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John Holman (chemist) Holman also authored the "Good Practical Science" report and was the lead author of Improving Secondary Science guidance report for the Educational Environment Foundation (2018). Holman was Knighted in the 2010 New Year Honours. In 2014 the Royal Society of Chemistry awarded him the Lord Lewis Prize "in recognition of his extensive influence over chemistry education policy". Holman was named in 2014 by the Science Council as one of the UK's 100 leading practising scientists, and was the 2014 recipient of the Royal Society's biennial Kavli Education Medal, "in recognition of his significant impact on science education within the UK". | https://en.wikipedia.org/wiki?curid=45138583 |
Richardson (Martian crater) Richardson is a crater in the Mare Australe quadrangle on Mars, located at 72.6°S and 180.4°W. It measures 95.9 kilometers in diameter and was named after Lewis Fry Richardson. The name was approved by the International Astronomical Union in 1973. | https://en.wikipedia.org/wiki?curid=45145189 |
Wright (Martian crater) Wright is an impact crater in the Phaethontis quadrangle of Mars, located at 58.9°S latitude and 151.0°W longitude. It measures approximately 114 kilometers in diameter and was named after American astronomer William Hammond Wright (1871–1959). The naming was approved by the IAU in 1973. The Keeler–Trumpler crater pair lies to the south. | https://en.wikipedia.org/wiki?curid=45154663 |
Trumpler (Martian crater) Trumpler is a crater in the Phaethontis quadrangle of Mars, located at 61.8°S latitude and 150.8°W longitude. It measures approximately 78 kilometers in diameter and was named after Swiss-American astronomer Robert Julius Trumpler (1886–1956). The name was approved by IAU's Working Group for Planetary System Nomenclature in 1973. The first image below shows the relationship among three craters that are near each other. Keeler Crater is to the North of Trumpler Crater. After Keeler was formed, a later impact formed Trumpler Crater, and in the process destroyed part of Keeler. | https://en.wikipedia.org/wiki?curid=45154716 |
Keeler (Martian crater) Keeler is an impact crater on Mars, located at 61.0°S latitude and 151.3°W longitude in the Phaethontis quadrangle. It is 95.0 km in diameter and was named after James Edward Keeler, and the name was approved in 1973. The first image below shows the relationship among three craters that are near each other. Keeler Crater is to the North of Trumpler Crater. After Keeler was formed, a later impact formed Trumpler Crater, and in the process destroyed part of Keeler. | https://en.wikipedia.org/wiki?curid=45154809 |
Siphonogamy is a condition in plants in which pollen tubes are developed for the transfer of the male cells to the eggs. The seed plants are siphonogamous, while in the lower plants the male cells usually swim to the eggs. As a consequence, the spermatophytes were sometimes called siphonogams. | https://en.wikipedia.org/wiki?curid=45156172 |
Melchett Medal The Melchett Award is an honour awarded by the Energy Institute for outstanding contributions to the science of fuel and energy. It was created by and named for Alfred Moritz Mond, 1st Baron Melchett, the 20th century businessman and philanthropist. Previous winners include: | https://en.wikipedia.org/wiki?curid=45158152 |
NGC 3359 is a galaxy located 49 million light years from Earth. The central bar is approximately 500 million years old. NGC is "devouring" the much smaller galaxy, nicknamed the Little Cub. | https://en.wikipedia.org/wiki?curid=45158715 |
NGC 3718 NGC 3718, also called Arp 214, is a galaxy located approximately 52 million light years from Earth in the constellation Ursa Major. It is either a lenticular or spiral galaxy. has a warped, s-shape. This may be due to gravitational interaction between it and NGC 3729, another spiral galaxy located 150,000 light-years away. is a member of the Ursa Major Cluster. | https://en.wikipedia.org/wiki?curid=45158758 |
Douglass (Martian crater) Douglass is a crater in Thaumasia quadrangle of Mars, located at 51.8°S latitude and 70.6°W longitude. It is 94.0 km in diameter. It was named after American astronomer Andrew E. Douglass, and the name was approved in 1973. | https://en.wikipedia.org/wiki?curid=45164926 |
Eudoxus (Martian crater) Eudoxus is an impact crater in the Phaethontis quadrangle of Mars, located at 44.9°S latitude and 147.5°W longitude. It is 98.0 km in diameter. It was named after Greek astronomer Eudoxus of Cnidus (4th century BC), and the name was approved in 1973. The closest named crater is Hipparchus to the west, other named craters are further away including Nansen to the southeast and Yaren to the east. | https://en.wikipedia.org/wiki?curid=45164968 |
Lamont (Martian crater) Lamont is a crater in the Thaumasia quadrangle of Mars, located at 58.6°S latitude and 113.6°W longitude. It is 76.0 kilometers in diameter. It was named after German astronomer Johann von Lamont. | https://en.wikipedia.org/wiki?curid=45165003 |
Li Fan (crater) Li Fan is an impact crater in the Phaethontis quadrangle of Mars, located at 47.2°S latitude and 153.2°W longitude. It is 104.8 kilometers in diameter. It was named after 1st century Chinese astronomer Li Fan; the name was approved in 1973. Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits. As craters get larger (greater than 10 km in diameter) they usually have a central peak. The peak is caused by a rebound of the crater floor following the impact. The picture on this page shows the central peak of Li Fan Crater. | https://en.wikipedia.org/wiki?curid=45167582 |
Kuiper (Martian crater) Kuiper is an impact crater in the Phaethontis quadrangle of Mars, located at 57.4°S latitude and 157.3°W longitude. It is 82 kilometers in diameter. It was named after Dutch–American astronomer Gerard Kuiper, and the name was approved in 1976. | https://en.wikipedia.org/wiki?curid=45167679 |
Williams (Martian crater) Williams is an impact crater on Mars, located in the Memnonia quadrangle at 18.7°S latitude and 164.3°W longitude. It measures 123.2 kilometers in diameter and was named after British astronomer Arthur S. Williams. The name was approved by IAU's Working Group for Planetary System Nomenclature in 1973. | https://en.wikipedia.org/wiki?curid=45168051 |
WISE J2209+2711 is a brown dwarf of spectral type Y0:, located in constellation Pegasus at 22 light-years from Earth. Its discovery was published in 2014 by Cushing "et al." | https://en.wikipedia.org/wiki?curid=45170102 |
Sweeping jet actuators are a type of active flow control technology based on fluidic oscillators used to produce sweeping jets. The first use of fluidic oscillators in the form of sweeping jets for flow control was demonstrated by Raman et al., 1999.<Cavity Resonance Suppression Using Miniature Fluidic Oscillators, G. Raman, S. Raghu and T.J. Bencic' AIAA-99-1900, 5th AIAA/CEAS Aeroacoustics Conference, Seattle, WA, May 10–12, 1999> and later by several authors working in the area of flow control. Many organizations have been working on the use of such actuators for flow control. Boeing, NASA and the University of Arizona Department of Aerospace and Mechanical Engineering, Illinois Institute of Technology, [Advanced Fluidics], Technical University of Berlin are a few of them. They are slots built into the control surface of an airfoil that build on the same principles as that of blown flaps; that by actively blowing air over the surface of an airfoil the effective lift produced by it is increased. The impetus behind the research into sweeping jet actuators lies in the realization that any vertical tail structure on an aircraft is a parasitic surface in level flight | https://en.wikipedia.org/wiki?curid=45173684 |
