April 7:                Moon 3.5º south of Jupiter at 19:39 hrs
April 9:                Moon 3.6º south of Neptune at 11:26 hrs
April 11:              Moon 2º south of Mercury at 19:47 hrs
April 12:              Moon 2.2º south of Venus at 22:32 hrs
April 13:              Moon 2º south of Uranus at 23:54 hrs
April 16:              Pluto at western quadrature at 23:19 hrs
April 17:              Limb of Jupiter 32 arcseconds south of the star Mu Capricorni (mv=5.08) at 4:19 hrs
April 17:              Moon occults Mars between 23:22 and 0:15 hrs
April 19:              Northern limb of Moon 13 arcminutes north of the star Mebsuta (Epsilon Geminorum (mv= 3.06) at 2:36 hrs
April 19:              Mercury in superior conjunction at 11:36 hrs
April 23:              Venus 14 arcminutes south of Uranus at 11:05 hrs
April 24:              Mercury 45 arcminutes north of Uranus at 14:52 hrs
April 26:              Mercury 1.2º north of Venus at 8:58 hrs
April 27:              Mercury at perihelion at 11:24 hrs
April 28:              Moon 1.9º north of the star Zuben Elgenubi (Alpha2 Librae, mv= 2.75) at 3:44 hrs
April 29:              Moon occults the star Graffias (Beta-1 Scorpii, mv= 2.56) between 8:23 and 9:09 hrs
 

 


The Planets for this month:

 

Mercury:    This month, the innermost planet is in the eastern pre-dawn sky, having passed between the Earth and the Sun (inferior conjunction) on February 8 last. It can be found on March 1 between Saturn and Jupiter in the constellation Capricornus, which rises in the east soon after 4 am. Mercury will be at its greatest angular distance from the Sun on March 5 and 6, and will also be about a half-a-degree (a Moon width) from Jupiter on both of those dates. Mercury will continue to move east along the ecliptic, and its separation from Jupiter will increase each morning. Mercury will pass by the star Deneb Algedi on March 11, with the waning crescent Moon close by. Mercury will pass into Aquarius on March 14, and as the days pass it will continue to approach the solar glare. By April 1, Mercury will be within a handspan of the Sun, and risky to observe. It will pass through superior conjunction (on the far side of the Sun) on April 19, and will reappear in the western twilight sky in mid-May. Mercury and Venus will be half-a-degree apart on the evening of May 29, but both will be less than a handspan from the Sun.

  

Venus:    This, the brightest planet, was an 'evening star' in the first five months of 2020. It passed through inferior conjunction (when it overtook the Earth by passing between us and the Sun) on June 4, after which it moved to the eastern pre-dawn sky. It is now a 'morning star', but on March 1 it is only 6.5 degrees from the Sun, and dangerous to observe without professional light filters. This situation will continue as it passes through superior conjunction on March 26, when it will be only 1.3 degrees south of the Sun. Venus will appear as an 'evening star' once again when it extricates itself from the glare of the Sun at the end of May. By the beginning of July it will be easily seen, and on July 13 Venus and Mars will be only half-a-degree apart, both being one-and-a-half handspans from the Sun. Venus will be easy to observe from late May on, but attempts earlier than that are not recommended.

(The coloured fringes to the second, third and fifth images below are due to refractive effects in our own atmosphere, and are not intrinsic to Venus itself. The planet was closer to the horizon when these images were taken than it was for the second photograph, which was taken when Venus was at its greatest elongation from the Sun).

         early July 2020                     mid-August 2020                      March 2021                      October 2021                       December 2021        

Click here for a photographic animation showing the Venusian phases. Venus is always far brighter than anything else in the sky except for the Sun and Moon. For all of 2019 up to July, Venus appeared as an 'Morning Star' in the eastern pre-dawn sky, but in August last year it moved to the evening sky to be an 'Evening Star'. It is now quite easy to find in the west as twilight begins to fade.

Because Venus is visible as the 'Evening Star' and as the 'Morning Star', astronomers of ancient times believed that it was two different objects. They called it Hesperus when it appeared in the evening sky and Phosphorus when it was seen before dawn. They also realised that these objects moved with respect to the so-called 'fixed stars' and so were not really stars themselves, but planets (from the Greek word for 'wanderers'). When it was finally realised that the two objects were one and the same, the two names were dropped and the Greeks applied a new name Aphrodite (Goddess of Love)  to the planet, to counter Ares (God of War). We use the Roman versions of these names, Venus and Mars, for these two planets.



Venus at 6.55 pm on September 7, 2018. The phase is 36 % and the angular diameter is 32 arcseconds.

 

Mars:  The red planet is poorly-placed for viewing this month, as it is on the far side of its orbit. In mid-March it is only 6 arcseconds in diameter, less than a third of its size last October, and its brightness has fallen to magnitude 1.1. It passed through eastern quadrature (culminating at sunset) on February 1. During the first week of March, Mars will 2.5º south of the Pleiades star cluster and heading towards the Hyades cluster. It will be slightly fainter than the nearby star Aldebaran, which is also orange in colour. The waxing crescent Moon will form a small triangle with Mars and Aldebaran on the evening of March 19, and again the following night, only the configuration will be different. Mars will be in conjunction with the Sun on October 8.

In this image, the south polar cap of Mars is easily seen. Above it is a dark triangular area known as Syrtis Major. Dark Sinus Sabaeus runs off to the left, just south of the equator. Between the south polar cap and the equator is a large desert called Hellas. The desert to upper left is known as Aeria, and that to the north-east of Syrtis Major is called Isidis Regio.  Photograph taken in 1971.



Mars photographed from Starfield Observatory, Nambour on June 29 and July 9, 2016, showing two different sides of the planet.  The north polar cap is prominent.

 

Brilliant Mars at left, shining at magnitude 0.9, passes in front of the dark molecular clouds in Sagittarius on October 15, 2014. At the top margin is the white fourth magnitude star 44 Ophiuchi. Its type is A3 IV:m. Below it and to the left is another star, less bright and orange in colour. This is the sixth magnitude star SAO 185374, and its type is K0 III. To the right (north) of this star is a dark molecular cloud named B74. A line of more dark clouds wends its way down through the image to a small, extremely dense cloud, B68, just right of centre at the bottom margin. In the lower right-hand corner is a long dark cloud shaped like a figure 5. This is the Snake Nebula, B72. Above the Snake is a larger cloud, B77. These dark clouds were discovered by Edward Emerson Barnard at Mount Wilson in 1905. He catalogued 370 of them, hence the initial 'B'. The bright centre of our Galaxy is behind these dark clouds, and is hidden from view. If the clouds were not there, the galactic centre would be so bright that it would turn night into day.


Mars near opposition, July 24, 2018


Mars, called the red planet but usually coloured orange, in mid-2018 took on a yellowish tint and brightened by 0.4 magnitude, making it twice as bright as previous predictions for the July 27 opposition. These phenomena were caused by a great dust storm which completely encircled the planet, obscuring the surface features so that they were only seen faintly through the thick curtain of dust. Although planetary photographers were mostly disappointed, many observers were interested to see that the yellow colour and increased brightness meant that a weather event on a distant planet could actually be detected with the unaided eye - a very unusual thing in itself.

The three pictures above were taken on the evening of July 24, at 9:05, 9:51 and 11:34 pm. Although the fine details that are usually seen on Mars were hidden by the dust storm, some of the larger features can be discerned, revealing how much Mars rotates in two and a half hours. Mars' sidereal rotation period (the time taken for one complete rotation or 'Martian day') is 24 hours 37 minutes 22 seconds - a little longer than an Earth day. The dust storm began in the Hellas Desert on May 31, and after two months it still enshrouded the planet. In September it began to clear, but by then the close approach had passed.
 

