Transit of Venus
A transit of Venus across the Sun takes place when the planet Venus passes directly between the Sun and Earth (or another planet), becoming visible against (and hence obscuring a small portion of) the solar disk. During a transit, Venus can be seen from Earth as a small black disk moving across the face of the Sun. The duration of such transits is usually measured in hours (the transit of 2012 lasted 6 hours and 40 minutes). A transit is similar to a solar eclipse by the Moon. While the diameter of Venus is more than 3 times that of the Moon, Venus appears smaller, and travels more slowly across the face of the Sun, because it is much farther away from Earth.
Transits of Venus are among the rarest of predictable astronomical phenomena. They occur in a pattern that generally repeats every 243 years, with pairs of transits eight years apart separated by long gaps of 121.5 years and 105.5 years. The periodicity is a reflection of the fact that the orbital periods of Earth and Venus are close to 8:13 and 243:395 commensurabilities.
The last transit of Venus was on 5 and 6 June 2012, and was the last Venus transit of the 21st century; the prior transit took place on 8 June 2004. The previous pair of transits were in December 1874 and December 1882. The next transits of Venus will be 10–11 December 2117, and in December 2125.
Venus transits are historically of great scientific importance as they were used to gain the first realistic estimates of the size of the Solar System. Observations of the 1639 transit, combined with the principle of parallax, provided an estimate of the distance between the Sun and the Earth that was more accurate than any other up to that time. The 2012 transit provided scientists with a number of other research opportunities, particularly in the refinement of techniques to be used in the search for exoplanets.
Venus, with an orbit inclined by 3.4° relative to the Earth's, usually appears to pass under (or over) the Sun at inferior conjunction. A transit occurs when Venus reaches conjunction with the Sun at or near one of its nodes—the longitude where Venus passes through the Earth's orbital plane (the ecliptic)—and appears to pass directly across the Sun. Although the inclination between these two orbital planes is only 3.4°, Venus can be as far as 9.6° from the Sun when viewed from the Earth at inferior conjunction. Since the angular diameter of the Sun is about half a degree, Venus may appear to pass above or below the Sun by more than 18 solar diameters during an ordinary conjunction.
Sequences of transits usually repeat every 243 years. After this period of time Venus and Earth have returned to very nearly the same point in their respective orbits. During the Earth's 243 sidereal orbital periods, which total 88757.3 days, Venus completes 395 sidereal orbital periods of 224.701 days each, equal to 88756.9 Earth days. This period of time corresponds to 152 synodic periods of Venus.
The pattern of 105.5, 8, 121.5 and 8 years is not the only pattern that is possible within the 243-year cycle, because of the slight mismatch between the times when the Earth and Venus arrive at the point of conjunction. Prior to 1518, the pattern of transits was 8, 113.5 and 121.5 years, and the eight inter-transit gaps before the 546 CE transit were 121.5 years apart. The current pattern will continue until 2846, when it will be replaced by a pattern of 105.5, 129.5 and 8 years. Thus, the 243-year cycle is relatively stable, but the number of transits and their timing within the cycle will vary over time. Since the 243:395 Earth:Venus commensurability is only approximate, there are different sequences of transits occurring 243 years apart, each extending for several thousand years, which are eventually replaced by other sequences. For instance, there is a series which ended in 541 BCE, and the series which includes 2117 only started in 1631 AD.
Ancient history 
Ancient Indian, Greek, Egyptian, Babylonian, Mayan, and Chinese observers knew of Venus and recorded the planet's motions. The early Greek astronomers called Venus by two names—Hesperus the evening star and Phosphorus the morning star. Pythagoras is credited with realizing they were the same planet. There is no evidence that any of these cultures knew of the transits. Venus was important to ancient American civilizations, in particular for the Maya, who called it Noh Ek, "the Great Star" or Xux Ek, "the Wasp Star"; they embodied Venus in the form of the god Kukulkán (also known as or related to Gukumatz and Quetzalcoatl in other parts of Mexico). In the Dresden Codex, the Maya charted Venus' full cycle, but despite their precise knowledge of its course, there is no mention of a transit.
Modern observations 
Aside from its rarity, the original scientific interest in observing a transit of Venus was that it could be used to determine the distance from the Earth to the Sun, and from this the size of the Solar System, by employing the parallax method and Kepler's third law. The technique involved making precise observations of the different durations of the transit when viewed from widely separated points on the Earth's surface. The distance between the points on the Earth was then used as a baseline to calculate the distance to Venus and the Sun via triangulation.