Sweeping jet actuators The design specification that must be met by the vertical stabilizer of any multi-engined aircraft is that it be able to produce enough lift to counteract any thrust asymmetry that would come as a result of engine failure during rotation (takeoff); but in any condition that is not an emergency or where a yaw moment is not desired the vertical stabilizer will only contribute added weight and drag to the aircraft. The jet nozzles (located directly upstream of the hinge around which the rudder moves) eject a subsonic stream of air that flows over the rudder and act to retain or reattach the boundary layer to the control surface as it is deflected beyond the incidence angle where natural flow would separate, generating as much as a 30-percent increase in the effective lift produced by the rudder. As of January 2015 sweeping jet actuators have only seen experimental application and are not included as a design feature of any known aircraft. Cavity Resonance Suppression Using Miniature Fluidic Oscillators, G. Raman, S. Raghu and T.J. Bencic, AIAA-99-1900, 5th AIAA/CEAS Aeroacoustics Conference, Seattle, WA, May 10–12, 1999 | https://en.wikipedia.org/wiki?curid=45173684 |
David Shugar (10 September 1915 – 31 October 2015) was a professor of the University of Warsaw. After the First World War, he settled as a child with his parents in Canada. In 1936 he concluded his education of physics at McGill University in Montreal and obtained his doctorate in 1940. Since January 1941, he did research in biophysics in the laboratory of Research Enterprises, Limited, a Crown Company in Leaside near Toronto, later served in the Canadian Marines with the rank of Electrical Sub-Lieutenant R.C.N.V.R. In 1946 he entered the employ of the Department of National Health and Welfare. was detained by the Royal Canadian Mounted Police in 1946 and charged with conspiring to hand over official secrets to the Russians. The government tried to charge him twice; however, in both situations there was not enough evidence to do so. He continued working as a researcher, first at the Pasteur Institute in Paris in the years 1948-1950, and later at the Center of Nuclear Physics of the Free University of Brussels until 1952. On the invitation of professor Leopold Infeld, he moved to Warsaw, where he took the post of the head of the Institute of Biochemistry at the National Institute of Hygiene. Since 1954, he conducted research at the Institute of Biochemistry and Biophysics of the Polish Academy of Sciences. In 1965, he created the Biophysics Department of the Faculty of Physics of University of Warsaw. The same year he was elected the Chairman of the Polish Society of Medical Physics | https://en.wikipedia.org/wiki?curid=45181017 |
David Shugar He was a member of the Polish Academy of Sciences since 1983. obtained in 1969 the honorary degree from Ghent University and in 1995 from the University of Warsaw. In 1999, Professor David Shugar, the founder of the Division of Biophysics and an architect of The Polish School of Molecular Biophysics, was inducted into The Royal Society of Canada. His spouse, Professor Grace Wales Shugar (1918 - 2013), created the Center of the Developmental Psycholinguistics at the Faculty of Psychology of the University of Warsaw. He died at the age of 100 on 31 October 2015. | https://en.wikipedia.org/wiki?curid=45181017 |
Vogel (Martian crater) Vogel is an impact crater in the Argyre quadrangle of Mars, located at 36.8°S latitude and 13.4°W longitude, and is inside Noachis Terra. It measures approximately 121 kilometers in diameter and was named after German astronomer Hermann Carl Vogel. The name was approved by IAU's Working Group for Planetary System Nomenclature in 1973. | https://en.wikipedia.org/wiki?curid=45198287 |
Tikhov (Martian crater) Tikhov is an impact crater in the Hellas quadrangle on Mars at 50.7°S and 105.8°E. It is 111.0 km in diameter. Its name was approved in 1973 by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature, and it was named after Russian astronomer Gavriil Adrianovich Tikhov. | https://en.wikipedia.org/wiki?curid=45198996 |
Wallace (Martian crater) Wallace is an impact crater in the Hellas quadrangle on Mars at 52.9°S and 249.4°W. It is 173.0 km in diameter. Its name was approved in 1973 by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature (WGPSN), and refers to British biologist Alfred Russel Wallace. | https://en.wikipedia.org/wiki?curid=45199018 |
Wells (crater) Wells is an impact crater in the Eridania quadrangle on Mars at 60.2°S and 237.9°W. It measures approximately 98 kilometers in diameter. The crater was named after English writer H. G. Wells (1866–1946). The name was approved in 1973, by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature. | https://en.wikipedia.org/wiki?curid=45199068 |
Martz (crater) Martz is an impact crater on Mars, located in the Eridania quadrangle at 35.3°S latitude and 215.9°W longitude. Martz is east of the giant impact basin Hellas Planitia. It measures 97.0 kilometers in diameter and was named after American physicist and astronomer Edwin P. Martz. The name was approved by IAU's Working Group for Planetary System Nomenclature in 1973. Gullies are visible in the images. | https://en.wikipedia.org/wiki?curid=45208830 |
Knobel (crater) Knobel is an impact crater in the Mare Tyrrhenum quadrangle of Mars, located at 6.7°S latitude and 226.8°W longitude and is in the northern end of Terra Cimmeria. It is 123 kilometers in diameter. It was named after British astronomer Edward Knobel; the name was approved in 1973 by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature (WGPSN). | https://en.wikipedia.org/wiki?curid=45209048 |
Huggins (Martian crater) Huggins is an impact crater in the Eridania quadrangle of Mars, located at 49.0°S latitude and 155.8°E longitude. It is 83 km in diameter. It was named after British astronomer William Huggins, and the name was approved in 1973 by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature (WGPSN). | https://en.wikipedia.org/wiki?curid=45210059 |
Hadley (crater) Hadley is an impact crater in the Aeolis quadrangle of Mars, located at 19.5°S latitude and 203.1°W longitude, and is inside Terra Cimmeria. It is 119.0 km in diameter. It was named after British meteorologist George Hadley; the name was approved in 1973. Dunes are present on the floor of the crater and can be seen in the pictures on the left. | https://en.wikipedia.org/wiki?curid=45210195 |
Gustave Arthur Poujade (1845–1909, Fontainebleau) was a French entomologist interested in Coleoptera and Lepidoptera. He was an honorary preparator in the Muséum national d'histoire naturelle in Paris. The museum holds his collections. He described new species of Lepidoptera in Bulletin du Muséum national d'Histoire naturelle de Paris and Bulletin de la Société entomologique de France. He was especially interested in the butterflies and moths of Tibet. Gustave Poujade was a Member of Société entomologique de France. | https://en.wikipedia.org/wiki?curid=45223088 |