Central meridian: 295º.
 

 

The two pictures immediately above were taken on the evening of September 7, at 6:25 and 8:06 pm. The dust storm was finally abating, and some of the surface features were becoming visible once again. This pair of images also demonstrates the rotation of Mars in 1 hour 41 minutes (equal to 24.6 degrees of longitude), but this time the view is of the opposite side of the planet to the set of three above. As we were now leaving Mars behind, the images are appreciably smaller (the angular diameter of the red planet had fallen to 20 arcseconds). Well past opposition, Mars on September 7 exhibited a phase effect of 92.65 %.


 
Central meridian: 180º.

 

Jupiter:   This gas giant planet reached conjunction with the Sun (passing behind it) on January 29. It is now in the pre-dawn eastern sky in the constellation of Capricornus, with Saturn and Mercury close by. This grouping will be joined by the waning crescent Moon on March 10, 11 and 12. Jupiter will not be seen before midnight until late May.

     

Jupiter as photographed from Nambour on the evening of April 25, 2017. The images were taken, from left to right, at 9:10, 9:23, 9:49, 10:06 and 10:37 pm. The rapid rotation of this giant planet in a little under 10 hours is clearly seen. In the southern hemisphere, the Great Red Spot (bigger than the Earth) is prominent, sitting within a 'bay' in the South Tropical Belt. South of it is one of the numerous White Spots. All of these are features in the cloud tops of Jupiter's atmosphere.



Jupiter as it appeared at 7:29 pm on July 2, 2017. The Great Red Spot was in a similar position near Jupiter's eastern limb (edge) as in the fifth picture in the series above. It will be seen that in the past two months the position of the Spot had drifted when compared with the festoons in the Equatorial Belt, so must rotate around the planet at a slower rate. In fact, the Belt enclosing the Great Red Spot rotates around the planet in 9 hours 55 minutes, and the Equatorial Belt takes five minutes less. This high rate of rotation has made the planet quite oblate. The prominent 'bay' around the Red Spot in the five earlier images appeared to be disappearing, and a darker streak along the northern edge of the South Tropical Belt was moving south. In June this year the Spot began to shrink in size, losing about 20% of its diameter. Two new white spots have developed in the South Temperate Belt, west of the Red Spot. The five upper images were taken near opposition, when the Sun was directly behind the Earth and illuminating all of Jupiter's disc evenly. The July 2 image was taken just four days before Eastern Quadrature, when the angle from the Sun to Jupiter and back to the Earth was at its maximum size. This angle means that we see a tiny amount of Jupiter's dark side, the shadow being visible around the limb of the planet on the left-hand side, whereas the right-hand limb is clear and sharp. Three of Jupiter's Galilean satellites are visible, Ganymede to the left and Europa to the right. The satellite Io can be detected in a transit of Jupiter, sitting in front of the North Tropical Belt, just to the left of its centre.  
 

Jupiter at opposition, May 9, 2018

     

Jupiter reached opposition on May 9, 2018 at 10:21 hrs, and the above photographs were taken that evening, some ten to twelve hours later. The first image above was taken at 9:03 pm, when the Great Red Spot was approaching Jupiter's central meridian and the satellite Europa was preparing to transit Jupiter's disc. Europa's transit began at 9:22 pm, one minute after its shadow had touched Jupiter's cloud tops. The second photograph was taken three minutes later at 9:25 pm, with the Great Red Spot very close to Jupiter's central meridian.

The third photograph was taken at 10:20 pm, when Europa was approaching Jupiter's central meridian. Its dark shadow is behind it, slightly below, on the clouds of the North Temperate Belt. The shadow is partially eclipsed by Europa itself. The fourth photograph at 10:34 pm shows Europa and its shadow well past the central meridian. Europa is the smallest of the Galilean satellites, and has a diameter of 3120 kilometres. It is ice-covered, which accounts for its brightness and whitish colour. Jupiter's elevation above the horizon for the four photographs in order was 50º, 55º, 66º and 71º. As the evening progressed, the air temperature dropped a little and the planet gained altitude. The 'seeing' improved slightly, from Antoniadi IV to Antoniadi III. At the time of the photographs, Europa's angular diameter was 1.57 arcseconds. Part of the final photograph is enlarged below.

 

Jupiter at 11:34 pm on May 18, nine days later. Changes in the rotating cloud patterns are apparent, as some cloud bands rotate faster than others and interact. Compare with the first photograph in the line of four taken on May 9. The Great Red Spot is ploughing a furrow through the clouds of the South Tropical Belt, and is pushing up a turbulent bow wave.
 

Jupiter at opposition, June 11, 2019

     

    

 

Jupiter reached opposition on June 11, 2019 at 01:20 hrs, and the above photographs were taken that evening, some twenty to twenty-two hours later. The first image above was taken at 10:01 pm, when the Great Red Spot was leaving Jupiter's central meridian and the satellite Europa was preparing to transit Jupiter's disc. Europa's transit began at 10:11 pm, and its shadow touched Jupiter's cloud tops almost simultaneously. Europa was fully in transit by 10:15 pm. The second photograph was taken two minutes later at 10:17 pm, with the Great Red Spot heading towards Jupiter's western limb.

The third photograph was taken at 10:41 pm, when Europa was about a third of its way across Jupiter. Its dark shadow is trailing it, slightly below, on the clouds of the North Temperate Belt. The shadow is partially eclipsed by Europa itself. The fourth photograph at 10:54 pm shows Europa and its shadow about a quarter of the way across. This image is enlarged below. The fifth photograph shows Europa on Jupiter's central meridian at 11:24 pm, with the Great Red Spot on Jupiter's limb. The sixth photograph taken at 11:45 pm shows Europa about two-thirds of the way through its transit, and the Great Red Spot almost out of sight. In this image, the satellite Callisto may be seen to the lower right of its parent planet. Jupiter's elevation above the horizon for the six photographs in order was 66º, 70º, 75º, 78º, 84º and 86º. As the evening progressed, the 'seeing' proved quite variable.

There have been numerous alterations to Jupiter's belts and spots over the thirteen months since the 2018 opposition. In particular, there have been major disturbances affecting the Great Red Spot, which appears to be slowly changing in size or "unravelling".


It was very fortuitous that, during the evenings of the days when the 2018 and 2019 oppositions occurred, there was a transit of one of the satellites as well as the appearance of the Great Red Spot. It was also interesting in that the same satellite, Europa, was involved both times.

 


Saturn:  
The ringed planet reached conjunction with the Sun on January 24, whereupon it moved from the evening twilight sky to the eastern pre-dawn sky. It is now in the constellation of Capricornus, and can be seen rising in the east and above Mercury and Jupiter before dawn breaks. This grouping will be joined by the waning crescent Moon on March 10, 11 and 12. Saturn will not be seen before midnight until late May.  

Left: Saturn showing the Rings when edge-on.    Right: Over-exposed Saturn surrounded by its satellites Rhea, Enceladus, Dione, Tethys and Titan - February 23/24, 2009.