Although by the 17th century astronomers could calculate each planet's relative distance from the Sun in terms of the distance of the Earth from the Sun (an astronomical unit), an accurate absolute value of this distance had not been determined. In 1627, Johannes Kepler became the first person to predict a transit of Venus, by predicting the 1631 event. His methods were not sufficiently accurate to predict that the transit would not be visible in most of Europe, and as a consequence, nobody was able to use his prediction to observe the phenomenon.
1639 – first scientific observation 
The first recorded observation of a transit of Venus was made by Jeremiah Horrocks from his home at Carr House in Much Hoole, near Preston in England, on 4 December 1639 (24 November under the Julian calendar then in use in England). His friend, William Crabtree, also observed this transit from Broughton, near Manchester. Kepler had predicted transits in 1631 and 1761 and a near miss in 1639. Horrocks corrected Kepler's calculation for the orbit of Venus, realized that transits of Venus would occur in pairs 8 years apart, and so predicted the transit in 1639. Although he was uncertain of the exact time, he calculated that the transit was to begin at approximately 3:00 pm. Horrocks focused the image of the Sun through a simple telescope onto a piece of paper, where the image could be safely observed. After observing for most of the day, he was lucky to see the transit as clouds obscuring the Sun cleared at about 3:15 pm, just half an hour before sunset. Horrocks' observations allowed him to make a well-informed guess as to the size of Venus, as well as to make an estimate of the distance between the Earth and the Sun. He estimated that distance to be 59.4 million miles (95.6 Gm, 0.639 AU) – about two thirds of the actual distance of 93 million miles (149.6 million km), but a more accurate figure than any suggested up to that time. The observations were not published until 1661, well after Horrocks' death.
1761 and 1769 
In 1663 Scottish mathematician James Gregory had suggested in his Optica Promota that observations of a transit of the planet Mercury, at widely spaced points on the surface of the Earth, could be used to calculate the solar parallax and hence the astronomical unit. Aware of this, a young Edmond Halley made observations of such a transit in 1676 from Saint Helena, but was disappointed to find that there had been only one other observation of the event and was not satisfied that the resulting calculation of the solar parallax at 45" was accurate. In a paper published in 1691, and a more refined one in 1716, he proposed that more accurate calculations could be made using measurements of a transit of Venus, although the next such event was not due until 1761. Halley died in 1742, but in 1761 numerous expeditions were made to various parts of the world so that precise observations of the transit could be made in order to make the calculations as described by Halley—an early example of international scientific collaboration. In an attempt to observe the first transit of the pair, scientists and explorers from Britain, Austria and France travelled to destinations around the world, including Siberia, Norway, Newfoundland and Madagascar. Most managed to observe at least part of the transit, but successful observations were made in particular by Jeremiah Dixon and Charles Mason at the Cape of Good Hope.
The existence of an atmosphere on Venus was concluded by Mikhail Lomonosov on the basis of his observation of the transit of Venus of 1761 from the Saint Petersburg. He used a two-lens achromat refractor and a weak solar filter (smoked glass) and reported seeing a bump or bulge of light ("Lomonosov's arc") off the solar disc as Venus began to exit the Sun. Lomonosov attributed that effect to refraction of solar rays through an atmosphere; he also reported the appearance of a sliver around the part of Venus that had just entered the Sun's disk during the initial phase of transit. In 2012, Pasachoff and Sheehan reported, based on knowing what Venus's atmosphere would look like because of Pasachoff and Schneider's observations of the 2004 transit of Venus, that what Lomonosov reported was not Venus's atmosphere. To make a decisive test, a group of researchers carried out experimental reconstruction of Lomonosov's discovery of Venusian atmosphere with antique refractors during the transit of Venus on 5–6 June 2012. They observed the "Lomonosov's arc" and other aureole effects due to Venus's atmosphere and concluded that Lomonosov's telescope was fully adequate to the task of detecting the arc of light around Venus off the Sun's disc during ingress or egress if proper experimental techniques as described by Lomonosov in his 1761 paper are employed.