Hooke (Martian crater) Hooke Crater is an impact crater in the Argyre quadrangle on Mars at 45.2°S and 44.4°W and is 139.0 km in diameter. It was named after British physicist-astronomer Robert Hooke. Some of the dunes have gullies on them. While these gullies may be a bit different then ones found on crater walls and other steep slopes, they have been thought by some to be caused by flowing water. | https://en.wikipedia.org/wiki?curid=45224102 |
Jones (Martian crater) Jones is an impact crater on Mars, located at in the Margaritifer Sinus quadrangle. It measures 94.0 kilometer in diameter and was named after English astronomer Harold Spencer Jones (1890–1960). The name was approved in 1973, by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature (WGPSN). | https://en.wikipedia.org/wiki?curid=45224125 |
Helmholtz (Martian crater) Helmholtz Crater is an impact crater in the Argyre quadrangle on Mars at 45.8°S and 21.3°W and is 111.5 km in diameter. Helmholtz is located just east of Argyre Planitia. Its name refers to German physicist Hermann von Helmholtz (1821–1894). | https://en.wikipedia.org/wiki?curid=45224240 |
Haldane (Martian crater) Haldane is an impact crater in the Eridania quadrangle of Mars, located at 52.8°S and 230.7°W. It is 77 km in diameter. It was named after British physiologist and geneticist J. B. S. Haldane; the name was approved in 1973 by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature (WGPSN). | https://en.wikipedia.org/wiki?curid=45231585 |
Huxley (Martian crater) Huxley is a crater in the Hellas quadrangle of Mars, located at 63.0°S latitude and 259.2°W longitude. It is 107.0 km in diameter. It was named after British biologist Thomas Henry Huxley, and the name was approved in 1973 by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature (WGPSN). | https://en.wikipedia.org/wiki?curid=45233200 |
Wojciech Królikowski (July 16, 1926 – April 29, 2019) was a Polish theoretical physicist, specialized in the theory of elementary particles and quantum field theory, retired professor of the Institute of Theoretical Physics at the University of Warsaw, member of the Polish Academy of Science. He obtained 1952 his doctor degree as pupil of professor Wojciech Rubinowicz, and his Habilitation in 1957. 1956–1957 he visited the Eidgenössische Technische Hochschule Zürich, Switzerland for scientific practice under Wolfgang Pauli. 1965 he obtained his professor title. 1961 he visited the Institute for Advanced Study in Princeton, New Jersey. He visited also the European Organization for Nuclear Research in Geneva and the International Centre for Theoretical Physics in the Miramare Castle near Trieste, Italy. He initiated the research of the theory of elementary particles at the University of Warsaw. He founded 1960 the Department of the Theory of Elementary Particles, and directed it till hir retirement. Together with Jan Rzewuski he gave the formula of relativistic quantum mechanics of some substances. He proposed the hypothesis of compound quarks. He created the model of three generations of leptons and quarks. Together with Wojciech Rubinowicz he wrote the handbook of Theoretical Mechanics (first edition 1955, until now nine editions). In 1987, he was awarded with the Marian Smoluchowski Medal. | https://en.wikipedia.org/wiki?curid=45236991 |
Dunathan stereoelectronic hypothesis is a concept in chemistry to explain the stereospecefic cleavage of bonds using pyridoxal phosphate. This occurs because stereoelectronic effects controls the actions of the enzyme. Before the correlation between fold type and reaction correlation of proteins were understood, Harmon C. Dunathan, a chemist at Haverford College proposed that the bond that is cleaved using pyridoxal is perpendicular to the system. Though an important concept in bioorganic chemistry, it is now known that enzyme conformations play a critical role in the final chemical reaction. The transition state is stabilized by the extended pi bond network (formation of anion). Furthermore hyperconjugation caused by the extended network draws electrons from the bond to be cleaved, thus weakening the chemical bond and making it labile The sigma bond that is parallel to the pi bond network will break. The bond that has the highest chance of being cleaved is one with the largest HOMO-LUMO overlap. This effect might be effected by electrostatic effects within the enzyme. This was seen in transferase and future interests lie in decarboxylation in various catalytic cycles. | https://en.wikipedia.org/wiki?curid=45239121 |
Jarry-Desloges (crater) Jarry-Desloges is an impact crater in the Iapygia quadrangle of Mars, located at 9.5°S latitude and 276.3°W longitude. It is 92.0 km in diameter and was named after René Jarry-Desloges, and the name was approved in 1973. Pictures show dunes on the floor of the crater; these can be seen in the pictures below; some of them are Barchans. When there are perfect conditions for producing sand dunes, steady wind in one direction and just enough sand, a barchan sand dune forms. Barchans have a gentle slope on the wind side and a much steeper slope on the lee side where horns or a notch often forms. The whole dune may appear to move with the wind. Observing dunes on Mars can tell us how strong the winds are, as well as their direction. | https://en.wikipedia.org/wiki?curid=45242346 |
Niesten (crater) Niesten is an impact crater on Mars, located in the Iapygia quadrangle at 28.3°S latitude and 302.3°W longitude. It measures 115 kilometers in diameter and was named after Belgian astronomer Louis Niesten. The name was approved by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature in 1973. | https://en.wikipedia.org/wiki?curid=45242440 |
Mie (crater) Mie Crater is an impact crater on Mars, located in the Cebrenia quadrangle at . It measures 104 kilometers in diameter and named after Gustav Mie. The name was approved by IAU's Working Group for Planetary System Nomenclature in 1973. | https://en.wikipedia.org/wiki?curid=45243261 |
Vinogradov (crater) Vinogradov is an impact crater in the Margaritifer Sinus quadrangle of Mars, located at 20.2°S°S latitude and 37.7°W°W longitude. It measures 223.5 km in diameter and was named after Alexander Pavlovich Vinogradov, and the name was approved in 1979 by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature (WGPSN). | https://en.wikipedia.org/wiki?curid=45250110 |
Vinogradsky (crater) Vinogradsky is an impact crater in the Eridania quadrangle of Mars, located at 56.5°S latitude and 216.2°W longitude. It measures 64 kilometers in diameter and was named after Sergei Winogradsky. The name was approved in 1973, by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature. | https://en.wikipedia.org/wiki?curid=45250172 |
Gledhill (crater) Gledhill is an impact crater in the Hellas quadrangle of Mars, located at 53.2°S latitude and 87.1°E longitude. It is 78.5 km in diameter. It was named after British astronomer Joseph Gledhill, and the name was approved in 1973 by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature (WGPSN). Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits. As craters get larger (greater than 10 km in diameter) they usually have a central peak. The peak is caused by a rebound of the crater floor following the impact. Gledhill Crater shows a central peak in a picture on this page. | https://en.wikipedia.org/wiki?curid=45250210 |