 Saturn with its Rings wide open on July 2, 2017. The shadow of its globe can just be seen on the far side of the Ring system. There are three main concentric rings: Ring A is the outermost, and is separated from the brighter Ring B by a dark gap known as the Cassini Division, which is 4800 kilometres wide, enough to drop Australia through. Ring A also has a gap inside it, but it is much thinner. Called the 'Encke Gap', it is only 325 kilometres wide and can be seen in the image above. The innermost parts of Ring B are not as bright as its outermost parts. Inside Ring B is the faint Ring C, almost invisible but noticeable where it passes in front of the bright planet as a dusky band. Spacecraft visiting Saturn have shown that there are at least four more Rings, too faint and tenuous to be observable from Earth, and some Ringlets. Some of these extend from the inner edge of Ring C to Saturn's cloudtops. The Rings are not solid, but are made up of countless small particles, 99.9% water ice with some rocky material, all orbiting Saturn at different distances and speeds. The bulk of the particles range in size from dust grains to car-sized chunks. At bottom centre, the southern hemisphere of the planet can be seen showing through the gap of the Cassini Division. The ring system extends from 7000 to 80 000 kilometres above Saturn's equator, but its thickness varies from only 10 metres to 1 kilometre. The globe of Saturn has a diameter at its equator of 120 536 kilometres. Being made up of 96% hydrogen and 3% helium, it is a gas giant, although it has a small, rocky core. There are numerous cloud bands visible.

The photograph above was taken when Saturn was close to opposition, with the Earth between Saturn and the Sun. At that time, the shadow of Saturn's globe upon the Ring system was directly behind the planet and hardly visible. The photograph below was taken at 7:14 pm on September 09, 2018, when Saturn was near eastern quadrature. At such a time, the angle from the Sun to Saturn and back to the Earth is near its maximum, making the shadow fall at an angle across the Rings as seen from Earth. It may be seen falling across the far side of the Ring to the left side of the globe.


Uranus:
 
This ice giant planet shines at about magnitude 5.8, so a pair of binoculars or a small telescope is required to observe it. Uranus is currently near the junction of the constellations Pisces, Cetus and Aries. This month it is about half a handspan south-east of the second magnitude star Sheratan. Uranus came to opposition last year on November 1 and reached eastern quadrature on January 26. The waxing crescent Moon will be 2.6 degrees east-south-east of Uranus at 7 pm on the evening of March 17. Uranus will be in conjunction with the Sun on May 1. 

 

Neptune:   The icy blue planet reached opposition (rising at sunset) on September 12 and eastern quadrature on December 10. A telescope is required to observe Neptune, as its magnitude is 7.9 and its angular diameter is only 2 arcseconds. It is located near the boundary of Aquarius and Pisces, 9 degrees south of the centre of the asterism known as the Circlet. This month it is too close to the Sun to be observed. It will pass through conjunction on March 11.

Neptune, photographed from Nambour on October 31, 2008


Pluto:
   The erstwhile ninth and most distant planet reached conjunction with the Sun on January 15. Pluto's angular diameter is 0.13 arcseconds, less than one twentieth that of Neptune. Located this month in the eastern end of Sagittarius, it is a 14.1 magnitude object.  Although it is very small and faint, it can be observed this month as it is 45 degrees (two-and-a-half handspans) above the Sun at sunrise. At mid-month, Pluto rises above the theoretical east-south-eastern horizon at about 1:20 am, so is well-placed for observing after 4 am. A telescope with an aperture of 25 cm is capable of locating Pluto when the seeing conditions are right.  The waning crescent Moon will be close to Pluto on the morning of March 9.

 

  

The movement of the dwarf planet Pluto in two days, between 13 and 15 September, 2008. Pluto is the one object that has moved.
Width of field:   200 arcseconds

This is a stack of four images, showing the movement of Pluto over the period October 22 to 25, 2014. Pluto's image for each date appears as a star-like point at the upper right corner of the numerals. The four are equidistant points on an almost-straight line. Four eleventh magnitude field stars are identified.  A is GSC 6292:20, mv = 11.6.  B is GSC 6288:1587, mv = 11.9.  C is GSC 6292:171, mv = 11.2.  D is GSC 6292:36, mv = 11.5.  (GSC = Guide Star Catalogue).   The position of Pluto on October 24 (centre of image) was at Right Ascension = 18 hours 48 minutes 13 seconds,  Declination =  -20º 39' 11".  The planet moved 2' 51" with respect to the stellar background during the three days between the first and last images, or 57 arcseconds per day, or 1 arcsecond every 25¼ minutes.



 



Planetary Alignments



During March there will be a fine alignment of three planets, but it will occur in the hours before dawn in the east-south-eastern sky. On March 1 the line of three will be standing almost vertically above the eastern horizon from about 4:30 am until dawn breaks. The uppermost one will be Saturn, the middle one Mercury, and Jupiter is the brightest one, closest to the horizon. In the first five days of March, Mercury (the fastest mover) will move down to Jupiter, which it will pass at 4 am on March 5, at a distance of 20 arcminutes north of Jupiter. For the rest of March, Mercury will head towards the Sun, until it cannot be seen due to the solar glare.

Saturn and Jupiter will both remain in the constellation Capricornus until Jupiter crosses into Aquarius on April 25. Jupiter will begin its retrograde loop on June 21, and will head back towards Saturn, crossing back into Capricornus on August 19. Saturn will reach opposition on August 2, and Jupiter will reach opposition on August 20.

The movements of planets including their alignments and close-up images can be watched using the freeware  Stellarium.

 

 

 

Meteor Showers:



No meteor showers in March.

Lyrids                              April 23                  Waxing gibbous Moon, 71% sunlit                         ZHR = 15
                                        Radiant:  Near the star Vega. 
      Associated with Comet Thatcher.

Pi Puppids                      April 24                   Waxing gibbous Moon, 81% sunlit                        ZHR = 10
                                        Radiant:  Between the False Cross and the tail of Canis Major


Use this 
Fluxtimator  to calculate the number of meteors predicted per hour for any meteor swarm on any date, for any place in the world.


ZHR = zenithal hourly rate (number of meteors expected to be observed at the zenith in one hour). The maximum phase of meteor showers usually occurs between 3 am and sunrise. The reason most meteors are observed in the pre-dawn hours is because at that time we are on the front of the Earth as it rushes through space at 107 000 km per hour (30 km per second). We are meeting the meteors head-on, and the speed at which they enter our atmosphere is the sum of their own speed plus ours. In the evenings, we are on the rear side of the Earth, and many meteors we see at that time are actually having to catch us up. This means that the speed at which they enter our atmosphere is less than in the morning hours, and they burn up less brilliantly.

Although most meteors are found in swarms associated with debris from comets, there are numerous 'loners', meteors travelling on solitary paths through space. When these enter our atmosphere, unannounced and at any time, they are known as 'sporadics'. On an average clear and dark evening, an observer can expect to see about ten meteors per hour. They burn up to ash in their passage through our atmosphere. The ash slowly settles to the ground as meteoric dust. The Earth gains about 80 tonnes of such dust every day, so a percentage of the soil we walk on is actually interplanetary in origin. If a meteor survives its passage through the air and reaches the ground, it is called a 'meteorite'.  In the past, large meteorites (possibly comet nuclei or small asteroids) collided with the Earth and produced huge craters which still exist today. These craters are called 'astroblemes'. Two famous ones in Australia are Wolfe Creek Crater and Gosse's Bluff. The Moon and Mercury are covered with such astroblemes, and craters are also found on Venus, Mars, planetary satellites, minor planets, asteroids and even comets.




 

Comets:

 

Comet NEOWISE (C/2020 F3)

Another new comet is heading towards the Sun. Comet NEOWISE (C/2020 F3) is approaching the orbit of Mercury and is presently at magnitude 7.4, three magnitudes brighter than expected. Located in the constellation of Orion north of the star Betelgeuse, it can be seen with binoculars from the Northern Hemisphere, but is close to the glare of the Sun. It has been photographed on June 10 by Michael Mattiazzo of Swan Hill, Victoria, but it is heading north and will soon be lost to southern hemisphere observers. It was at its closest approach to the Sun (perihelion) on July 3, swinging around the far side and heading outbound. Comet NEOWISE (C/2020 F3)'s nucleuse is quite large, recent images revealing it to be about 5 kilometres across. This may account for its survival of its close encounter with the Sun. It had its closest approach to the Earth, 103 505 306 kilometres, on July 23.

