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Klymene is a large, dark Themistian asteroid that was discovered by J. C. Watson on September 13, 1868, and named after one of the many Clymenes in Greek mythology. It is orbiting the Sun with a period of 5.60 years and an eccentricity of 0.16. The orbital plane is inclined by 2.8° to the plane of the ecliptic. It is classified as a C-type asteroid, indicating it probably has a carbonaceous composition. The spectra indicates the presence of aqueous-altered minerals on the surface based upon a sharp feature at a wavelength of 3 μm, and, as of 2015, is the only member of the Themis family found to show this absorption.
Hecuba is a fairly large and bright main-belt asteroid. It was discovered by Karl Theodor Robert Luther on 2 April 1869, and named after Hecuba, wife of King Priam in the legends of the Trojan War in Greek Mythology. This object is orbiting the Sun with a period of 5.83 years and an eccentricity of 0.06. It became the first asteroid discovered to orbit near a 2:1 mean-motion resonance with the planet Jupiter, and is the namesake of the Hecuba group of asteroids.
Maria is a Main belt asteroid that was discovered by French astronomer Henri Joseph Perrotin on January 10, 1877. Its orbit was computed by Antonio Abetti, and the asteroid was named after his sister, Maria. This is the namesake of the Maria asteroid family; one of the first asteroid families to be identified by Japanese astronomer Kiyotsugu Hirayama in 1918.
Kiyotsugu Hirayama was a Japanese astronomer, best known for his discovery that many asteroid orbits were more similar to one another than chance would allow, leading to the concept of asteroid families, now called "Hirayama families" in his honour.
Shin Hirayama, also read as Makoto Hirayama, was the first Japanese astronomer to discover an asteroid. In 1900 he discovered 498 Tokio and 727 Nipponia. The crater Hirayama on the Moon is jointly named after him and Kiyotsugu Hirayama.
An asteroid family is a population of asteroids that share similar proper orbital elements, such as semimajor axis, eccentricity, and orbital inclination. The members of the families are thought to be fragments of past asteroid collisions. An asteroid family is a more specific term than asteroid group whose members, while sharing some broad orbital characteristics, may be otherwise unrelated to each other.
The Vesta family is a family of asteroids. The cratering family is located in the inner asteroid belt in the vicinity of its namesake and principal body, 4 Vesta. It is one of the largest asteroid families with more than 15,000 known members and consists of mostly bright V-type asteroids, so-called "vestoids".
The Eos family is a very large asteroid family located in the outer region of the asteroid belt. The family of K-type asteroids is believed to have formed as a result of an ancient catastrophic collision. The family's parent body is the asteroid 221 Eos.
The Pallas family is a small asteroid family of B-type asteroids at very high inclinations in the intermediate asteroid belt.
Tokio is a main-belt asteroid discovered on 2 December 1902 by Auguste Charlois at the Nice Observatory. Attribution to Astronomer Shin Hirayama of the Azabu Observatory, Tokyo, Japan for the 1900 discovery and naming of Tokio as cited in the 1947 Monthly Newsletter of the Royal Astronomical Society Vol 107, page 45.
727 Nipponia is a minor planet orbiting the Sun. It is a member of the Maria family of asteroids.
The proper orbital elements or proper elements of an orbit are constants of motion of an object in space that remain practically unchanged over an astronomically long timescale. The term is usually used to describe the three quantities:
The Flora family is a prominent family of stony asteroids located in the inner region of the asteroid belt. It is one of the largest families with more than 13,000 known members, or approximately 3.5% of all main-belt asteroids.
The Hygiea or Hygieanfamily is a grouping of dark, carbonaceous C-type and B-type asteroids in outer asteroid belt, the largest member of which is 10 Hygiea. About 1% of all known asteroids in the asteroid belt belong to this family.
1999 Hirayama is a dark background asteroid from the outer region of the asteroid belt, approximately 34 kilometers in diameter. It was discovered on 27 February 1973, by Czech astronomer Luboš Kohoutek at the Hamburger Bergedorf Observatory in Germany, and later named after Japanese astronomer Kiyotsugu Hirayama.
1181 Lilith is a metallic asteroid from the middle region of the asteroid belt, approximately 23 kilometers in diameter. It was discovered on 11 February 1927, by Russian–French astronomer Benjamin Jekhowsky at Algiers Observatory in Algeria, Northern Africa, and named after French composer Lili Boulanger.
3103 Eger is an Apollo and Mars-crosser asteroid that was discovered in 1982, by Miklós Lovas. It was named after the city of Eger, Hungary. It has an albedo of 0.64, making it a highly reflective asteroid.
The Maria family is a collisional asteroid family located in the inner parts of the intermediate asteroid belt, near the 1:3 Kirkwood gap. The family consist of several thousand stony S-type asteroids. It is named after its parent body and lowest numbered member, the asteroid 170 Maria. It is also known as the Roma family, named after its alternative parent body, 472 Roma.
2153 Akiyama, provisional designation 1978 XD, is a carbonaceous Themistian asteroid from the outer region of the asteroid belt, approximately 17 kilometers in diameter.
2090 Mizuho, provisional designation 1978 EA, is a stony asteroid from the outer region of the asteroid belt, approximately 18 kilometers in diameter.
References
- 1 2 Hirayama, Kiyotsugu (October 1918). "Groups of asteroids probably of common origin". Astronomical Journal: 185–188. Bibcode:1918AJ.....31..185H. doi: 10.1086/104299 . Retrieved 28 April 2018.
- ↑ Hirayama family, www.daviddarling.info
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