Ludwig Carl Friedrich Graeser Ludwig Carl Friedrich (Louis) Graeser (12 February 1840, in Dresden – 9 December 1913, in Hamburg) was a German entomologist who specialised in Palearctic Lepidoptera. He was a bookbinder. His collections are in the Zoological Museum of the Zoological Institute of the Russian Academy of Sciences (Amur, Siberia) and Zoologisches Museum Hamburg (West Palearctic) 1888-9 Beiträge zur Kenntnis der Lepidopteren-Fauna des Amurlandes "Berl. Ent. Zs." 32 (1): 33–153 (1888), (2): 309–414 (1889) | https://en.wikipedia.org/wiki?curid=45251121 |
NGC 4145 is a barred spiral galaxy located in the Ursa Major galaxy cluster, 68 million light years from the Earth. The galaxy has little star formation, except on its outer edges. Due to the loss of energy that occurs without star formation, some astronomers predict that the galaxy will degenerate into a lenticular galaxy in the near future. However, the galaxy's interaction with NGC 4151 may "maintain [its] star formation". | https://en.wikipedia.org/wiki?curid=45254922 |
Matt Wedel Mathew John Wedel is an American paleontologist. He is associate professor at the Western University of Health Sciences Department of Anatomy in California. Wedel studies sauropods and the evolution of pneumatic bones in dinosaurs. At Western University, Wedel teaches gross anatomy. He has authored papers naming "Aquilops" (2014), "Brontomerus" (2011), and "Sauroposeidon" (2000). Along with paleontologists Darren Naish and Mike P. Taylor, he founded the paleontology blog Sauropod Vertebrae Picture of the Week. | https://en.wikipedia.org/wiki?curid=45254942 |
NGC 6861 is a lenticular galaxy located in the constellation Telescopium. It is the second-brightest object in the constellation. Unlike most lenticular galaxies, which tend to be mostly devoid of both gas and dust, exhibits a thick obscuring ring of dust around the nucleus where star formation is occurring. The galaxy was discovered by Scottish astronomer James Dunlop, in 1826. is interacting with NGC 6868, and it is predicted that they will eventually merge. | https://en.wikipedia.org/wiki?curid=45262979 |
NGC 2217 is a nearly face-on lenticular galaxy of about 100 thousand light-years across that lies roughly 65 million light years from Earth in the constellation of Canis Major. It is part of the Group of galaxies. It is classified as a barred spiral galaxy. A notable feature is the swirling shape of this galaxy. In its very concentrated central region we can see a distinctive, very luminous bar of stars within an oval ring. Further out, a set of tightly wound spiral arms almost form a circular ring around the galaxy. Central bars play an important role in the development of a galaxy. They can, for example, funnel gas towards the center of the galaxy, helping to feed a central black hole, or to form new stars. | https://en.wikipedia.org/wiki?curid=45280259 |
Tyndall (Martian crater) Tyndall is an impact crater in the Cebrenia quadrangle of Mars, located at 40.0°N latitude and 190.1°W longitude. It measures approximately 87 kilometers in diameter and was named after Irish physicist John Tyndall (1820–1893). The name was approved in 1973, by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature. | https://en.wikipedia.org/wiki?curid=45284409 |
Baldet (Martian crater) Baldet Crater is an impact crater in the Syrtis Major quadrangle of Mars, located at 23.0°N latitude and 294.6°W longitude. It is 180.0 km in diameter and was named after Fernand Baldet, and the name was approved in 1973 by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature (WGPSN). Baldet crater overlaps the rim of the larger Antoniadi crater, which lies to the west, just outside this image on the left. Antoniadi crater is more than twice as big as Baldet. | https://en.wikipedia.org/wiki?curid=45284504 |
Peridier (crater) Peridier is an impact crater on Mars, located in the Syrtis Major quadrangle at 25.5°N latitude and 83.9°E longitude. It measures 100 kilometers in diameter and was named after French electrical engineer and amateur astronomer Julien Peridier. The naming was approved by IAU's Working Group for Planetary System Nomenclature in 1973. | https://en.wikipedia.org/wiki?curid=45284643 |
Penta-graphene is a carbon allotrope composed entirely of carbon pentagons and resembling the Cairo pentagonal tiling. was proposed in 2014 on the basis of analyses and simulations. Further calculations showed that it is unstable in its pure form, but can be stabilized by hydrogenation. Owing to its atomic configuration, penta-graphene has an unusually negative Poisson’s ratio and very high ideal strength believed to exceed that of a similar material, graphene. contains both "sp" and "sp" hybridized carbon atoms. Contrary to graphene, which is a good conductor of electricity, penta-graphene is an insulator with an indirect band gap of 4.1–4.3 eV. Its hydrogenated form is called penta-graphane. It has a diamond-like structure with "sp" and no "sp" bonds, and therefore a wider band gap (ca. 5.8 eV) than penta-graphene. Chiral penta-graphene nanotubes have also been studied as metastable allotropes of carbon. | https://en.wikipedia.org/wiki?curid=45294937 |
Fanny Hesse (born Angelina Fanny Elishemius, June 22, 1850 – December 1, 1934) is best known for her work in microbiology alongside her husband, Walther Hesse. Together they were instrumental in developing agar as a medium for culturing microorganisms. Hesse was born in 1850 in New York City to Gottfried Elishemius, a wealthy import merchant, and his wife, Ceclie Elise. She met her husband and research partner, Walther Hesse, in 1872 while in Germany. They were engaged in 1873, and married in 1874 in Geneva. Hesse worked in an unpaid capacity to assist her husband through preparing bacterial growth media, cleaning equipment and producing illustrations for publications. In 1881, while her husband was working in the laboratory of German physician and microbiologist Robert Koch, Hesse suggested that agar was preferable to gelatin for cultivating bacteria. She was aware of the properties of agar as a gelling agent that maintained its gel properties at warm temperatures through using it at home to make puddings and jellies. A neighbour who had lived in Java had introduced agar to her when she lived in America. This led to Koch using agar to cultivate the bacteria that cause tuberculosis. Although Koch, in an 1882 paper on tuberculosis bacilli, mentioned he used agar instead of gelatin, he did not credit either Hesse, or mention why he made the switch. Hesse's suggestion never resulted in financial benefit for the Hesse family. | https://en.wikipedia.org/wiki?curid=45295473 |
Le Verrier (Martian crater) Le Verrier is an impact crater in the Noachis quadrangle of Mars, located at 38.0°S latitude and 342.9°W longitude, and is inside Noachis Terra. It is 138 kilometers in diameter. It was named after French mathematician and astronomer Urbain Le Verrier. The name was approved in 1973 by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature (WGPSN). | https://en.wikipedia.org/wiki?curid=45296275 |
Redi (crater) Redi is an impact crater Mars, located in the Hellas quadrangle at 60.6°S latitude and 267.3°W longitude. The crater measures 62 kilometers in diameter and was named after 17th century Italian physician Francesco Redi. The name was approved by IAU's Working Group for Planetary System Nomenclature in 1973. Redi Crater displays dust devil tracks. Part of its floor is covered by a smooth deposit called "latitude dependent mantle." | https://en.wikipedia.org/wiki?curid=45296303 |
