A transit of Mercury across the Sun takes place when the planet Mercury passes directly between the Sun and a superior planet. During a transit, Mercury appears as a tiny black dot moving across the Sun as the planet obscures a small portion of the solar disk. Because of orbital alignments, transits viewed from Earth occur in May or November. The last four such transits occurred on May 7, 2003; November 8, 2006; May 9, 2016; and November 11, 2019. The next will occur on November 13, 2032. A typical transit lasts several hours. Mercury transits are much more frequent than transits of Venus, with about 13 or 14 per century, primarily because Mercury is closer to the Sun and orbits it more rapidly.
On June 3, 2014, the Mars rover Curiosity observed the planet Mercury transiting the Sun, marking the first time a planetary transit has been observed from a celestial body besides Earth. [1]
The orbit of the planet Mercury lies interior to that of the Earth, and thus it can come into an inferior conjunction with the Sun. When Mercury is near the node of its orbit, it passes through the orbital plane of the Earth. If an inferior conjunction occurs as Mercury is passing through its orbital node, the planet can be seen to pass across the disk of the Sun in an event called a transit. Depending on the chord of the transit and the position of the planet Mercury in its orbit, the maximum length of this event is 7h 50m. [2]
Transit events are useful for studying the planet and its orbit. Examples of the scientific investigations based on transits of Mercury are:
Transits of Mercury can only occur when the Earth is aligned with a node of Mercury's orbit. Currently that alignment occurs within a few days of May 8 (descending node) and November 10 (ascending node), with the angular diameter of Mercury being about 12″ for May transits, and 10″ for November transits. The average date for a transit increases over centuries as a result of Mercury's nodal precession and Earth's axial precession.
Transits of Mercury occur on a regular basis. As explained in 1882 by Newcomb, [8] : 477–487 the interval between passages of Mercury through the ascending node of its orbit is 87.969 days, and the interval between the Earth's passage through that same longitude is 365.254 days. Using continued fraction approximations of the ratio of these values, it can be shown that Mercury will make an almost integral number of revolutions about the Sun over intervals of 6, 7, 13, 33, 46, and 217 years.
In 1894 Crommelin [15] noted that at these intervals, the successive paths of Mercury relative to the Sun are consistently displaced northwards or southwards. He noted the displacements as:
Interval | May transits | November transits |
---|---|---|
After 6 years | 65′ 37″ S | 31′ 35″ N |
After 7 years | 48′ 21″ N | 23′ 16″ S |
Hence after 13 years (6 + 7) | 17′ 16″ S | 8′ 19″ N |
... 20 years (6 + 2 × 7) | 31′ 05″ N | 14′ 57″ S |
... 33 years (2 × 6 + 3 × 7) | 13′ 49″ N | 6′ 38″ S |
... 46 years (3 × 13 + 7) | 3′ 27″ S | 1′ 41″ N |
... 217 years (14 × 13 + 5 × 7) | 0′ 17″ N | 0′ 14″ N |
Comparing these displacements with the solar diameter (about 31.7′ in May, and 32.4′ in November) the following may be deduced about the interval between transits:
Transits that occur 46 years apart can be grouped into a series. For November transits each series includes about 20 transits over 874 years, with the path of Mercury across the Sun passing further north than for the previous transit. For May transits each series includes about 10 transits over 414 years, with the path of Mercury across the Sun passing further south than for the previous transit. Some authors [16] have allocated a series number to transits on the basis of this 46-year grouping.
Similarly transits that occur 217 years apart can be grouped into a series. For November transits each series would include about 135 transits over 30,000 years. For May transits each series would include about 110 transits over 24,000 years. For both the May and November series, the path of Mercury across the Sun passes further north than for the previous transit. Series numbers have not been traditionally allocated on the basis of the 217 year grouping.