Note:  NEOWISE refers to the Near-Earth Object Wide-field Infrared Survey Explorer satellite which discovered this comet. This satellite was placed in orbit in December 2009 as the WISE (Wide-field Infrared Survey Explorer). Its mission was to chart the sky in the infrared band, and it discovered thousands of minor planets and star clusters. Having completed its survey in a little over a year, it was placed in hibernation in February 2011. In September 2013 it was reactivated and assigned a new mission - to search the sky for and identify any objects that might present a danger by coming too close to the Earth. Its name was therefore changed to NEOWISE. It studies these Near-Earth Objects through their thermal emissions.
 


Comet
SWAN (C/2020 F8) and Comet ATLAS (2019 Y4)

Both of these comets appeared in the last two months in orbits that would cause them to dive towards the Sun's surface before swinging around the Sun and heading back towards the far reaches of the Solar System. Such comets are called 'Sun grazers', and their close approach to the Sun takes them through its immensely powerful gravitational field and the hot outer atmosphere called the 'corona'. They brighten considerably during their approach, but most do not survive and disintegrate as the ice which holds them together melts. While expectations were high that these two would emerge from their encounter and put on a display as bright comets with long tails when they left the Sun, as they came close to the Sun they both broke up into small fragments of rock and ice and ceased to exist. Comet NEOWISE above is on the same course and may also break up, or we may be third time lucky.


 

Comet 46P/Wirtanen

In December 2018, Comet 46P/Wirtanen swept past Earth, making one of the ten closest approaches of a comet to our planet since 1960. It was faintly visible to the naked eye for two weeks. Although Wirtanen's nucleus is only 1.2 kilometres across, its green atmosphere became larger than the Full Moon, and was an easy target for binoculars and small telescopes. It reached its closest to the Sun (perihelion) on December 12, and then headed in our direction. It passed the Earth at a distance of 11.5 million kilometres (30 times as far away as the Moon) on December 16. In the week preceding it was at its brightest at magnitude 4, but this was a cloudy week at Nambour. It passed between the Pleiades and Hyades star clusters on the night of December 19-20, but the light of the almost Full Moon made it difficult to see. It then headed towards the star Capella in Auriga, which it passed on December 24-25. It is currently 470 million kilometres away in the constellation Virgo, between Spica and Arcturus, and close to the star Heze (Zeta Virginis), but at 18th magnitude it is too faint for most amateur telescopes. Click  here  for more information and charts.



Comet 46/P Wirtanen was photographed on November 29, 2018 between 9:45 and 9:47 pm.  The comet's position was Right Ascension = 2 hrs 30 min 11 secs, Declination = 21º 43' 13", and it was heading towards the top of the picture. The nearest star to the comet's position, just to its left, is GSC 5862:549, magnitude 14.1. The spiral galaxy near the right margin is NGC 908. The right-hand star in the yellow circle is SAO 167833, magnitude 8.31.

Comet 46/P Wirtanen on November 30, 2018. This image is a stack of five exposures between 8:13 and 9:05 pm. The comet's movement over the 52 minute period can be seen, the five images of the comet merging into a short streak. It is heading towards the upper left corner of the image, and is brightening as it approaches the Sun, with perihelion occurring on December 12. The images of the stars in the five exposures overlap each other precisely. The length of the streak indicates that the comet is presently moving against the starry background at 1.6º per day. The comet at 9:05 pm was at Right Ascension = 2 hrs 32 min 56 secs, Declination = 20º 27' 20". The upper star in the yellow circle is SAO 167833, magnitude 8.31, the same one circled in the preceding picture but with higher magnification. It enables the two photographs to be linked.

Comet 46/P Wirtanen at perihelion on December 12, 2018, at 00:55 am. It was faintly visible to the unaided eye, but easily visible through binoculars.  The circled star has a magnitude of 15.77, and the brighter one just to its left is GSC 60:1162, magnitude 13.8. The comet is moving north-east, or to the right. Its position at the time of the photograph was RA = 3 hr 23 min 13 sec, Declination +4º 34' 31", at the boundary of the constellations Cetus and Taurus. The comet may brighten as it passes by the Earth on December 16. Width of field = 18.6 arcminutes.

 

 Comet Lulin

This comet, (C/2007 N3), discovered in 2007 at Lulin Observatory by a collaborative team of Taiwanese and Chinese astronomers, is now in the outer Solar System, and has faded below magnitude 15.

Comet Lulin at 11:25 pm on February 28, 2009, in Leo. The brightest star is Nu Leonis, magnitude 5.26.

 

The LINEARrobotic telescope operated by Lincoln Near Earth Asteroid Research is used to photograph the night skies, searching for asteroids which may be on a collision course with Earth. It has also proved very successful in discovering comets, all of which are named ‘Comet LINEAR’ after the centre's initials. This name is followed by further identifying letters and numbers. Generally though, comets are named after their discoverer, or joint discoverers. There are a number of other comet and near-Earth asteroid search programs using robotic telescopes and observatory telescopes, such as:
Catalina Sky Survey, a consortium of three co-operating surveys, one of which is the Australian Siding Springs Survey (below),
Siding Spring Survey, using the 0.5 metre Uppsala Schmidt telescope at Siding Spring Observatory, N.S.W., to search the southern skies,
LONEOS, (Lowell Observatory Near-Earth Object Search), concentrating on finding near-Earth objects which could collide with our planet,
Spacewatch, run by the Lunar and Planetary Laboratory of the University of Arizona,
Ondrejov, run by Ondrejov Observatory of the Academy of Sciences in the Czech Republic, 
Xinglong, run by Beijing Astronomical Observatory 

Nearly all of these programs are based in the northern hemisphere, leaving gaps in the coverage of the southern sky. These gaps are the areas of sky where amateur astronomers look for comets from their backyard observatories.

To find out more about current comets, including finder charts showing exact positions and magnitudes, click here. To see pictures of these comets, click here.

 

The 3.9 metre Anglo-Australian Telescope (AAT) at the Australian Astronomical Observatory near Coonabarabran, NSW.

 

 

 

Deep Space

 

 

Sky Charts and Maps available on-line:


There are some useful representations of the sky available here. The sky charts linked below show the sky as it appears to the unaided eye. Stars rise four minutes earlier each night, so at the end of a week the stars have gained about half an hour. After a month they have gained two hours. In other words, the stars that were positioned in the sky at 8 pm at the beginning of a month will have the same positions at 6 pm by the end of that month. After 12 months the stars have gained 12 x 2 hours = 24 hours = 1 day, so after a year the stars have returned to their original positions for the chosen time. This accounts for the slow changing of the starry sky as the seasons progress.

The following interactive sky charts are courtesy of Sky and Telescope magazine. They can simulate a view of the sky from any location on Earth at any time of day or night between the years 1600 and 2400. You can also print an all-sky map. A Java-enabled web browser is required. You will need to specify the location, date and time before the charts are generated. The accuracy of the charts will depend on your computer’s clock being set to the correct time and date.

To produce a real-time sky chart (i.e. a chart showing the sky at the instant the chart is generated), enter the name of your nearest city and the country. You will also need to enter the approximate latitude and longitude of your observing site. For the Sunshine Coast, these are:

latitude:   26.6o South                      longitude:   153o East

Then enter your time, by scrolling down through the list of cities to "Brisbane: UT + 10 hours". Enter this one if you are located near this city, as Nambour is. The code means that Brisbane is ten hours ahead of Universal Time (UT), which is related to Greenwich Mean Time (GMT), the time observed at longitude 0o, which passes through London, England. Click here to generate these charts.