Lassell (Martian crater) Lassell is an impact crater in the Coprates quadrangle of Mars, located at 20.9°S latitude and 62.5°W longitude. It is 92.0 km in diameter. It was named after British astronomer William Lassell, and the name was approved in 1973. | https://en.wikipedia.org/wiki?curid=45296546 |
Lampland (Martian crater) Lampland is an impact crater on Mars, located in the Thaumasia quadrangle at 35.9°S latitude and 79.6°W longitude. It is 79.0 kilometers in diameter and was named after Carl Otto Lampland. The name was approved by IAU's Working Group for Planetary System Nomenclature in 1973. The density of impact craters is used to determine the surface ages of Mars and other solar system bodies. The older the surface, the more craters present. Crater shapes can reveal the presence of ground ice. Lampland Crater sits in an area with many craters, hence this region is considered to be quite old. | https://en.wikipedia.org/wiki?curid=45296626 |
Graff (Martian crater) Graff is an impact crater in the Aeolis quadrangle of Mars, located at 21.4°S latitude and 206.3°W longitude and is inside Terra Cimmeria. It is 158.0 km in diameter. It was named after German astronomer Kasimir Graff, and the name was approved in 1973. | https://en.wikipedia.org/wiki?curid=45304503 |
Lambert (Martian crater) Lambert is an impact crater in the Sinus Sabaeus quadrangle of Mars, located at 20.2°S latitude and 334.7°W longitude. It is 92 km in diameter. It was named after German physicist Johann Heinrich Lambert, and the name was approved in 1973. | https://en.wikipedia.org/wiki?curid=45304535 |
Millochau (crater) Millochau is an impact crater on Mars, located in the Iapygia quadrangle at 21.4°S latitude and 275.0°W longitude. It measures 115 kilometers in diameter and was named after French astronomer Gaston Millochau. The naming was approved by IAU's Working Group for Planetary System Nomenclature in 1973. | https://en.wikipedia.org/wiki?curid=45304569 |
Priestley (Martian crater) Priestley is an impact crater in the Eridania quadrangle of Mars, located at 54.4°S latitude and 229.4°W longitude. It measures 41.9 kilometers in diameter and was named after English clergyman and scientist Joseph Priestley. The naming was approved by IAU's Working Group for Planetary System Nomenclature in 1973. | https://en.wikipedia.org/wiki?curid=45306572 |
Elysium Health is a company founded in 2014 by biologist Leonard Guarente, Dan Alminana, and Eric Marcotulli to market dietary supplements. The next year, the company started selling a dietary supplement called Basis that packages two supplements, nicotinamide riboside (NR), a form of B vitamin found in yeast, and pterostilbene, a polyphenol found in blueberries, into one capsule. The company says that these two ingredients help cells make nicotinamide adenine dinucleotide (NAD) and that they stimulate sirtuins. The company is widely described as being in the anti-aging field and similar to Sirtris Pharmaceuticals which was developing resveratrol. Elysium has tried to differentiate the product within the dietary supplement industry as being more scientific and exclusive, by means of the product's minimalist packaging, by not selling the product in drug stores but rather only through its website, and by getting several Nobel prize winners to join its scientific advisory board. The company has been criticized for using this advisory board to lend credibility to its product. Like other companies in the supplement industry, Elysium marketed the product heavily on social media. Elysium originally bought the ingredients in Basis from ChromaDex, which as of December 2016, sold the two ingredients to other supplement companies that also marketed products containing them | https://en.wikipedia.org/wiki?curid=45314746 |
Elysium Health The two companies had an agreement under which didn't have to acknowledge ChromaDex as the source of the ingredients, but then after Elysium recruited the head of business development from Chromadex and allegedly stopped paying Chromadex, Chromadex sued Elysium and the information became public. In September 2018, Dartmouth College and ChromaDex sued Elysium for infringement of two issued patents exclusively licensed by ChromaDex on use of NR to increase NAD that were invented by Charles Brenner. Elysium is one of several companies founded at around the same time by people with backgrounds in the tech industry and Silicon Valley who saw opportunities in the health and biomedical industries, often focused on anti-aging. | https://en.wikipedia.org/wiki?curid=45314746 |
Asteroid Zoo is a citizen science project run by the Zooniverse and Planetary Resources, to use volunteer classifications to find unknown asteroids using old Catalina Sky Survey data. The main goals of the project are to search for undiscovered asteroids in order to protect the planet by locating potentially harmful near-Earth Asteroids, locate targets for future asteroid mining, study the solar system, and study the potential uses and advantages of people looking through the images over computers. It was created along with the ARKYD project through Kickstarter, funded with just over 1.5 million dollars. The AsteroidZoo community has exhausted the data that were available. With all the data examined they paused the experiment. produced several scientific publications. Zooniverse projects: | https://en.wikipedia.org/wiki?curid=45317477 |
Captive bubble method The is a method for measuring contact angle between a liquid and a solid, by using drop shape analysis. In this method, a bubble of air is injected beneath a solid, the surface of which is located in the liquid, instead of placing a drop on the solid as in the case of the sessile drop technique. The method is particularly suitable for solids with high surface free energy on which liquids spread out. Hydrogels, such as soft contact lenses for example, are likewise inaccessible for the standard arrangement; the captive bubble method is also used in such cases.The captive bubble method is a scientific method for measuring the contact angle between a solid surface and liquid in a fluid. A contact angle is formed on a smooth, periodically heterogeneous solid surface. Above the solid surface, a liquid drop is submerged to the solid in a fluid. The measurement of contact angles usually contributes to the measurement of the surface energy of solids in the industry. Different from other methods of measuring the contact angle, such as the sessile drop method, the system utilized in the captive bubble method has the fluid bubble attached from below to the solid surface, in which both the liquid bubble and the solid interact with a fluid. As a system is formed from a solid surface and a drop of liquid, energy minima and maxima are produced by the free energy of the system | https://en.wikipedia.org/wiki?curid=45330103 |