Predictions of transits of Mercury covering many years are available at NASA, [16] SOLEX, [17] and Fourmilab. [18]
At inferior conjunction, the planet Mercury subtends an angle of 12″ , which, during a transit, is too small to be seen without a telescope. [19] A common observation made at a transit [20] is recording the times when the disk of Mercury appears to be in contact with the limb of the Sun. [21] Those contacts are traditionally referred to as the 1st, 2nd, 3rd and 4th contacts – with the 2nd and 3rd contacts occurring when the disk of Mercury is fully on the disk of the sun. [22] As a general rule, 1st and 4th contacts cannot be accurately detected, [7] while 2nd and 3rd contacts are readily visible within the constraints of the Black Drop effect, [23] irradiation, atmospheric conditions, and the quality of the optics being used. [24]
Observed contact times for transits between 1677 and 1881 are given in S Newcomb's analysis of transits of Mercury. [8] : 367 Observed 2nd and 3rd contacts times for transits between 1677 and 1973 are given in Royal Greenwich Observatory Bulletin No.181, 359-420 (1975). [25]
This section needs additional citations for verification .(May 2024) |
Sometimes Mercury appears to only graze the Sun during a transit. There are two possible scenarios:
The possibility that, at mid-transit, Mercury is seen to be fully on the solar disk from some parts of the world, and completely miss the Sun as seen from other parts of the world cannot occur.[ citation needed ]
The first observation of a Mercury transit was observed on November 7, 1631 by Pierre Gassendi. He was surprised by the small size of the planet compared to the Sun. Johannes Kepler had predicted the occurrence of transits of Mercury and Venus in his ephemerides published in 1630. [30]
Images of the November 15, 1999 transit from the Transition Region and Coronal explorer (TRACE) satellite were on Astronomy Picture of the Day (APOD) on November 19. [31] Three APODs featured the May 9, 2016 transit. [32] [33] [34]
The Shuckburgh telescope of the Royal Observatory, Greenwich in London was used for the 1832 Mercury transit. [35] It was equipped with a micrometer by Dollond and was used for a report of the events as seen through the small refractor. [35] By observing the transit in combination with timing it and taking measures, a diameter for the planet was taken. [35] They also reported the peculiar effects that they compared to pressing a coin into the Sun. [35] The observer remarked:
I afterwards observed, that immediately around the planet there was a dusky tinge, making it appear as if, in a small degree sunk below the sun's surface.
— Royal Astronomical Society, Vol II, No. 13 [35]
For the 1907 Mercury transit, telescopes used at the Paris Observatory included: [36]
The telescopes were mobile and were placed on the terrace for the several observations. [36]
The table below includes all historical transits of Mercury from 1605 on:
Past transits of Mercury [16] | |||||
---|---|---|---|---|---|
Date of mid-transit | Time (UTC) | Notes | |||
Start | Mid | End | |||
1605 Nov 1 | 18:47 | 20:02 | 21:18 | ||
1615 May 3 | 06:44 | 10:09 | 13:33 | ||
1618 Nov 4 | 11:10 | 13:42 | 16:14 | ||
1628 May 5 | 14:23 | 17:32 | 20:40 | ||
1631 Nov 7 | 04:39 | 07:20 | 10:01 | Observed by Pierre Gassendi. | |
1644 Nov 9 | 22:55 | 00:57 | 02:58 | ||
1651 Nov 3–4 | 23:09 | 00:52 | 02:35 | Observed by Jeremy Shakerly in Surat, reported in letter to Henry Osbourne, January 1652. Shakerly is thought to have died in India around 1655. [37] | |