_____________________________________


Similar real-time charts can also be generated from another source, by following this second link:

Click here for a different real-time sky chart.

The first, circular chart will show the full hemisphere of sky overhead. The zenith is at the centre of the circle, and the cardinal points are shown around the circumference, which marks the horizon. The chart also shows the positions of the Moon and planets at that time. As the chart is rather cluttered, click on a part of it to show that section of the sky in greater detail. Also, click on Update to make the screen concurrent with the ever-moving sky.

The stars and constellations around the horizon to an elevation of about 40o can be examined by clicking on

View horizon at this observing site

The view can be panned around the horizon, 45 degrees at a time. Scrolling down the screen will reveal tables showing setup and customising options, and an Ephemeris showing the positions of the Sun, Moon and planets, and whether they are visible at the time or not. These charts and data are from YourSky, produced by John Walker.

The charts above and the descriptions below assume that the observer has a good observing site with a low, flat horizon that is not too much obscured by buildings or trees. Detection of fainter sky objects is greatly assisted if the observer can avoid bright lights, or, ideally, travel to a dark sky site. On the Sunshine Coast, one merely has to travel a few kilometres west of the coastal strip to enjoy magnificent sky views. On the Blackall Range, simply avoid streetlights. Allow your eyes about 15 minutes to become dark-adapted, a little longer if you have been watching television. Small binoculars can provide some amazing views, and with a small telescope, the sky’s the limit.

This month, the Eta Carinae Nebula is available for viewing all night, but will be best seen after 10 pm, as at mid-month it culminates at 1 am.

 

 

 

The Stars and Constellations for this month:

 

This description of the night sky is for 9 pm on March 1 and 7 pm on March 31. They start at Orion, which is very high in the north-west.

 

This month, Orion (see below) is high in the north-west. By mid-month, Orion will have set by midnight. Canis Major (the Large Dog) is just west of the zenith at this time, with the brilliant white star Sirius (Alpha Canis Majoris) showing the Dog's heart. Sirius, also known as the Dog Star, is the brightest star in the night sky and is about a handspan from the zenith. The brilliant white star Rigel (Beta Orionis) is about two handspans west of the zenith. Nearly overhead are the constellations Puppis, the Stern (of the ship, Argo) and Columba, the Dove. Columba culminates at 8 pm on March 1.

Sirius (Alpha Canis Majoris) is the brightest star in the night sky. It has been known for centuries as the Dog Star. It is a very hot A0 type star, larger than our Sun. It is bright because it is one of our nearest neighbours, being only 8.6 light years away. The four spikes are caused by the secondary mirror supports in the telescope's top end. The faintest stars on this image are of magnitude 15. To reveal the companion Sirius B, which is currently 10.4 arcseconds from its brilliant primary, the photograph below was taken with a magnification of 375x, although the atmospheric seeing conditions in the current heatwave were more turbulent. The exposure was much shorter to reduce the overpowering glare from the primary star.



Sirius is a binary, or double star. Whereas Sirius A is a main sequence star like our Sun, only larger, hotter and brighter, its companion Sirius B is very tiny, a white dwarf star nearing the end of its life. Although small, Sirius B is very dense, having a mass about equal to the Sun's packed into a volume about the size of the Earth. In other words, a cubic centimetre of Sirius B would weigh over a tonne. Sirius B was once as bright as Sirius A, but reached the end of its lifespan on the main sequence much earlier, whereupon it swelled into a red giant. Its outer layers were blown away, revealing the incandescent core as a white dwarf. All thermonuclear reactions ended, and no fusion reactions have been taking place on Sirius B for many millions of years. Over time it will radiate its heat away into space, becoming a black dwarf, dead and cold. Sirius B is 63000 times fainter than Sirius A. Sirius B is seen at position angle 62º from Sirius A (roughly east-north-east, north is at the top), in the photograph above which was taken at Nambour on January 31, 2017.  That date is exactly 155 years after Alvan Graham Clark discovered Sirius B in 1862 with a brand new 18.5 inch (47 cm) telescope made by his father, which was the largest refractor existing at the time.


The constellation Taurus with the clusters Pleiades and Hyades is between Orion and the north-western horizon. The brightest star in Taurus is a star dominating (but not actually a member of) the Hyades cluster. This is Aldebaran, a K5 orange star with a visual magnitude of 0.87. It is only half as far away as the Hyades. The Pleiades is a small group like a question mark, and is often called the Seven Sisters, although excellent eyes are needed to detect the seventh star without optical aid. All the stars in this cluster are hot and blue. They are also the same age, as they formed as a group out of a gas cloud or nebula. There are actually more than 250 stars in the Pleiades.  The Pleiades will have disappeared by 10 pm early in the month, and the rest of Taurus follows them below the horizon soon after. The planet Mars will be alongside the Pleiades as night falls on March 1. Venus and Mercury will be near the Pleiades and underneath the Hyades in the first week of May, but this will occur at sunset and will be swamped with the glare of the setting Sun.

The Pleiades is the small cluster at centre left, while the Hyades is the much larger grouping at centre right.

Wisps of a nebula through which the Pleiades are passing can be seen around the brighter stars in the cluster.


Between Orion’s head and the north-western horizon is a large constellation shaped roughly like a pentagon. It is north of Taurus. This is Auriga the Charioteer, its brightest star being Capella, at the bottom of the tilted pentagon. Capella is the sixth brightest star in the sky, after Sirius, Canopus, Alpha Centauri, Beta Centauri and Vega. To the left of Capella is a small triangle of stars known as 'The Kids’. The lowest star in this triangle is Epsilon Aurigae, one of the largest stars known. It is also very distant.

To the east of Auriga, Gemini is quite high, the two twin stars at its eastern end, Pollux and Castor being due north. At 9 pm at the beginning of the month they are straddling the meridian (the line that runs from due south to due north and passing through the zenith - directly overhead). When a sky object crosses the meridian, it is said to be culminating. At that point, it ceases rising and begins setting. The Twins will have set by 1.30 am.

Tonight, at a little over two handspans above the northern horizon, and directly above Pollux and Castor, is the first magnitude star Procyon, which is the brightest star in the constellation Canis Minor (the Small Dog).

High in the north-east is another zodiacal constellation, Leo, the Lion. The bright star Regulus (Alpha Leonis) marks the Lion’s heart, and Denebola, the star marking the tip of the lion's tail, is low in the east-north-east. From the southern hemisphere, we always see the Lion upside-down. His head and mane are marked by a curved line of stars shaped like an upside-down question mark. This line is also known as the 'Reaping Hook' or 'Sickle', the star Regulus marking the end of the Sickle's handle.

Between Gemini and Leo is the faint constellation of Cancer the Crab. Though a fairly unremarkable constellation in other ways, Cancer does contain a large star cluster called Praesepe or the Beehive, which presents well in binoculars. Also known as M44* , Praesepe is a little more than halfway along a line between Pollux and Regulus.

Rising above the eastern horizon is the next zodiacal constellation after Leo, Virgo, the Virgin. The brightest star in Virgo is Spica, an ellipsoidal variable star whose brightness averages magnitude 1. This makes it the sixteenth brightest star, and its colour is blue-white. Spica is about 10 degrees above the theoretical eastern horizon at this time. Between Denebola and Spica is a fainter star, Porrima, which has a magnitude of 2.74. 

High in the east above Spica is the constellation Corvus the Crow, shaped like a quadrilateral of magnitude 3 stars. A large but faint constellation, Hydra, the Water Snake, winds its way from near Procyon around the north-eastern part of the sky at an altitude of about 60 degrees above the horizon. It passes over the top of Corvus and Virgo to end near Libra, which will not rise until 10 pm (at the beginning of the month).