For the 1769 transit, scientists traveled to Canada, San José del Cabo (Baja California, then under Spanish control), Tahiti, and Norway. The Czech astronomer Christian Mayer was invited by Catherine the Great to observe the transit in Saint Petersburg with Anders Johan Lexell, while other members of Russian Academy of Sciences went to eight other locations in the Russian Empire. The Hungarian astronomer Maximilian Hell and his assistant János Sajnovics traveled to Vardø, Norway, delegated by Christian VII of Denmark. William Wales and Joseph Dymond made their observation in Hudson Bay, Canada, for the Royal Society. In Philadelphia, the American Philosophical Society erected three temporary observatories and appointed a committee, of which David Rittenhouse was the head. The results of these observations were printed in the first volume of the Society's Transactions, published in 1771.
The unfortunate Guillaume Le Gentil spent eight years travelling in an attempt to observe either of the transits. His unsuccessful journey led to him losing his wife and possessions and being declared dead (his efforts became the basis of the play Transit of Venus by Maureen Hunter). Under the influence of the Royal Society Ruđer Bošković travelled to Istanbul, but arrived too late.
Unfortunately, it was impossible to time the exact moment of the start and end of the transit because of the phenomenon known as the "black drop effect". This effect was long thought to be due to Venus' thick atmosphere, and initially it was held to be the first real evidence that Venus had an atmosphere. However, recent studies demonstrate that it is an optical effect caused by the smearing of the image of Venus by turbulence in the Earth's atmosphere or imperfections in the viewing apparatus.
In 1771, using the combined 1761 and 1769 transit data, the French astronomer Jérôme Lalande calculated the astronomical unit to have a value of 153 million kilometers (±1 million km). The precision was less than had been hoped for because of the black drop effect, but still a considerable improvement on Horrocks' calculations.
Maximilian Hell published the results of his expedition in 1770, in Copenhagen. Based on the results of his own expedition, and of Wales and Cook, in 1772 he presented another calculation of the astronomical unit: 151.7 million kilometers. Lalande queried the accuracy and authenticity of the Hell expedition, but later he retreated in an article of Journal des sçavans, in 1778.
1874 and 1882 
Transit observations in 1874 and 1882 allowed this value to be refined further. Several expeditions were sent to the Kerguelen Archipelago for the 1874 observations. The American astronomer Simon Newcomb combined the data from the last four transits, and he arrived at a value of about 149.59 million kilometers (±0.31 million kilometers). Modern techniques, such as the use of radio telemetry from space probes, and of radar measurements of the distances to planets and asteroids in the Solar System, have allowed a reasonably accurate value for the astronomical unit (AU) to be calculated to a precision of about ±30 meters. As a result, the need for parallax calculations has been superseded.
2004 and 2012 
A number of scientific organizations headed by the European Southern Observatory (ESO) organized a network of amateur astronomers and students to measure Earth's distance from the Sun during the transit. The participants' observations allowed a calculation of the astronomical unit (AU) of 149 608 708 km ± 11 835 km which had only a 0.007% difference to the accepted value. 
There was a good deal of interest in the 2004 transit as scientists attempted to measure the pattern of light dimming as Venus blocked out some of the Sun's light, in order to refine techniques that they hope to use in searching for extrasolar planets. Current methods of looking for planets orbiting other stars only work for a few cases: planets that are very large (Jupiter-like, not Earth-like), whose gravity is strong enough to wobble the star sufficiently for us to detect changes in proper motion or Doppler shift changes in radial velocity; Jupiter or Neptune sized planets very close to their parent star whose transit causes changes in the luminosity of the star; or planets which pass in front of background stars with the planet-parent star separation comparable to the Einstein ring and cause gravitational microlensing. Measuring light intensity during the course of a transit, as the planet blocks out some of the light, is potentially much more sensitive, and might be used to find smaller planets. However, extremely precise measurement is needed: for example, the transit of Venus causes the Sun's light to drop by a mere 0.001 magnitude, and the dimming produced by small extrasolar planets will be similarly tiny.
- Measuring dips in a star's brightness caused by a known planet transiting the Sun will help astronomers find exoplanets. Unlike the 2004 Venus transit, the 2012 transit occurred during an active phase of the 11-year activity cycle of the Sun, and it is likely to give astronomers practice in picking up a planet's signal around a "spotty" variable star.
- Measurements made of the apparent diameter of Venus during the transit, and comparison with its known diameter, will give scientists an idea of how to estimate exoplanet sizes.
- Observation made of the atmosphere of Venus simultaneously from Earth-based telescopes and from the Venus Express gives scientists a better opportunity to understand the intermediate level of Venus' atmosphere than is possible from either viewpoint alone. This will provide new information about the climate of the planet.