1661 May 3 | 13:08 | 16:54 | 20:40 | Occurred on the day of the coronation of King Charles II of England. Observed by Christiaan Huygens, Nicholas Mercator, and Thomas Streete in Long Acre, London. [38] | |
1664 Nov 4 | 15:54 | 18:32 | 21:10 | ||
1674 May 7 | 22:01 | 00:16 | 02:31 | ||
1677 Nov 7 | 09:33 | 12:11 | 14:48 | Observed by Edmund Halley in St Helena and Richard Towneley in Lancashire to determine solar parallax, also noted by Jean Charles Gallet in Avignon; as reported in a letter from John Flamsteed to Johannes Hevelius May 23, 1678. [39] | |
1690 Nov 10 | 03:59 | 05:43 | 07:27 | ||
1697 Nov 3 | 03:40 | 05:42 | 07:43 | ||
1707 May 5 | 19:37 | 23:32 | 03:27 | Observed by Abraham Sharp. [40] [16] | |
1710 Nov 6 | 20:40 | 23:22 | 02:03 | ||
1723 Nov 9 | 14:27 | 16:59 | 19:30 | ||
1736 Nov 11 | 09:11 | 10:30 | 11:49 | ||
1740 May 2 | 21:42 | 23:02 | 00:21 | ||
1743 Nov 5 | 08:15 | 10:30 | 12:45 | ||
1753 May 6 | 02:19 | 06:13 | 10:06 | Coordinated scientific observations were organized by Joseph-Nicolas Delisle worldwide. [41] | |
1756 Nov 7 | 01:28 | 04:10 | 06:54 | ||
1769 Nov 9–10 | 19:23 | 21:46 | 00:10 | Observed by Charles Green and James Cook from Mercury Bay in New Zealand. [42] Noted that Mercury had little or no atmosphere. | |
1776 Nov 2 | 21:03 | 21:36 | 22:09 | ||
1782 Nov 12 | 14:42 | 15:16 | 15:50 | Observed from Cambridge U.K. [43] [16] | |
1786 May 4 | 03:01 | 05:41 | 08:21 | ||
1789 Nov 5 | 12:53 | 15:19 | 17:44 | ||
1799 May 7 | 09:10 | 12:50 | 16:31 | Observed by Capel Lofft in England. [44] | |
1802 Nov 9 | 06:16 | 08:58 | 11:41 | Observed by William Herschel and Capel Lofft in England. [45] [46] | |
1815 Nov 12 | 00:20 | 02:33 | 04:46 | ||
1822 Nov 5 | 01:04 | 02:25 | 03:45 | ||
1832 May 5 | 09:04 | 12:25 | 15:47 | ||
1835 Nov 7 | 17:35 | 20:08 | 22:41 | ||
1845 May 8 | 16:24 | 19:37 | 22:49 | Observed by William Lassell. [47] | |
1848 Nov 9 | 11:07 | 13:48 | 16:28 | ||
1861 Nov 12 | 05:21 | 07:19 | 09:18 | Partially observed from Malta by William Lassell. [48] | |
1868 Nov 5 | 05:28 | 07:14 | 09:00 | ||
1878 May 6 | 15:16 | 19:00 | 22:44 | Observed from Greenwich Observatory. [49] | |
1881 Nov 6–7 | 22:19 | 00:57 | 03:36 | Observed by John Tebbutt. [50] | |
1891 May 8–9 | 23:57 | 02:22 | 04:47 | ||
1894 Nov 10 | 15:58 | 18:35 | 21:11 | Observed from Sidmouth, Devon by H.H. Turner and A. F. Lindemann [51] | |
1907 Nov 14 | 10:24 | 12:07 | 13:50 | Observed from Johannesburg by R. T. A. Innes [52] | |
1914 Nov 7 | 09:57 | 12:03 | 14:09 | Seen by several observers across the U.K. including A. Grace Cook and T. E. R. Phillips. [53] | |
1924 May 8–9 | 21:44 | 01:41 | 05:38 | Final stages observed by Basil Brown. [54] | |
1927 Nov 10 | 03:02 | 05:46 | 08:29 | Final stages observed from the U.K. [55] | |
1937 May 11 | 08:53 | 08:59 | 09:06 | Only visible as partial transit in Southern Africa, Southern Arabia, South Asia, and Western Australia. [56] | |
1940 Nov 11–12 | 20:49 | 23:21 | 01:53 | Observed from New South Wales. [57] | |
1953 Nov 14 | 15:37 | 16:54 | 18:11 | Observed from the Royal Observatory at the Cape of Good Hope. [58] | |
1957 May 5–6 | 23:59 | 01:14 | 02:30 | ||
1960 Nov 7 | 14:34 | 16:53 | 19:12 | [59] | |
1970 May 9 | 04:19 | 08:16 | 12:13 | [60] | |
1973 Nov 10 | 07:47 | 10:32 | 13:17 | [61] | |
1986 Nov 13 | 01:43 | 04:07 | 06:31 | [62] | |
1993 Nov 6 | 03:06 | 03:57 | 04:47 | [63] This brief transit was only visible from the south pole. [64] | |
1999 Nov 15 | 21:15 | 21:41 | 22:07 | [65] Partial transit in Australia, Antarctica, and New Zealand's South Island. | |
