A Transit of Mercury across the solar disk is a relatively rare occurrence that averages about thirteen each century. They are however more frequent than Venus transits, which occur in pairs roughly every 120 years. (See Transit of Venus Page) Mercury cannot transit once every 116 days (synodic period) because its orbit is highly elliptical and tilted some 7° to the ecliptic. Transits can only occur when the planetary orbit intersects or moves across the ecliptic. This is specifically during the times of the ascending or descending nodes, when the Earth is exactly aligned with Mercury and the Sun. Therefore transits can only happen when Mercury both passes through its inferior conjunction AND when the nodes are in alignment. Subsequently, these particular geometric positions do mean that all transits are six months apart — in either early May or early to mid-November. Average transit dates of the event are either the 8th May or 10th November, and these can vary only by one or two days around these times.
Historically, transits of Mercury were known since about the time of the telescope.
One of the first valuable avenues astronomical research with the inner planets was to use their transits to determine the value astronomical unit (AU), as to, in turn, to find the true scale of the Solar System. During the expedition of Lt. James Cook, he famously observed the Transit of Venus on 3rd June 1768, but unbeknown to most, Cook also observed a transit of Mercury on 10th November 1769 from New Zealand for the use of the same purpose. (Also see article The Dawn of Australian Astronomy for further discussion.)
Later, serious discussion of these transits was made by French astronomer Le Verrier during mid-1800s, who used the perturbations of Mercury as a means of determining the mass of Venus I.e. Williams (1938) He used observations from twelve Mercury transits between 1697 and 1832, and organised new timings for the transits of 1845 and 1848. [In Annales de l’Observatoire de Paris, 5 (1859).] Using these results, to also derived improved orbital elements and corrections for the planet motion. [Le Verrier’s small book entitled “Théorie du Mouvement de Mercure”
From this, also it was later found that the ambiguity with the precession of the perihelion of Mercury, that was eventually explained by Einstein’s Theory of Relativity. Le Verrier found that motion precesses perihelia by 38.3 arcsec; per century, but he was unable to explain its cause. By the 1870s, Simon Newcomb reinvestigated the problem and agreed with this disparity, and by 1898 he found that perihelion increased by century 43.37 arcsec. Debate continued on the veracity of the accuracy of these earlier transits, and this appeared in a paper by R.T.A. Innes.
Three of the last transits happened on 15th November 1999, 07th May 2003 and 08th November 2006. From Australasia, the May 2003 was not a full transit across the solar disk, and only the initial ingress contact was seen in the mid-afternoon from around 15h 14m A.E.S.T. (05 U.T.) Observers throughout much of Asia, Russia, Europe and Africa were able to see both ingress and egress events. On 08th November 2006 the last Mercury transit could be seen from New Zealand and the eastern coast of Australia, yet was invisible in Europe and much of North America. The next locally observable transit will be on 10th May 2016, but will not be seen again from Australian shores until 13th November 2032.
Mercury in 2003 glanced only near the edges of the Sun, whose contact entered the mean position angles (P.A.) of 14.9° and exiting at 291.7°. Average duration of the entire transit event will take 05h 18m 50.2 second with the least possible angular distance being 11′ 48″ — roughly one-third the solar diameter. This mid-event was invisible from everywhere Australia eastward of an imaginary line roughly between Darwin and Perth. Ingress and egress are divided into two phases — the exterior (I and II) and interior (III and IV) contacts of each side of the Mercurian disk. The time it takes to enter the solar disk is about 04 minutes 27 seconds, and at the mid-time, it will seem as if a smallish bite has been taken out of the Sun. The whole transit takes around 5 hours, which averages between 1600 AD and 2300 AD as 04 hours 53 minutes.
Slight differences in the placement of Mercury’s disk occur with different latitudes on Earth. In this case, such differences only amount to several minutes. Interestingly, during the last 1999 transit there was significant differences where you were placed on Earth. Then Mercury only just grazed the solar limb.
Transits general appear like a small-blackened disk similar to one small black dot on a piece of paper, subtending about 12.0 arcsec across. When the orbit of Mercury passes near aphelion, this makes the planet to be near its observed greatest maximum size. By eye, at least by the safest observational method of solar telescopic projection, the planet does not look like any sunspot because it is quite inky black and obviously too symmetrically round and without the usual outer penumbra area of the sunspot.