- Spectrographic data taken of the well-known atmosphere of Venus will be compared to studies of exoplanets whose atmospheres are thus far unknown.
- The Hubble Space Telescope, which cannot be pointed directly at the Sun, used the Moon as a mirror to study the light that had passed through the atmosphere of Venus in order to determine its composition. This will help to show whether a similar technique could be used to study exoplanets.
Past and future transits 
- For a complete list see NASA's Six Millennium Catalog of Venus Transits: 2000 BCE to 4000 CE
Currently, transits occur only in June or December (see table) and the occurrence of these events slowly drifts becoming later in the year by about two days every 243-year cycle. Transits usually occur in pairs, on nearly the same date eight years apart. This is because the length of eight Earth years is almost the same as 13 years on Venus, so every eight years the planets are in roughly the same relative positions. This approximate conjunction usually results in a pair of transits, but it is not precise enough to produce a triplet, since Venus arrives 22 hours earlier each time. The last transit not to be part of a pair was in 1396. The next will be in 3089; in 2854 (the second of the 2846/2854 pair), although Venus will just miss the Sun as seen from the Earth's equator, a partial transit will be visible from some parts of the southern hemisphere.
|Past transits of Venus|
|Time (UTC)||Notes||Transit path
|23 November 1396||15:45||19:27||23:09||Last transit not part of a pair.|||
|25–26 May 1518||22:46
|23 May 1526||16:12||19:35||21:48||Last transit before invention of telescope|||
|7 December 1631||03:51||05:19||06:47||Predicted by Kepler|||
|4 December 1639||14:57||18:25||21:54||First transit observed by Horrocks and Crabtree|||
|6 June 1761||02:02||05:19||08:37||Lomonosov, Chappe d'Auteroche and others observe from Russia; Mason and Dixon observe from the Cape of Good Hope.|||
|3–4 June 1769||19:15
|Cook sent to Tahiti to observe the transit|||
|9 December 1874||01:49||04:07||06:26||Pietro Tacchini leads expedition to Muddapur, India. A French expedition goes to New Zealand's Campbell Island and a British expedition travels to Hawaii.|||
|6 December 1882||13:57||17:06||20:15||John Philip Sousa composes a march, the "Transit of Venus", in honor of the transit.|||
|8 June 2004||05:13||08:20||11:26||Various media networks globally broadcast live video of the Venus transit.|||
|5–6 June 2012||22:09
|Visible in its entirety from the Pacific and Eastern Asia, with the beginning of the transit visible from North America and the end visible from Europe. First transit while a spacecraft orbits Venus.|||
|Future transits of Venus|
|Time (UTC)||Notes||Transit path
|10–11 December 2117||23:58
|Visible in entirety in eastern China, Japan, Taiwan, Indonesia, and Australia. Partly visible on extreme U.S. West Coast, and in India, most of Africa, and the Middle East.|||
|8 December 2125||13:15||16:01||18:48||Visible in entirety in South America and the eastern U.S. Partly visible in Western U.S., Europe, and Africa.|||
|11 June 2247||08:42||11:33||14:25||Visible in entirety in Africa, Europe, and the Middle East. Partly visible in East Asia and Indonesia, and in North and South America.|||
|9 June 2255||01:08||04:38||08:08||Visible in entirety in Russia, India, China, and western Australia. Partly visible in Africa, Europe, and the western U.S.|||
|12–13 December 2360||22:32
|Visible in entirety in Australia and most of Indonesia. Partly visible in Asia, Africa, and the western half of the Americas.|||
|10 December 2368||12:29||14:45||17:01||Visible in entirety in South America, western Africa, and the U.S. East Coast. Partly visible in Europe, the western U.S., and the Middle East.|||
|12 June 2490||11:39||14:17||16:55||Visible in entirety through most of the Americas, western Africa, and Europe. Partly visible in eastern Africa, the Middle East, and Asia.|||
|10 June 2498||03:48||07:25||11:02||Visible in entirety through most of Europe, Asia, the Middle East, and eastern Africa. Partly visible in eastern Americas, Indonesia, and Australia.|||
Over longer periods of time, new series of transits will start and old series will end. Unlike the saros series for lunar eclipses, it is possible for a transit series to restart after a hiatus. The transit series also vary much more in length than the saros series.