2003 May 7 | 05:13 | 07:52 | 10:32 | [66] | |
2006 Nov 8 | 18:12 | 20:41 | 23:10 | [67] | |
2016 May 9 | 11:12 | 14:57 | 18:42 | Entire transit in S. America, eastern N. America, western Europe; part of transit everywhere else except Australia and far eastern Asia. [68] | |
2019 Nov 11 | 12:35 | 15:20 | 18:04 | [16] | |
Future transits of Mercury [16] | |||||
Date of mid-transit | Time (UTC) | Notes | |||
Start | Mid | End | |||
2032 Nov 13 | 06:41 | 08:54 | 11:07 | ||
2039 Nov 7 | 07:17 | 08:46 | 10:15 | ||
2049 May 7 | 11:03 | 14:24 | 17:44 | ||
2052 Nov 8–9 | 22:53 | 01:29 | 04:06 | ||
2062 May 10–11 | 18:16 | 21:36 | 01:00 | ||
2065 Nov 11–12 | 17:24 | 20:06 | 22:48 | ||
2078 Nov 14 | 11:42 | 13:41 | 15:39 | ||
2085 Nov 7 | 11:42 | 13:34 | 15:26 | ||
2095 May 8–9 | 17:20 | 21:05 | 00:50 | ||
2098 Nov 10 | 04:35 | 07:16 | 09:57 | ||
2108 May 12 | 01:40 | 04:16 | 06:52 | ||
2111 Nov 14–15 | 22:15 | 00:53 | 03:30 | ||
2124 Nov 15 | 16:49 | 18:28 | 20:07 |
The Solar System is the gravitationally bound system of the Sun and the objects that orbit it. It was formed 4.6 billion years ago when a dense region of a molecular cloud collapsed, forming the Sun and a protoplanetary disc. The Sun is an ordinary main sequence star that maintains a balanced equilibrium by the fusion of hydrogen into helium at its core, releasing this energy from its outer photosphere.
Vulcan was a theorized planet that some pre-20th century astronomers thought existed in an orbit between Mercury and the Sun. Speculation about, and even purported observations of, intermercurial bodies or planets date back to the beginning of the 17th century. The case for their probable existence was bolstered by the support of the French mathematician Urbain Le Verrier, who had predicted the existence of Neptune using disturbances in the orbit of Uranus. By 1859 he had confirmed unexplained peculiarities in Mercury's orbit and predicted that they had to be the result of the gravitational influence of another unknown nearby planet or series of asteroids. A French amateur astronomer's report that he had observed an object passing in front of the Sun that same year led Le Verrier to announce that the long sought after planet, which he gave the name Vulcan, had been discovered at last.
In astronomy, a conjunction occurs when two astronomical objects or spacecraft appear to be close to each other in the sky. This means they have either the same right ascension or the same ecliptic longitude, usually as observed from Earth.
In astronomy, axial tilt, also known as obliquity, is the angle between an object's rotational axis and its orbital axis, which is the line perpendicular to its orbital plane; equivalently, it is the angle between its equatorial plane and orbital plane. It differs from orbital inclination.
In astronomy, a transit is the passage of a celestial body directly between a larger body and the observer. As viewed from a particular vantage point, the transiting body appears to move across the face of the larger body, covering a small portion of it.
Astronomical symbols are abstract pictorial symbols used to represent astronomical objects, theoretical constructs and observational events in European astronomy. The earliest forms of these symbols appear in Greek papyrus texts of late antiquity. The Byzantine codices in which many Greek papyrus texts were preserved continued and extended the inventory of astronomical symbols. New symbols have been invented to represent many planets and minor planets discovered in the 18th to the 21st centuries.