Captive bubble method When the solid surface is rough or homogeneous, the system, which is made up of a solid, a liquid, and a fluid, could have multiple minima produced from the free energy at different minima points. One of these minima is called the global minimum. The global minimum has the lowest free energy within the system and is defined to be the stable equilibrium state. Furthermore, the other minima illustrate the metastable equilibrium states of the system. In between these minima are the energy barriers which hinder the motion of energy between the various metastable states in the system. The transition of energy between metastable states is also affected by the availability of external energy of the system, which is as well associated with the volume of the liquid drop on top of the solid surface. Likewise, the volume of the liquid could potentially have an impact on the locations of the minima points, which could influence the contact angles created by the solid and the liquid. Besides, the contact angles are directly related to whether the solid surface is ideal, in other words, whether it is a smooth, heterogeneous surface. In the Captive Bubble Method, the bubble indicating the liquid drop makes an angle with the solid surface which is called the contact angle. The stability of the liquid phase on the solid is measured with an intrinsic contact angle. Theoretically, the contact angle equals to the value of the local intrinsic contact angle with the assumption of a negligible effect of line tension | https://en.wikipedia.org/wiki?curid=45330103 |
Captive bubble method The measurement of contact angles with the Captive Bubble method could also be useful in the surface analysis of the reverse osmosis membrane for the studying of membrane performances. Through the analysis of contact angles, properties of membranes, such as roughness, can be determined. The roughness of membranes, which indicates the effective surface area, can further lead to the investigation in the hydrophilic and hydrophobic properties of the surface. Through studies, a higher contact angle may correspond to a more hydrophobic surface in membrane analysis. In the performance of the Captive Bubble Method in membrane analysis, several factors can have influence on the contact angle, including the bubble volume, liquid types and tensions. In the apparatus of the captive bubble method in membrane analysis, the membrane sample is attached to a piece of glass, while a J-shaped needle is inserted from below the glass in the liquid to release air bubbles. In this case, the contact angle between the air bubble and the glass surface is recorded as a function of time to investigate the effect of measurement time. In comparison to the use of the captive bubble method in the measurement of contact angles in other cases, the contact angle in the study of lung surfactant monolayer is kept at constant, which is 180 degrees, due to the property of a hydrated agar gel of the ceiling of the bubble | https://en.wikipedia.org/wiki?curid=45330103 |
Captive bubble method The system applied in the study of lung surfactant is designed to be a leak-proof system, ensuring the independence of the surface film of bubbles from other materials and substances like plastic walls, barriers, and outlets. Instead of adding extra tubing or piercing the bubble air-water interface with needles, this closed system is created by adjusting the pressure within the closed sample chamber by adding or removing aqueous media to regulate the bubble size and surface tension of insoluble films at the bubble surface. Since the bubble volumes are controlled by modifying the pressure in the sample chamber, the surface area and the surface tension of the surfactant film at the bubble surface are reduced as the volume of the bubble decreases. The bubble shape, in this case, can vary from spherical to oval shape depending on the surface tension, which can be calculated through the measurement of height and diameter of bubbles. In addition to measuring the surface tension, bubble formation can also be utilized in the measurement of the adsorption of lung surfactant, which defines how quickly substances build up on the air-liquid interface of pulmonary surfactants to form a film. There are two methods to measure adsorption with captive bubbles: The sessile drop method is also one popular way to measure contact angles by placing a two-dimensional drop on a solid surface and controlling the volume of liquid in the drop | https://en.wikipedia.org/wiki?curid=45330103 |
Captive bubble method The sessile drop method and the captive bubble method are usually interchangeable in performing experiments since their common property of symmetry. Specifically, the axis of symmetry of the drop and bubble of the two methods makes the contact line of the drop of liquid with the solid surface circular, which therefore creates an observable contact angle in corresponding to each contact radius of the drop and bubble. However, interacting with a rough homogeneous surface in measurements of contact angles, the drop and bubble of the two methods each presents different behaviours in the measuring process, which are related to the volume of liquid and contact angles. | https://en.wikipedia.org/wiki?curid=45330103 |
Salvatore Trinchese (4 April 1836 – 11 January 1897) was an Italian zoologist who specialised in Mollusca. was born in Martano, a small town in the province of Lecce in Italy, on 4 April 1836. He attended the "Reale Collegio San Giuseppe" of Jesuits in Lecce. In 1856 he went to Pisa to study medicine and surgery. In 1860 he graduated and obtained a scholarship which allowed him to study abroad. Thus, in the same year he moved to Paris, where he worked as a researcher in the prestigious laboratories of Claude Bernard, Henri Milne-Edwards, Emile Blanchard and Charles-Philippe Robin. During this period he started his histological studies on the nervous system and on the systematic microscopy on gastropod molluscs. In 1865 he started to teach mineralogy, geology, zoology and comparative anatomy at the University of Genoa. Then he taught in Bologna and Naples. In 1886 he became the dean of the University of Naples and, after few years, was nominated as the city councilman. He died of nephritis in Naples on 11 January 1897. | https://en.wikipedia.org/wiki?curid=45334061 |
Sperm precedence Sperm precedence, also known as sperm predominance, is tendency of a female who has been bred by multiple males to give birth to their offspring in unequal proportions. is an important factor in the sperm competition. can be temporal, favoring either the first or last male to breed the female. (The former is known as "first sperm precedence" and the latter is known as "last sperm precedence"); or it can favor the male whose sperm are the most motile; or the male whose sperm were delivered closest to the female's ova. | https://en.wikipedia.org/wiki?curid=45335171 |
Zinaida Aksentyeva Zinaïda Mikolaïevna Aksentieva (July 25, 1900 – April 8, 1969) was a Ukrainian/Soviet astronomer and geophysicist. Aksentieva or Aksentyeva was born in Odessa in 1900. She graduated from Odessa University in 1924. She worked on mapping gravity and her observatory was one of the first to be able to accurately find the centre of the earth. She worked in Poltava Observatory. She became observatory director in 1951. Her areas of study were tidal deformation of the earth and gravimeter Earth profiles. She has a crater on Venus that is named in her honour. Aksentieva died in 1969 in Poltava where her observatory was. | https://en.wikipedia.org/wiki?curid=45339895 |