Grazing and simultaneous transits 
Sometimes Venus only grazes the Sun during a transit. In this case it is possible that in some areas of the Earth a full transit can be seen while in other regions there is only a partial transit (no second or third contact). The last transit of this type was on 6 December 1631, and the next such transit will occur on 13 December 2611. It is also possible that a transit of Venus can be seen in some parts of the world as a partial transit, while in others Venus misses the Sun. Such a transit last occurred on 19 November 541 BCE, and the next transit of this type will occur on 14 December 2854. These effects occur due to parallax, since the size of the Earth affords different points of view with slightly different lines of sight to Venus and the Sun. It can be demonstrated by closing an eye and holding a finger in front of a smaller more distant object; when you open the other eye and close the first, the finger will no longer be in front of the object.
The simultaneous occurrence of a transit of Mercury and a transit of Venus does occur, but extremely infrequently. Such an event last occurred on 22 September 373,173 BCE and will next occur on 26 July 69,163, and again on 29 March 224,508. The simultaneous occurrence of a solar eclipse and a transit of Venus is currently possible, but very rare. The next solar eclipse occurring during a transit of Venus will be on 5 April 15,232. The last time a solar eclipse occurred during a transit of Venus was on 1 November 15,607 BCE. It could be noticed that the day after the Venerean transit of 3 June 1769 there was a total solar eclipse, which was visible in Northern America, Europe and Northern Asia.
See also 
- McClure, Bruce (29 May 2012). "Everything you need to know: Venus transit on June 5–6". EarthSky. Earthsky communications Inc. Retrieved 2 June 2012.
- Langford, Peter M. (September 1998). "Transits of Venus". La Société Guernesiaise Astronomy Section web site. Astronomical Society of the Channel Island of Guernsey. Retrieved 1 March 2012.
- Shortt, David (22 May 2012). "Some Details About Transits of Venus". Planetary Society web site. The Planetary Society. Retrieved 22 May 2012.
- Westfall, John E. (November 2003). "June 8, 2004: The Transit of Venus". Archived from the original on 8 August 2007. Retrieved 25 September 2006.
- Westfall, John E. "June 8, 2004: The Transit of Venus". alpo-astronomy.org. Retrieved 8 December 2009.
- Klotz, Irene (6 June 2012). "Venus transit offers opportunity to study planet's atmosphere (+video)". Christian Science Monitor. Retrieved 2012-06-06.
- "Venus compared to Earth". European Space Agency. 2000. Retrieved 25 September 2006.
- Giesen, Juergen (2003). "Transit Motion Applet". Retrieved 26 September 2006.
- Espenak, Fred (11 February 2004). "Transits of Venus, Six Millennium Catalog: 2000 BCE to 4000 CE". NASA. Archived from the original on 24 June 2011.
- Walker, John. "Transits of Venus from Earth". Fourmilab Switzerland. Retrieved 21 September 2006.
- Rincon, Paul (7 November 2005). "Planet Venus: Earth's 'evil twin'". BBC. Retrieved 25 September 2006.
- Morley, Sylvanus G. (1994). The Ancient Maya (5th ed.). Stanford University Press. ISBN 978-0-8047-2310-7.
- Böhm, Bohumil; Böhm, Vladimir. "The Dresden Codex – the Book of Mayan Astronomy". Retrieved 25 September 2006.
- Halley, Edmund (1716). "A New Method of Determining the Parallax of the Sun, or His Distance from the Earth". Philosophical Transactions XXIX: 454. Archived from the original on 24 June 2011.
- van Gent, Robert H. "Transit of Venus Bibliography". Retrieved 11 September 2009.
- Kollerstrom, Nicholas (2004). "William Crabtree's Venus transit observation". Proceedings IAU Colloquium No. 196, 2004. International Astronomical Union. Retrieved 10 May 2012.
- Marston, Paul (2004). Jeremiah Horrocks—young genius and first Venus transit observer. University of Central Lancashire. pp. 14–37.
- Teets, D.A. (2003). "Transits of Venus and the Astronomical Unit". Mathematics Magazine 76: 335–348. JSTOR 3654879.
- Leverington, David (2003). Babylon to Voyager and beyond: a history of planetary astronomy. Cambridge, UK: Cambridge University Press. pp. 140–142. ISBN 0-521-80840-5.