Hydra has one bright star, Alphard, mv=2.2, an orange star that was known by Arabs in ancient times as ‘The Solitary One’, as it lies in an area of sky with no other bright stars nearby.

Well up in the south-south-east, Crux (Southern Cross) is almost horizontal. The two Pointers Alpha and Beta Centauri lie below Crux. Crux will have rotated clockwise to a vertical position by 1 am at mid-month. Surrounding Crux on three sides is the large constellation Centaurus, and between Crux and the southern horizon are two brilliant stars, Alpha and Beta Centauri. Beta is the one nearer to Crux. These two stars are also known as the Guardians of the Cross.

Crux is at centre, lying horizontally. Beneath Crux lies the Coalsack. Towards the bottom are the two Pointers, Alpha and Beta Centauri. At top centre, the Eta Carinae nebula, also shown below.

To the right of Crux is a small, fainter quadrilateral of stars, Musca, the Fly. Out of all the 88 constellations, it is the only insect. Below and to the right of Alpha Centauri and underneath Musca is a (roughly) equilateral triangle of 4th magnitude stars. This is the constellation Triangulum Australe, the Southern Triangle. It is about half a handspan above the south-south-eastern horizon.

Between Crux and Sirius is a very large area of sky filled with interesting objects. This was once the constellation Argo Navis, named for Jason’s famous ship used by the Argonauts in their quest for the Golden Fleece. The constellation Argo was found to be too large, so modern star atlases divide it into three sections - Carina (the Keel) , Vela (the Sails) and Puppis (the Stern).

The central part of the Eta Carinae nebula, showing dark lanes, molecular clouds, and glowing clouds of fluorescing hydrogen

The Keyhole, a dark cloud obscuring part of the Eta Carinae Nebula

The Homunculus, a tiny planetary nebula ejected by the eruptive variable star, Eta Carinae

One and a half handspans south of Sirius is the second brightest star in the night sky, Canopus (Alpha Carinae). On the border of Carina and Vela is the False Cross, larger and more lopsided than the Southern Cross. The False Cross is a little more than a handspan above Crux and to the right, and is also lying on its side at this time of year. It is high in the south, and will soon culminate. Both of these Crosses are actually more like kites in shape, for, unlike Cygnus (the Northern Cross) they have no star at the intersection of the two cross arms.

A handspan above the south-south-western horizon is Achernar, Alpha Eridani. It is the brightest star in Eridanus the River, which winds its way with faint stars from Achernar in a northerly direction to Cursa, a mv= 2.9 star close to brilliant Rigel in Orion. At magnitude 0.49, Achernar is the ninth brightest star. It swings down towards the south-south-westerly horizon during the evening, and sets soon after midnight.

High in the south, about 43 degrees above the horizon, the Large Magellanic Cloud (LMC) is faintly visible as a diffuse glowing patch. It is a little less than a handspan below (south of) Canopus. About a handspan below the LMC is the Small Magellanic Cloud (SMC), a smaller glowing patch. The LMC and SMC are described below. The major planets Jupiter and Saturn will not rise above the eastern horizon until after 2:30 am at the beginning of March.

The zodiacal constellations visible tonight, starting at the western horizon and heading east (passing about two handspans north of the zenith, are Aries, Taurus, Gemini, Cancer, Leo and Virgo.

 

 

The season of the Hunter and his Dogs

 

Two of the most spectacular constellations in the sky may be seen near the zenith as soon as darkness falls. These are Orion the Hunter, and his large dog, Canis Major. Orion straddles the celestial equator, midway between the south celestial pole and its northern equivalent. This means that the centre of the constellation, the three stars known as Orion's Belt, rise due east and set due west. 

Orion:

This is one of the most easily recognised constellations, as it really does give a very good impression of a human figure. From the northern hemisphere he appears to stand upright when he is high in the sky, but from our location ‘down under’ he appears lying down when rising and setting, and upside down when high in the sky. You can, though, make him appear upright when high in the sky (near the meridian), by observing him from a reclining chair, with your feet pointing to the south and your head tilted back

Orion has two bright stars marking his shoulders, the red supergiant Betelgeuse and Bellatrix. A little north of a line joining these stars is a tiny triangle of stars marking Orion’s head. The three stars forming his Belt are, from west to east, Mintaka, Alnilam and Alnitak. These three stars are related, and all lie at a distance of 1300 light years. They are members of a group of hot blue-white stars called the Orion Association.

The red supergiant star, Betelgeuse, is a variable star. In late 2019, its brightness suddenly dropped from 0.5 to 1.5 over the period of several weeks. Such a dimming was unprecedented, a full magnitude, taking it from being the 9th brightest night-time star to the 21st. Prior to this event, Betelgeuse was slightly brighter than nearby Aldebaran in Taurus (the 14th brightest star), but by the end of January it was noticeably dimmer. It continued to fade, and soon it was fainter than its close neighbour Bellatrix (26th brightest) and approaching the brightness of the stars Alnilam (29th brightest) and Alnitak (30th brightest) in Orion’s Belt, a change easily noticeable to the naked eye. Astronomers also detected that its shape had become 'lop-sided'. Whether Betelgeuse would recover or become the Milky Way’s first supernova since Cassiopeia A in ~1667 AD was unknown. By April of 2020 Betelgeuse had returned to normal brightness.

To the south of the Belt, at a distance of about one Belt-length, we see another faint group of stars in a line, fainter and closer together than those in the Belt. This is Orion’s Sword. Orion’s two feet are marked by brilliant Rigel and fainter Saiph. Both of these stars are also members of the Orion Association.

The Saucepan, with Belt at right, M42 at upper left.

Orion is quite a symmetrical constellation, with the Belt at its centre and the two shoulder stars off to the north and the two knee stars to the south. It is quite a large star group, the Hunter being over twenty degrees (a little more than a handspan) tall. 

The stars forming the Belt and Sword are popularly known in Australia as ‘The Saucepan’, with the Sword forming the Saucepan’s handle. Tonight this asterism appears right-side up, as in the photographs above. The faint, fuzzy star in the centre of the Sword, or the Saucepan's handle, is a great gas cloud or nebula where stars are being created. It is called the ‘Great Nebula in Orion’ or ‘M42’ (number 42 in Messier’s list of nebulae). A photograph of it appears below:

The Sword of Orion, with the Great Nebula, M42, at centre

The central section of the Great Nebula in Orion. At the brightest spot is a famous multiple star system, the Trapezium, illustrated below.

New stars are forming in the nebula. At the brightest spot is a famous multiple star system, the Trapezium, illustrated below.

Canis Major

Above Orion as twilight ends (facing west), a brilliant white star will be seen about one handspan away. This is Sirius, or Alpha Canis Majoris, and it is the brightest star in the night sky with a visual magnitude of -1.43. It marks the heart of the hunter's dog, and has been known for centuries as the Dog Star. As we see him tonight, the dog is on his feet with his tail at upper left. A front leg stretches down from Sirius to Mirzam. It is also known as Beta Canis Majoris, which tells us that it is the second-brightest star in the constellation. Mirzam is about one-third of a handspan below Sirius.

The hindquarters of the Dog are indicated by a large right-angled triangle of stars located above and to the left of Sirius. The end of his tail is the top-left corner of the triangle, about one handspan south (above and to the left) of Sirius. It is marked by a blue-white star, Aludra.

Both Sirius and Rigel are bright white stars and each has a tiny, faint white dwarf companion. Whereas a small telescope can reveal the companion to Rigel quite easily, the companion to Sirius the Dog Star, (called ‘the Pup’), can only be observed by using a powerful telescope with excellent optics during rare periods of a completely still atmosphere, as it is very close to brilliant Sirius and is usually lost in the glare..