Neupert effect The refers to an empirical tendency for high-energy ('hard') X-ray emission to coincide temporally with the rate of rise of lower-energy ('soft') X-ray emission of a solar flare. Here 'hard' and 'soft' mean above and below an energy of about 10 keV to solar physicists, though in non-solar X-ray astronomy one typically sets this boundary at a lower energy. This effect gets its name from NASA solar physicist and spectroscopist Werner Neupert, who first documented a related correlation (the integral form) between microwave (gyrosynchrotron) and soft X-ray emissions in 1968. The standard interpretation is that the accumulated energy injection associated with the acceleration of non-thermal electrons (which produce the hard X-rays via non-thermal bremsstrahlung) release energy in the lower solar atmosphere (the chromosphere); this energy then leads to thermal (soft X-ray) emission as the chromospheric plasma heats and expands into the corona. The effect is very common, but does not represent an exact relationship and is not observed in all solar flares. | https://en.wikipedia.org/wiki?curid=45342879 |
Ukureyskaya Formation The Ukureyskaya Formation, also referred to as the Ukurey Formation is a geological formation made up of Middle Jurassic and Late Jurassic layers. It covers large areas around Kulinda. The formation is where the type specimen fossils of "Kulindadromeus zabaikalicus" were found, alongside a single tooth from a medium-sized theropod of unknown affiliations and other indeterminate ornithschians. Recent dating work suggest that the layers containing "Kulindadromeus" are Bathonian in age. | https://en.wikipedia.org/wiki?curid=45358785 |
Smith (Martian crater) Smith is an impact crater on Mars, located in the Mare Australe quadrangle at 66.1°S latitude and 102.9°W longitude. It measures 74.33 kilometers in diameter and was named after English geologist William Smith (1769–1839). The name was approved in 1973, by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature. | https://en.wikipedia.org/wiki?curid=45361974 |
Heaviside (Martian crater) Heaviside is an impact crater in the Mare Australe quadrangle of Mars, located at 70.7°S latitude and 95.3°W longitude. It is 87.4 km in diameter. It was named after British physicist Oliver Heaviside; the name was approved in 1973 by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature (WGPSN). | https://en.wikipedia.org/wiki?curid=45362055 |
Mitchel (crater) Mitchel is an impact crater in the Mare Australe quadrangle of Mars, located at 67.7°S latitude and 76.0°E longitude. It is 138.4 kilometers in diameter. Its name refers to Ormsby M. Mitchel, an American astronomer and major general in the American Civil War. | https://en.wikipedia.org/wiki?curid=45374089 |
Holmes (crater) Holmes is an impact crater in the Mare Australe quadrangle of Mars, located at 75.0°S latitude and 293.2°W longitude. It is 122.0 km in diameter and was named after Arthur Holmes, and the name was approved in 1973 by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature (WGPSN). | https://en.wikipedia.org/wiki?curid=45374332 |
Jeans (Martian crater) Jeans is an impact crater in the Mare Australe quadrangle of Mars, located at 69.8°S latitude and 205.9°W longitude. It is 80.2 km in diameter and was named after James Hopwood Jeans, and the name was approved in 1973 by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature (WGPSN). The pictures below show dark areas in which frost is disappearing and the dark ground beneath is being exposed. Layers are also visible—probably from the many cycles of mantle deposition. | https://en.wikipedia.org/wiki?curid=45376448 |
Steno (Martian crater) Steno is an impact crater on Mars, located in the Mare Australe quadrangle at 68.0°S latitude and 115.6°W longitude. It measures 106.9 kilometers in diameter and was named after Danish scientist Nicolas Steno (1638–1686). The name was approved in 1973, by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature. | https://en.wikipedia.org/wiki?curid=45382178 |
Teri (geology) Teri or Teri dune complex is a coastal landscape peculiar to some parts of Tamil Nadu mainly in southeastern India. The landscape consists of sediments dating to the Quaternary Period and made of marine deposits with aeolianite and characteristic red sand and silt dunes. These red soils are thought to have originated in the Pleistocene. Robert Bruce Foote hypothesized that these dunes were created by the action of winds (aeolian) lifing the fine silt fraction from further east. These dunes are oriented along the axis running parallel to the coast and between the latitudes of 8°00′ to 9°30′ N and longitudes 77°18′ to 79°00′ E. The soils also have calcium deposits replacing the old roots of vegetation. The soil is rich in ilmenite and the red colour is derived from haematite originating from garnet. | https://en.wikipedia.org/wiki?curid=45388637 |
Suess (Martian crater) Suess is an impact crater in the Mare Australe quadrangle of Mars, located at 67.1°S latitude and 178.6°W longitude. It measures 71.9 kilometers in diameter and was named after Austrian geologist Eduard Suess. The name was approved in 1973, by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature. | https://en.wikipedia.org/wiki?curid=45400454 |
Stoney (Martian crater) Stoney is an impact crater in the Mare Australe quadrangle of Mars, located at 69.8°S latitude and 138.6°W longitude. It measures 161.37 kilometers in diameter and was named after Anglo-Irish physicist George Johnstone Stoney (1826–1911). The name was officially adopted by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature in 1973. | https://en.wikipedia.org/wiki?curid=45400483 |
Weinbaum (crater) Weinbaum is an impact crater in the Mare Australe quadrangle of Mars, located at 65.5°S latitude and 245.4°W longitude. It measures 82 kilometers in diameter and was named after American science fiction writer Stanley Weinbaum (1902–1935). The name was adopted in 1973 by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature. | https://en.wikipedia.org/wiki?curid=45400739 |
Liais (crater) Liais is an impact crater in the Mare Australe quadrangle of Mars, located at 75.4°S latitude and 252.8°W longitude. It measures 132.0 kilometers in diameter and was named after Emmanuel Liais. The name was approved in 1973, by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature (WGPSN). Liais Crater displays layers on its floor. Many places on Mars show rocks arranged in layers. The study of layering on Mars greatly expanded when the Mars Global Surveyor sent back images. Rock can form layers in a variety of ways. Volcanoes, wind, or water can produce layers. A detailed discussion of layering with many Martian examples can be found in Sedimentary Geology of Mars. A paper by Grotzinger and Milliken discusses the role of water and wind in forming layers of sedimentary rocks. | https://en.wikipedia.org/wiki?curid=45400800 |
Scale (chemistry) The scale of a chemical process refers to the rough ranges in mass or volume of a chemical reaction or process that define the appropriate category of chemical apparatus and equipment required to accomplish it, and the concepts, priorities, and economies that operate at each. While the specific terms used—and limits of mass or volume that apply to them—can vary between specific industries, the concepts are used broadly across industry and the fundamental scientific fields that support them. Use of the term "scale" is unrelated to the concept of weighing; rather it is related to cognate terms in mathematics (e.g., geometric scaling, the linear transformation that enlarges or shrinks objects, and scale parameters in probability theory), and in applied areas (e.g., in the scaling of images in architecture, engineering, cartography, etc.). Practically speaking, the scale of chemical operations also relates to the training required to carry them out, and can be broken out roughly as follows: For instance, the production of the streptomycin-class of antibiotics, which combined biotechnologic and chemical operations, involved use of a 130,000 liter fermenter, an operational scale approximately one million-fold larger than the microbial shake flasks used in the early laboratory scale studies. As noted, nomenclature can vary between manufacturing sectors; some industries use the scale terms "pilot plant" and "demonstration plant" interchangeably | https://en.wikipedia.org/wiki?curid=45413683 |