- Pogge, Prof. Richard. "Lecture 26: How far to the Sun? The Venus Transits of 1761 & 1769". Retrieved 25 September 2006.
- "Oxford Dictionary of National Biography: Jeremiah Dixon". Oxford University Press. Retrieved 22 February 2012.
- "V.Shiltsev, "Lomonosov's Discovery of Venus Atmosphere in 1761: English Translation of Original Publication with Commentaries" (2012)". Arxiv.org. Retrieved 2013-05-06.
- Marov, Mikhail Ya. (2004). "Mikhail Lomonosov and the discovery of the atmosphere of Venus during the 1761 transit". Proceedings of the International Astronomical Union (Cambridge University Press) 2004: 209–219. Bibcode:2005tvnv.conf..209M. doi:10.1017/S1743921305001390.
- Pasachoff, Jay; Sheehan, William (2012). "Lomonosov, the Discovery of Venus's Atmosphere, and Eighteenth-century Transits of Venus". Journal of Astronomical History and Heritage 15: 1. Bibcode:2012JAHH...15....3P.
- "A.Koukarine, et al, "Experimental Reconstruction of Lomonosov's Discovery of Venus's Atmosphere with Antique Refractors During the 2012 Transit of Venus" (2012)". Arxiv.org. 2012-08-27. Retrieved 2013-05-06.
- V.Shiltsev, I.Nesterenko, and R.Rosenfeld, "Replicating the discovery of Venus’s atmosphere", Physics Today, Feb.2013 / Volume 66, Issue 2, p.64 (2013) http://www.physicstoday.org/resource/1/phtoad/v66/i2/p64_s1
- "James Cook and the Transit of Venus". NASA Headline News: Science News. nasa.gov. Retrieved 6 June 2012.
- Mayer, Christian; Parsons, James (1764). "An Account of the Transit of Venus: In a Letter to Charles Morton, M. D. Secret. R. S. from Christian Mayer, S. J. Translated from the Latin by James Parsons, M. D". Philosophical Transactions of the Royal Society 54: 163. Bibcode:1764RSPT...54..163M. doi:10.1098/rstl.1764.0030.
- "American Philosophical Society ". Encyclopedia Americana. 1920.
- See, for example, Stanley, David (2004). Moon Handbooks South Pacific (8 ed.). Avalon Travel Publishing. p. 175. ISBN 978-1-56691-411-6.
- Rhys, Ernest, ed. (1999). The Voyages of Captain Cook. Wordsworth Editions Ltd. pp. 29–30. ISBN 1-84022-100-3.
- Ruđer Bošković, Giornale di un viaggio da Constantinopoli in Polonia, 1762
- "Explanation of the Black-Drop Effect at Transits of Mercury and the Forthcoming Transit of Venus". AAS. 4 January 2004. Archived from the original on 10 July 2006. Retrieved 21 September 2006.
- "Transits of Venus – Kiss of the goddess". The Economist. 27 May 2004. Retrieved 25 September 2006.
- R. P. Maximiliani Hell e S. J. – Observatio transitus Veneris ante discum Solis die 3. junii anno 1769. Wardoëhusii, auspiciis potentissimi ac clementissimi regis Daniae et Norvegiae, Christiani septimi, facta et societati reg. scientiarum Hafniensi die 24. Novembris 1769. Praelecta. Hafniae, typ. Orphanotrophii regii, excudit Gerhard Wiese Salicath, 82 p.
- Ephemerides astronomicae, anni 1773. Adjecta Collectione omnium observationum transitus Veneris ante discum Solis diei 3. Junii 1769. per orbem universum factorum, atque Appendice de parallaxi Solis ex observationibus tarnsitus Veneris anni 1769. Vindobonae, 1773, typ. Trattner, 311, 121 p.
- De parallaxi Solis ex obervationibus transitus Veneris anni 1769. Vindobonae, 1772, typ. J. Trattner, 116 p.
- European Southern Observatory. "The Venus Transit 2004". Retrieved 2012-06-06.
- European Southern Observatory. "Summing Up the Unique Venus Transit 2004 (VT-2004) Programme". Retrieved 2012-06-06.
- McKee, Maggie (6 June 2004). "Extrasolar planet hunters eye Venus transit". New Scientist. Retrieved 27 September 2006.