Canis Major as it appears almost overhead at 9 pm at mid-month (observer facing west).

Canis Minor    

By 8.00 pm at mid-month, this small constellation is about one and a half handspans due north of the zenith. It contains only two main stars, the brighter of which is Procyon (Alpha Canis Minoris). This yellow-white star of mv= 0.5 forms one corner of a large equilateral triangle, the other two corners being the red Betelgeuse and white Sirius. Beta Canis Minoris is also known as Gomeisa, a blue-white star of mv= 3.1.

 

 

Some fainter constellations

 

Between the two Dogs is the constellation Monoceros the Unicorn, undistinguished except for the presence of the remarkable Rosette Nebula. South of Orion is a small constellation, Lepus the Hare. Between Lepus and the star Canopus is the star group Columba the Dove. Eridanus the River winds its way from near Orion west of the zenith to Achernar, high in the south-west. Between Achernar and the western horizon is the star Fomalhaut, a white star of first magnitude in the small constellation of Piscis Austrinus (the Southern Fish). To the left of Fomalhaut is the triangular constellation of Grus, the Crane. Between the zenith and the south-western horizon are a number of small, faint constellations, Horologium, Pictor, Caelum, Mensa, Tucana, Phoenix, Hydrus and Reticulum. The LMC lies in the constellation Dorado, and the South Celestial Pole is in the very faint constellation Octans.

 

 

Finding the South Celestial Pole

 

The South Celestial Pole is that point in the southern sky around which the stars rotate in a clockwise direction. The Earth's axis is aimed exactly at this point. For an equatorially-mounted telescope, the polar axis of the mounting also needs to be aligned exactly to this point in the sky for accurate tracking to take place.

Project a line from the top of the Cross (the star Gacrux) down through its base (the star Acrux) and continue straight on towards the south for another four Cross lengths. This will locate the approximate spot. There is no bright star to mark the Pole, whereas in the northern hemisphere they have Polaris (the Pole Star) to mark fairly closely the North Celestial Pole.

Another way to locate the South Celestial Pole is to draw an imaginary straight line joining Beta Centauri (a handspan above the south-south-eastern horizon) to Achernar (a handspan above the south-western horizon. At 8 pm at mid-month, both stars will be at similar altitudes and the line will be horizontal. Bisect this line to find the pole with an accuracy of two degrees.

Interesting photographs of this area can be taken by using a camera on time exposure. Set the camera on a tripod pointing due south, and open the shutter for thirty minutes or more. The stars will move during the exposure, being recorded on the film as short arcs of a circle. The arcs will be different colours, as the stars are. All the arcs will have a common centre of curvature, which is the south celestial pole.

A wide-angle view of trails around the South Celestial Pole, with Scorpius and Sagittarius at left, Crux and Centaurus at top, and Carina and False Cross at right.

Star trails between the South Celestial Pole and the southern horizon. All stars that do not pass below the horizon are circumpolar.

 

 

Double and multiple stars

 

Estimates vary that between 15% and 50% of stars are single bodies like our Sun, although the latest view is that less than 25% of stars are solitary. At least 30% of stars and possibly as much as 60% of stars are in double systems, where the two stars are gravitationally linked and orbit their mutual centre of gravity. Such double stars are called binaries. The remaining 20%+ of stars are in multiple systems of three stars or more. Binaries and multiple stars are formed when a condensing Bok globule or protostar splits into two or more parts.

Binary stars may have similar components (Alpha Centauri A and B are both stars like our Sun - B is even said to have an Earth-sized planet), or they may be completely dissimilar, as with Albireo (Beta Cygni, where a bright golden giant star is paired with a smaller bluish main sequence star).

     

 The binary stars Rigil Kentaurus (Alpha Centauri) at left, and Albireo (Beta Cygni) at right.

     

Rigel (Beta Orionis, left) is a binary star which is the seventh brightest star in the night sky.  Rigel A is a large white supergiant which is 500 times brighter than its small companion, Rigel B, Yet Rigel B is itself composed or a very close pair of Sun-type stars that orbit each other in less than 10 days. Each of the two stars comprising Rigel B is brighter in absolute terms than Sirius (see above). The Rigel B pair orbit Rigel A at the immense distance of 2200 Astronomical Units, equal to 12 light-days. (An Astronomical Unit or AU is the distance from the Earth to the Sun.)  In the centre of the Great Nebula in Orion (M42) is a multiple star known as the Trapezium (right). This star system has four bright white stars, two of which are binary stars with fainter red companions, giving a total of six. The hazy background is caused by the cloud of fluorescing hydrogen comprising the nebula.

Acrux, the brightest star in the Southern Cross, is also known as Alpha Crucis.  It is a close binary, circled by a third dwarf companion.

Alpha Centauri (also known as Rigil Kentaurus, Rigil Kent or Toliman) is a binary easily seen with the smallest telescope. The components are both solar-type main sequence stars, one of type G and the other, slightly cooler and fainter, of type K. Through a small telescope this star system looks like a pair of distant but bright car headlights.

Alpha Centauri A and B take 80 years to complete an orbit, but a tiny third component, the 11th magnitude red dwarf Proxima Centauri, takes about 1 million years to orbit the other two. It is about one tenth of a light year from the bright pair and a little closer to us, hence its name. This makes it our nearest interstellar neighbour, with a distance of 4.3 light years. Red dwarfs are by far the most common type of star, but, being so small and faint, none is visible to the unaided eye. Because they use up so little of their energy, they are also the longest-lived of stars. The bigger a star is, the shorter its life.

Alpha Centauri, with Proxima

Proxima Centauri

Knowing the orbital period of the two brightest stars A and B, we can apply Kepler’s Third Law to find the distance they are apart. This tells us that Alpha Centauri A and B are about 2700 million kilometres apart or about 2.5 light hours. This makes them a little less than the distance apart of the Sun and Uranus (the orbital period of Uranus is 84 years, that of Alpha Centauri A and B is 80 years.)

Albireo (Beta Cygni) is sometimes described poetically as a large topaz with a small blue sapphire. It is one of the sky’s most beautiful objects. The stars are of classes G and B, making a wonderful colour contrast. It lies at a distance of 410 light years, 95 times further away  than Alpha Centauri.

Binary stars may be widely spaced, as the two examples just mentioned, or so close that a telescope is struggling to separated them (Acrux, Castor, Antares, Sirius). Even closer double stars cannot be split by the telescope, but the spectroscope can disclose their true nature by revealing clues in the absorption lines in their spectra. These examples are called spectroscopic binaries. In a binary system, closer stars will have shorter periods for the stars to complete an orbit. Eta Cassiopeiae takes 480 years for the stars to circle each other. The binary with the shortest period is AM Canum Venaticorum, which takes only 17½ minutes.

Sometimes one star in a binary system will pass in front of the other one, partially blocking off its light. The total light output of the pair will be seen to vary, as regular as clockwork. These are called eclipsing binaries, and are a type of variable star, although the stars themselves usually do not vary.

 

 

 

Star Clusters


The two clusters in Taurus, the Pleiades and the Hyades, are known as Open Clusters or Galactic Clusters. The name 'open cluster' refers to the fact that the stars in the cluster are grouped together, but not as tightly as in globular clusters (see below). The stars appear to be loosely arranged, and this is partly due to the fact that the cluster is relatively close to us, i.e. within our galaxy, hence the alternate name, 'galactic cluster'. These clusters are generally formed from the condensation of gas in a nebula into stars, and some are relatively young.

The photograph below shows a typical open cluster, M7* . It is found in the constellation Scorpius, just below the scorpion's sting. It lies in the direction of our galaxy's centre. The cluster itself is the group of white stars in the centre of the field. Its distance is about 380 parsecs or 1240 light years.

