![]() Comet Seki photographed by Elizabeth Roemer on 18 October 1961 | |
Discovery | |
---|---|
Discovered by | Tsutomu Seki |
Discovery date | 10 October 1961 |
Designations | |
1961f 1961 VIII | |
Orbital characteristics [1] | |
Epoch | 12 November 1961 (JD 2437615.5) |
Observation arc | 75 days |
Number of observations | 15 |
Aphelion | 173 AU |
Perihelion | 0.681 AU |
Semi-major axis | 86.8 AU |
Eccentricity | 0.9921 |
Orbital period | ~810 years |
Inclination | 155.71° |
247.36° | |
Argument of periapsis | 126.59° |
Last perihelion | 10 October 1961 |
TJupiter | -0.871 |
Earth MOID | 0.084 AU |
Jupiter MOID | 0.490 AU |
Physical characteristics | |
4 |
C/1961 T1 (Seki) is a long-period comet discovered by Tsutomu Seki on 10 October 1961. The comet has been identified as the parent body of the December ρ-Virginids meteor shower.
The comet was discovered on 10 October 1961 by Tsutomu Seki from Kochi, Japan. He used a 9-cm refractor, which had a larger field of view from his previous reflector telescope, to sweep the southeastern sky before the start of the twilight. He quickly spotted the comet 10 degrees above the horizon in the constellation of Leo and estimated its magnitude at 7–8. The comet was then at perihelion and at an elongation of 31 degrees. [2]
The presence of the comet was confirmed by Minoru Honda on 11 October, and described the comet as diffuse with central concentration and a magnitude of 8. The comet reached its northernmost declination on 14 October, at 14° north. [2] On that day the comet was reported by Ahnert to have a tail 4 degrees long while George Alcock estimated the comet to have an apparent magnitude of 7. [3] Elias and Phocas observed the comet from Athens Observatory and noted that the nucleus and had split in three on 17 October and there were bright condensations around the nucleus on 19 October. [4] On the 25 October Elizabeth Roemer estimated using binoculars that the comet had an apparent magnitude of 6.5. [5]
The comet brightened in November, as it approached Earth, and was moving rapidly southwards. The comet was first reported to be visible with naked eye on 11 November, with brightness estimates between 4.5 and 5.5. [2] The comet approached Earth to a distance of 0.102 AU on 15 November 1961. [1] S. Archer from Rhodes University, South Africa, estimated that the comet peaked at an apparent magnitude of 4.3 and its coma was up to 40 arcminutes across. [6] John Caister Bennett estimated the comet had an apparent magnitude of 4 on 13 and 15 November. The comet reached its southernmost declination of 16 November, at -69°. [2] After that the comet faded quickly and on 4 December its magnitude was reported to be 8.4. It was last detected on 29 December 1961. [2]
The comet approaches Earth to a distance of 0.08 AU and thus it was suggested from 1961 that is could be a source of meteors. Mathematical models indicate that the meteor stream of the comet evolved into two filaments. The shower associated with the first filament was identified as the December ρ-Virginids, while the other shower was identified as the γ-Sagittariids. [7]
Comet Ikeya–Seki, formally designated C/1965 S1, 1965 VIII, and 1965f, was a long-period comet discovered independently by Kaoru Ikeya and Tsutomu Seki. First observed as a faint telescopic object on 18 September 1965, the first calculations of its orbit suggested that on October 21, it would pass just 450,000 km (280,000 mi) above the Sun's surface, and would probably become extremely bright.
Comet Encke, or Encke's Comet, is a periodic comet that completes an orbit of the Sun once every 3.3 years. Encke was first recorded by Pierre Méchain on 17 January 1786, but it was not recognized as a periodic comet until 1819 when its orbit was computed by Johann Franz Encke. Like Halley's Comet, it is unusual in its being named after the calculator of its orbit rather than its discoverer. Like most comets, it has a very low albedo, reflecting only 4.6% of the light its nucleus receives, although comets generate a large coma and tail that can make them much more visible during their perihelion. The diameter of the nucleus of Encke's Comet is 4.8 km.
12P/Pons–Brooks is a periodic comet with an orbital period of 71 years. Comets with an orbital period of 20–200 years are referred to as Halley-type comets. It is one of the brightest known periodic comets, reaching an absolute visual magnitude of about 5 in its approach to perihelion. Comet Pons-Brooks was conclusively discovered at Marseilles Observatory in July 1812 by Jean-Louis Pons, and on its next appearance in 1883 by William Robert Brooks. There are ancient records of comets that are suspected of having been apparitions of 12P/Pons–Brooks.
13P/Olbers is a periodic comet with an orbital period of 69 years. It fits the classical definition of a Halley-type comet with a period between 20 and 200 years. The comet last passed perihelion 30 June 2024 and it was previously seen in 1956. The next perihelion is in 2094.