- Gould, A. et al. (10 June 2006). "Microlens OGLE-2005-BLG-169 Implies That Cool Neptune-like Planets Are Common". The Astrophysical Journal Letters (The American Astronomical Society) 644 (1): L37–L40. arXiv:astro-ph/0603276. Bibcode:2006ApJ...644L..37G. doi:10.1086/505421.
- Espenak, Fred (18 June 2002). "2004 and 2012 Transits of Venus". NASA. Retrieved 25 September 2006.
- Wall, Michael (16 May 2012). "Venus Transit On June 5 May Bring New Alien Planet Discoveries". space.com. TheHuffingtonPost.com, Inc. Retrieved 21 May 2012.
- "Counting down to the Transit of Venus – our nearest exoplanet test-lab", phys.org, 5 March 2012
- "The Venus Twilight Experiment: Refraction and scattering phenomena during the transit of Venus on June 5–6, 2012", venustex.oca.eu.
- Although transits occurred in May and November before 1631, this apparent jump in dates was due to the changeover from the Julian calendar to the Gregorian calendar on 15 October 1582
- Bell, Steve (2004). "Transits of Venus 1000 AD – 2700 AD". HM Nautical Almanac Office. Archived from the original on 7 September 2006. Retrieved 25 September 2006.
- "Hobby Q&A", Sky&Telescope, August 2004, p. 138
- Espenak, Fred (21 April 2005). "Transits of Mercury, Seven Century Catalog: 1601 CE to 2300 CE". NASA. Retrieved 27 September 2006.
- Jeliazkov, Jeliazko. "Simultaneous occurrence of solar eclipse and a transit". transit.savage-garden.org. Retrieved 11 August 2009.
- de La Lande, Jérôme; Messier, Charles (1769). "Observations of the Transit of Venus on 3 June 1769, and the Eclipse of the Sun on the Following Day, Made at Paris, and Other Places. Extracted from Letters Addressed from M. De la Lande, of the Royal Academy of Sciences at Paris, and F. R. S. to the Astronomer Royal; And from a Letter Addressed from M. Messier to Mr. Magalhaens". Philosophical Transactions (1683–1775) 59 (0): 374–377. Bibcode:1769RSPT...59..374D. doi:10.1098/rstl.1769.0050.
Further reading 
- Anderson, Mark (2012). The Day the World Discovered the Sun: An Extraordinary Story of Scientific Adventure and the Race to Track the Transit of Venus. Boston: Da Capo Press. ISBN 978-0-306-82038-0.
- Chauvin, Michael (2004). Hokuloa: The British 1874 Transit of Venus Expedition to Hawaii. Honolulu: Bishop Museum Press. ISBN 1-581-78023-0.
- Lomb, Nick (2011). Transit of Venus: 1631 to the Present. Sydney, Australia: NewSouth Publishing. ISBN 978-1-74223-269-0. OCLC 717231977.
- Maor, Eli (2000). Venus in Transit. Princeton: Princeton University Press. ISBN 0-691-11589-3.
- Maunder, Michael; Moore, Patrick (2000). Transit: When Planets Cross the Sun. London: Springer-Verlaf. ISBN 1-85233-621-8.
- Sellers, David (2001). The Transit of Venus: The Quest to Find the True Distance of the Sun. Leeds, UK: Magavelda Press. ISBN 0-9541013-0-8.
- Sheehan, William; Westfall, John (2004). The Transits of Venus. Amherst, New York: Prometheus Books. ISBN 1-59102-175-8.
- Simaan, Arkan (May 2004). "The transit of Venus across the Sun". Physics Education 39 (3): 247–251. doi:10.1088/0031-9120/39/3/001.
- Wulf, Andrea (2012). Chasing Venus: The Race to Measure the Heavens. New York: Knopf. ISBN 978-0-307-70017-9.
|Wikimedia Commons has media related to: Transit of Venus|
- Transit of Venus – Information
- Venus Transits: Measuring the Solar System
- Historical observations of the transit of Venus
- Edmond Halley's 1716 paper describing how transits could be used to measure the Sun's distance, translated from Latin.
- Chasing Venus: Observing the Transits of Venus, 1631–2004 (Smithsonian Libraries)
- Merrifield, Michael. "Venus Transit". Sixty Symbols. Brady Haran for the University of Nottingham.
- June 2012 transit
- 2012 Transit of Venus – International Astronomical Union
- National Solar Observatory – Transit of Venus June 5–6 2012
- 2012 Transit of Venus Live Webcast and chatroom with SEMS at UND live From Alaska