Galactic Cluster M7 in Scorpius

Outside the plane of our galaxy, there is a halo of Globular Clusters. These are very old, dense clusters, containing perhaps several hundred thousand stars. These stars are closer to each other than is usual, and because of its great distance from us, a globular cluster gives the impression of a solid mass of faint stars. Many other galaxies also have a halo of globular clusters circling around them.

The largest and brightest globular cluster in the sky is NGC 5139**, also known as Omega Centauri. It has a slightly oval shape. It is an outstanding winter object, but is also observable in autumn. Shining at fourth magnitude, it is faintly visible to the unaided eye, but is easily seen with binoculars, like a light in a fog. A telescope of 20 cm aperture or better will reveal its true nature, with hundreds of faint stars giving the impression of diamond dust on a black satin background. It lies at a distance of 5 kiloparsecs, or 16 300 light years.

The globular cluster Omega Centauri

The central core of Omega Centauri

There is another remarkable globular, second only to Omega Centauri. About two degrees below the SMC (see below), binoculars can detect a fuzzy star. A telescope will reveal this faint glow as a magnificent globular cluster, lying at a distance of 5.8 kiloparsecs. Its light has taken almost 19 000 years to reach us. This is NGC 104, commonly known as 47 Tucanae. Some regard this cluster as being more spectacular than Omega Centauri, as it is more compact, and the faint stars twinkling in its core are very beautiful. This month, 47 Tucanae is low in the south-south-west, and not clearly visible. By 10 pm Omega Centauri is high enough for detailed viewing.

Observers aiming their telescopes towards the SMC generally also look at the nearby 47 Tucanae, but there is another globular cluster nearby which is also worth a visit. This is NGC 362, which appears to lie above 47 Tucanae as we see it in mid-evening this month. It is less than half as bright as the other globular, but this is because it is more than twice as far away. Its distance is 12.6 kiloparsecs or 41 000 light years, so it is about one-fifth of the way from our galaxy to the SMC. Both NGC 104 and NGC 362 are always above the horizon for all parts of Australia south of the Tropic of Capricorn.

Globular Cluster NGC104 in Tucana

The globular cluster NGC 6752 in the constellation Pavo.

 

*     M42:This number means that the Great Nebula in Orion is No. 42 in a list of 103 astronomical objects compiled and published in 1784 by Charles Messier. Charles was interested in the discovery of new comets, and his aim was to provide a list for observers of fuzzy nebulae and clusters which could easily be reported as comets by mistake. Messier's search for comets is now just a footnote to history, but his list of 103 objects is well known to all astronomers today, and has even been extended to 110 objects.

**    NGC 5139: This number means that Omega Centauri is No. 5139 in the New General Catalogue of Non-stellar Astronomical Objects. This catalogue was first published in 1888 by J. L. E. Dreyer under the auspices of the Royal Astronomical Society, as his New General Catalogue of Nebulae and Clusters of Stars. As larger telescopes built early in the 20th century discovered fainter objects in space, and also dark, obscuring nebulae and dust clouds, the NGC was supplemented with the addition of the Index Catalogue (IC). Many non-stellar objects in the sky have therefore NGC numbers or IC numbers. For example, the famous Horsehead Nebula in Orion is catalogued as IC 434. The NGC was revised in 1973, and lists 7840 objects. 

The recent explosion of discovery in astronomy has meant that more and more catalogues are being produced, but they tend to specialise in particular types of objects, rather than being all-encompassing, as the NGC / IC try to be. Some examples are the Planetary Nebulae Catalogue (PK) which lists 1455 nebulae, the Washington Catalogue of Double Stars (WDS) which lists 12 000 binaries, the General Catalogue of Variable Stars (GCVS) which lists 28 000 variables, and the Principal Galaxy Catalogue (PGC) which lists 73 000 galaxies. The largest modern catalogue is the Hubble Guide Star Catalogue (GSC) which was assembled to support the Hubble Space Telescope's need for guide stars when photographing sky objects. The GSC contains nearly 19 million stars brighter than magnitude 15.

 

 

Two close galaxies

 

High in the south, to the left of Achernar, two large smudges of light may be seen. These are the two Clouds of Magellan, known to astronomers as the LMC (Large Magellanic Cloud) and the SMC (Small Magellanic Cloud). The LMC is to the left and above the SMC, and is noticeably larger. They lie at a distance of 160 000 light years, and are about 60 000 light years apart. They are dwarf galaxies, and they circle our own much larger galaxy, the Milky Way. The LMC is slightly closer, but this does not account for its larger appearance. It really is larger than the SMC, and has developed as an under-sized barred spiral galaxy.

From our latitude both Magellanic Clouds are circumpolar. This means that they are closer to the South Celestial Pole than that Pole's altitude above the horizon, so they never dip below the horizon. They never rise nor set, but are always in our sky. Of course, they are not visible in daylight, but they are there, all the same.

The Large Magellanic Cloud - the bright knot of gas to left of centre is the famous Tarantula Nebula (below)

These two Clouds are the closest galaxies to our own, but lie too far south to be seen by the large telescopes in Hawaii, California and Arizona. They are 15 times closer than the famous Andromeda and Triangulum galaxies referred to above, and so can be observed in much clearer detail. Our great observatories in Australia, both radio and optical, have for many years been engaged in important research involving these, our nearest inter-galactic neighbours. 

 

 

Why are some constellations bright, while others are faint ?

 

The Milky Way is a barred spiral galaxy some 100000 – 120000 light-years in diameter which contains 100 – 400 billion stars. It may contain at least as many planets as well. Our galaxy is shaped like a flattened disc with a central bulge. The Solar System is located within the disc, about 27000 light-years from the Galactic Centre, on the inner edge of one of the spiral-shaped concentrations of gas and dust called the Orion Arm. When we look along the plane of the galaxy, either in towards the centre or out towards the edge, we are looking along the disc through the teeming hordes of stars, clusters, dust clouds and nebulae. In the sky, the galactic plane gives the appearance which we call the Milky Way, a brighter band of light crossing the sky. This part of the sky is very interesting to observe with binoculars or telescope. The brightest and most spectacular constellations, such as Crux, Canis Major, Orion and Scorpius are located close to the Milky Way.

If we look at ninety degrees to the plane, either straight up and out of the galaxy or straight down, we are looking through comparatively few stars and gas clouds and so can see out into deep space. These are the directions of the north and south galactic poles, and because we have a clear view in these directions to distant galaxies, these parts of the sky are called the intergalactic windows. The southern window is in the constellation Sculptor, not far from the star Fomalhaut. This window is too low in the south-west in the early evenings this month for useful viewing. The northern window is between the constellations Virgo and Coma Berenices, roughly between the stars Denebola and Arcturus. It begins to rise in the east-north-east at 8 pm at mid-month, and is well placed for viewing at midnight.

Some of the fainter and apparently insignificant constellations are found around these windows, and their lack of bright stars, clusters and gas clouds presents us with the opportunity to look out across the millions of light years of space to thousands of distant galaxies. 

 

 

Astronomy Picture of the Day

Click here to access a new spectacular picture every day - this link will also provide you with access to a wonderful library of astronomical photographs from telescopes, spacecraft and manned lunar missions.

 

 

Virtual Moon freeware

Study the Moon in close-up, spin it around to see the far side, find the names and physical attributes of craters, seas, ranges and other features, by clicking  here.

 

 

 

Calsky software

Check out where the planets and their moons are, as well as most other sky objects, by clicking  here.


 

 

Stellarium freeware

New version. Check out where the stars and constellations are, as well as most other sky objects, by clicking  here.



 

 

Observatory Home Page and Index