45P/Honda–Mrkos–Pajdušáková is a short-period comet discovered by Minoru Honda December 3, 1948. It is named after Minoru Honda, Antonín Mrkos, and Ľudmila Pajdušáková. The object revolves around the Sun on an elliptical orbit with a period of 5.25 years. The nucleus is 1.3 kilometers in diameter. On August 19 and 20, 2011, it became the fifteenth comet detected by ground radar telescope.
C/2007 W1 (Boattini) is a non-periodic comet discovered on 20 November 2007, by Andrea Boattini at the Mt. Lemmon Survey. At the peak the comet had an apparent magnitude around 5.
255P/Levy, formerly P/2006 T1 and P/2011 Y1, is a periodic comet with an orbital period of 5.25 years. It last came to perihelion on 14 January 2012. During the 2006 passage the comet achieved an apparent magnitude of ~9.5. Levy (PK06T010) was believed to have been recovered on 3 June 2011 at magnitude 19.8, but other observatories were unable to confirm a recovery. It was most likely a false positive because of large residuals. Levy was recovered on 17 December 2011 at magnitude 19.8, and given the second designation 2011 Y1. It was then numbered.
Comet Swift–Tuttle is a large periodic comet with a 1995 (osculating) orbital period of 133 years that is in a 1:11 orbital resonance with Jupiter. It fits the classical definition of a Halley-type comet, which has an orbital period between 20 and 200 years. The comet was independently discovered by Lewis Swift on July 16, 1862 and by Horace Parnell Tuttle on July 19, 1862.
209P/LINEAR is a periodic comet with an orbital period of 5.1 years. The comet has extremely low activity for its size and is probably in the process of evolving into an extinct comet.
93P/Lovas, also called Comet Lovas 1, is a Jupiter-family comet with an orbital period of 9.2 years. It was discovered in 1980 by Hungarian astronomer Miklós Lovas.
Comet 252P/LINEAR is a periodic comet and near-Earth object discovered by the LINEAR survey on April 7, 2000. The comet is a Jupiter family comet, meaning that it passes quite close to the orbit of Jupiter.
126P/IRAS is a periodic comet with an orbital period of 13.4 years. It was discovered in images taken by the Infrared Astronomical Satellite (IRAS) on 28 July 1983 by J. Davies. The discovery was confirmed with images taken with the 1.2-m Schmidt telescope at Palomar Observatory.
C/1962 C1 (Seki–Lines), also known as Comet Seki–Lines and 1962c, was a hyperbolic comet discovered independently by Richard D. Lines and Tsutomu Seki on 4 February 1962. The comet became vry bright in April 1962, as passed its perihelion on 1 April at a distance of 0.031 AU.
C/1963 A1 (Ikeya), also known as Comet 1963I and 1963a, is a long period comet discovered by Kaoru Ikeya on 2 January 1963. The comet last passed perihelion on 21 March 1963, when it reached an apparent magnitude of 2.8.
C/1979 Y1 (Bradfield), also known as Comet 1979X and 1979l, is a long period comet discovered by William A. Bradfield on 24 December 1979. The comet has an orbital period of 308 ± 6 years and last passed perihelion on 21 December 1979. It is considered to be the parent body of the July Pegasids meteor shower. It is expected to next come to perihelion around 2287.
C/1917 F1 (Mellish), also known as Comet 1917Ι and 1917a, is a Halley-type comet discovered by John E. Mellish on 19 March 1917. The comet has an orbital period of 143 years and last passed perihelion on 11 April 1917. It is the parent body of the December Monocerotids and has also been suggested to be the parent body of daytime kappa Leonids, April ρ-Cygnids, November Orionids, and Canis-Minorids meteor showers.
Comet Tago–Sato–Kosaka, formally designated as C/1969 T1, is a non-periodic comet that became visible in the naked eye between late 1969 and early 1970. It was the first comet ever observed by an artificial satellite.
C/1939 H1 (Jurlof–Achmarof–Hassel) is a long-period comet discovered on 15 April 1939. The comet was discovered by many observers independently but the first reports were those of Olaf Hassel, Achmarof, and Jurlof. The comet had a magnitude of 3 upon discovery.
C/1911 N1 (Kiess) is a non-periodic comet discovered by Carl Clarence Kiess on 6 July 1911. The comet has been identified as the parent body of the Aurigids meteor shower.
C/1975 T2 (Suzuki–Saigusa–Mori) is a long-period comet discovered on 5 October 1975. The comet approached Earth at a distance of 0.1 AU on 31 October 1975 and became visible with naked eye. The comet has been associated with the lambda Ursae Majorids meteor shower.