Although fairly sluggish in motion, some general movement will be detectable in over some minutes when compared to other solar feature like nearby sunspots, whose own progress across the solar disk can only be really detected daily. Its relative small size of Mercury compared to the Sun is about two-hundredths its diameter.
Most recommend that the best telescopic magnification is about 80× to 120×, with higher magnifications often limited because of the general poor seeing conditions. Of course, observers should always heed the important warning below;
One of the only real serious scientific endeavours is knowing the contact events timings at the solar limb edges. This may not be easy as it seems because of the effects of atmospheric seeing and when the events start are subject to considerable uncertainty. Worse is, unlike Venus, the size of the apparent disk is small, requiring a decent aperture above 20cm. or so. Some, because of this, have recommended making timings in Hydrogen-alpha (Hα) filters rather than ordinary projected white-light. This is because prominences can be focussed on or placed to backdrop Mercury’s disk before to the contact points, thus increasing the observational accuracy. Perhaps the U.S. Naval Observatory would likely be interested in such observations. If they did, they would require the exact known geographical position that have been taken from some accurate topographic or even by way of Google maps. Also need would be the times, timing method, estimation of observational errors, and the observation conditions.
All November transits can recur over intervals of seven, thirteen, or forty-six years, but May transits recur in either thirteen, or forty-six years. These differing periods are caused by the relative motions of Mercury during either aphelion or perihelion. Overall, November perihelion transits are longer, though Mercury has a smaller 10 arcsec disk. All May aphelions are generally shorter but have slightly larger Mercurian disk of up to 12 arcsec. Furthermore, the May transits of Mercury are 1.9 times less likely than November ones.
Between 1600 AD and 2300 AD, of the predicted ninety-five transits, only twenty-four are May transits and the other seventy-one are November transits. I.e. 34%. Regarding the height differences between the different transits, similar transit circumstances recur once every 217 years.
|PREVIOUS MERCURY TRANSITS|
|09 May 1970||22:16||08:16||114|
|10 Nov 1973||00:32||10:32||026|
|13 Nov 1986||18:07*||04:07||471|
|06 Nov 1993||19:57*||03:57||927|
|13 Nov 1986||18:07*||04:07||471|
|06 Nov 1993||19:57*||03:57||927|
|15 Nov 1999||11:41||21:41||963|
|07 May 2003||17:52*||07:52||708|
|09 Nov 2006||07:41||21:41||423|
|FUTURE MERCURY TRANSITS|
|10 May 2016||00:57||16:57||319|
|12 Nov 2019||01:20||15:20||076|
|13 Nov 2032||18:54*||08:54||572|
|07 Nov 2039||20:46||10:46||822|
|08 May 2049||00:24||14:24||512|
|09 Nov 2052||14:30*||02:30||319|
|10 May 2062||11:37||21:37||521|
|11 Nov 2065||10:07||20:07||181|
|14 Nov 2078||03:42||13:42||674|
|07 Nov 2085||03:36||13:36||718>|
|08 May 2095||11:08||21:08||310|
|10 Nov 2098||21:18*||07:18||215|
|* Previous Day|
According to the useful table produced by Fred Espenak, the longest Mercury transit last occurred on 15th May 1707 with the long duration of 07 hours 56 minutes — passing within 64.5 arcsec of the observed centre of the Sun. One of the next lengthy transit lasting above 07 hours will happen on 09th May 2016, but is totally invisible from Australasia. Shortest of these previous transits during in this period occurred in 11th May 1937 and transited in only thirteen short minutes.
Jean Meeus has calculated the shortest Mercury transit time in the future within the same time frame of 1600 AD to 2300 AD will occur on 18th November 2216AD. This transit is only partial and of short duration of only be about twenty minutes. Only contacts I and IV will occur! Widest of all the transits in this periods occurs in 12 November 2190 AD and will crosses only 9 arcsec from the centre of the Sun. This latter event shall also be one of the longest of any of the May transits in this 700-year period — taking fractionally over nine hours to complete the entire transit.
The user applying this data for any purpose forgoes any liability against the author. None of the information should be used for regarding either legal or medical purposes. Although the data is accurate as possible some errors might be present. The onus of its use is placed solely with the user.
Last Update : 1st December 2012
Southern Astronomical Delights © (2012)