A synodic day is the period for a celestial object to rotate once in relation to the star it is orbiting, and is the basis of solar time.
A transit of Venus takes place when Venus passes directly between the Sun and the Earth, becoming visible against the solar disk. During a transit, Venus can be seen as a small black circle moving across the face of the Sun.
Atira asteroids or Apohele asteroids, also known as interior-Earth objects (IEOs), are Near-Earth objects whose orbits are entirely confined within Earth's orbit; that is, their orbit has an aphelion smaller than Earth's perihelion, which is 0.983 astronomical units (AU). Atira asteroids are by far the least numerous group of near-Earth objects, compared to the more populous Aten, Apollo and Amor asteroids.
Beta Pictoris is the second brightest star in the constellation Pictor. It is located 63.4 light-years (19.4 pc) from the Solar System, and is 1.75 times as massive and 8.7 times as luminous as the Sun. The Beta Pictoris system is very young, only 20 to 26 million years old, although it is already in the main sequence stage of its evolution. Beta Pictoris is the title member of the Beta Pictoris moving group, an association of young stars which share the same motion through space and have the same age.
A transit of Mercury across the Sun as seen from Mars takes place when the planet Mercury passes directly between the Sun and Mars, obscuring a small part of the Sun's disc for an observer on Mars. During a transit, Mercury can be seen from Mars as a small black disc moving across the face of the Sun.
The Astronomical Almanac is an almanac published by the United Kingdom Hydrographic Office; it also includes data supplied by many scientists from around the world. On page vii, the listed major contributors to its various Sections are: H.M Nautical Almanac Office, United Kingdom Hydrographic Office; the Nautical Almanac Office, United States Naval Observatory; the Jet Propulsion Laboratory, California Institute of Technology; the IAU Standards Of Fundamental Astronomy (SOFA) initiative; the Institut de Mécanique Céleste et des Calcul des Éphémerides, Paris Observatory; and the Minor Planet Center, Cambridge, Massachusetts. It is considered a worldwide resource for fundamental astronomical data, often being the first publication to incorporate new International Astronomical Union resolutions. The almanac largely contains Solar System ephemerides based on the JPL Solar System integration "DE440", and catalogs of selected stellar and extragalactic objects. The material appears in sections, each section addressing a specific astronomical category. The book also includes references to the material, explanations, and examples. It used to be available up to one year in advance of its date, however the current 2024 edition became available only one month in advance; in December 2023.
Edwin Dunkin FRS, FRAS was a British astronomer and the president of the Royal Astronomical Society and the Royal Institution of Cornwall.
Discovery and exploration of the Solar System is observation, visitation, and increase in knowledge and understanding of Earth's "cosmic neighborhood". This includes the Sun, Earth and the Moon, the major planets Mercury, Venus, Mars, Jupiter, Saturn, Uranus, and Neptune, their satellites, as well as smaller bodies including comets, asteroids, and dust.
Kepler-9 is a sunlike star in the constellation Lyra. Its planetary system, discovered by the Kepler Mission in 2010 was the first detected with the transit method found to contain multiple planets.
In astronomy, a syzygy is a roughly straight-line configuration of three or more celestial bodies in a gravitational system.
A fundamental ephemeris of the Solar System is a model of the objects of the system in space, with all of their positions and motions accurately represented. It is intended to be a high-precision primary reference for prediction and observation of those positions and motions, and which provides a basis for further refinement of the model. It is generally not intended to cover the entire life of the Solar System; usually a short-duration time span, perhaps a few centuries, is represented to high accuracy. Some long ephemerides cover several millennia to medium accuracy.
An exocomet, or extrasolar comet, is a comet outside the Solar System, which includes rogue comets and comets that orbit stars other than the Sun. The first exocomets were detected in 1987 around Beta Pictoris, a very young A-type main-sequence star. There are now a total of 27 stars around which exocomets have been observed or suspected.
In astronomy, planetary transits and occultations occur when a planet passes in front of another object, as seen by an observer. The occulted object may be a distant star, but in rare cases it may be another planet, in which case the event is called a mutual planetary occultation or mutual planetary transit, depending on the relative apparent diameters of the objects.