Scale (chemistry) Apart from defining the category of chemical apparatus and equipment required at each scale, the concepts, priorities and economies that obtain, and the skill-sets needed by the practicing scientists at each, defining scale allows for theoretical work prior to actual plant operations (e.g., defining relevant process parameters used in the numerical simulation of large-scale production processes), and allows economic analyses that ultimately define how manufacturing will proceed. Besides the chemistry and biology expertises involved in scaling designs and decisions, varied aspects of process engineering and mathematical modeling, simulations, and operations research are involved. | https://en.wikipedia.org/wiki?curid=45413683 |
NGC 1398 is an isolated barred spiral galaxy exhibiting a double ring structure. It is located 65 million light years from the Earth, in the constellation of Fornax. The galaxy, with a diameter of 135,000 light years, is slightly larger than the Milky Way. Over 100 billion stars are in the galaxy. It was first discovered by Friedrich Winnecke of Karlsruhe, Germany, on 17 December 1868, while he was searching for comets. | https://en.wikipedia.org/wiki?curid=45423814 |
NGC 695 is a spiral galaxy located 450 million light years from the Earth, in the constellation of Aries. It has been described as an abnormal galaxy, and has the appearance of "a revolving tornado". Its arms are not tightly held together, and it is interacting with another small astronomical object. | https://en.wikipedia.org/wiki?curid=45429453 |
NGC 6786 is an interacting spiral galaxy 350 million light years from the Earth, in the constellation of Draco. In 2004, a supernova occurred inside the galaxy. is currently interacting with LEDA 62867, and, being the larger galaxy, it is likely that will absorb LEDA 62867 in the future. Both galaxies appear to be undergoing a starburst, a phenomenon commonly seen among interacting and merging galaxies. | https://en.wikipedia.org/wiki?curid=45437549 |
NGC 6090 is a merging pair of spiral galaxies, 400 million light-years from the Earth, in the constellation of Draco. The cores of the two galaxies are around 10,000 light-years apart from each other, meaning that the merger is likely at its intermediate stage. Two large "tails", made of galactic material gravitationally ejected during the merger, have formed outside the main galaxies. Newly formed stars can be seen in the overlapping area. | https://en.wikipedia.org/wiki?curid=45437874 |
Adolphe Hercule de Graslin (11 April 1802, Chateaux de Malitourne, Flée, Sarthe – 31 May 1882, Malitourne) was a French entomologist. specialised in Lepidoptera. He was a founding member of the Société Entomologique de France. His collection was acquired by Charles Oberthür. With Jean Alphonse Boisduval and Jules Pierre Rambur, he wrote "Collection iconographique et historique des chenilles; ou, Description et figures des chenilles d'Europe, avec l'histoire de leurs métamorphoses, et des applications à l'agriculture", Paris, Librairie encyclopédique de Roret, 1832. | https://en.wikipedia.org/wiki?curid=45449734 |
Jules Ferdinand Fallou (9 August 1812, in Paris – 19 June 1895, in Paris) was a French entomologist who specialised in Lepidoptera and Coleoptera. Jules Fallou was a manufacturer of surgical instruments. His collection of European Lepidoptera, mostly from France and Switzerland is held by Muséum national d'histoire naturelle in Paris. He was a Member of the Société entomologique de France. Descriptive papers in "Annales de la Société Entomologique de France". | https://en.wikipedia.org/wiki?curid=45455924 |
Constant Bar (14 October 1817, Nantes – June 1884, Paramaribo) was a French entomologist. lived in French Guiana at L'île Portal in the commune of Saint-Laurent-du-Maroni and with his three brothers made extensive entomological explorations of that region, collecting specimens for his own studies and for Charles Oberthür and others. He wrote "Note critique sur les différent systèmes de classification des lépidoptères rhopalocères établis depuis l'époque de Latreille et essai d'une nouvelle classification jusqu'aux genres exclusivement" for the "Annales de la Societé entomologique de France" in 1878. In 1854 he became a member of the Société entomologique de France. He is honoured in the names "Hypercompe bari", "Heliconia bari" and "Parides lysander bari". | https://en.wikipedia.org/wiki?curid=45457517 |
Antoine Barthélemy Jean Guillemot (11 November 1822, Thiers – 25 August 1902, Thiers) was a French entomologist . He wrote "Catalogue des lépidoptères du Département du Puy-de-Dome" Clermont-Ferrand, Impr. de Thibaud-Landriot published in 1854 online at BHL Antoine Guillemot was a member of the Société entomologique de France. Charles Oberthür, 1904 "Etudes de lépidoptérologie comparée" Impr. Oberthür in Rennes . | https://en.wikipedia.org/wiki?curid=45458751 |
Tombaugh (crater) Tombaugh is an impact crater on Mars, located in the Elysium quadrangle at 3.5°N latitude and 198.2°W longitude. It measures 60.3 kilometers in diameter and was named after Clyde Tombaugh, American astronomer (1906–1997). The name was approved in 2006, by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature. | https://en.wikipedia.org/wiki?curid=45460170 |
DRIP-seq (DRIP-sequencing) is a technology for genome-wide profiling of a type of DNA-RNA hybrid called an "R-loop". utilizes a sequence-independent but structure-specific antibody for DNA-RNA immunoprecipitation (DRIP) to capture R-loops for massively parallel DNA sequencing. An R-loop is a three-stranded nucleic acid structure, which consists of a DNA-RNA hybrid duplex and a displaced single stranded DNA (ssDNA). R-loops are predominantly formed in cytosine-rich genomic regions during transcription and are known to be involved with gene expression and immunoglobulin class switching. They have been found in a variety of species, ranging from bacteria to mammals. They are preferentially localized at CpG island promoters in human cells and highly transcribed regions in yeast. Under abnormal conditions, namely elevated production of DNA-RNA hybrids, R-loops can cause genome instability by exposing single-stranded DNA to endogenous damages exerted by the action of enzymes such as AID and APOBEC, or overexposure to chemically reactive species. Therefore, understanding where and in what circumstances R-loops are formed across the genome is crucial for the better understanding of genome instability. R-loop characterization was initially limited to locus specific approaches. However, upon the arrival of massive parallel sequencing technologies and thereafter derivatives like DRIP-seq, the possibility to investigate entire genomes for R-loops has opened up. relies on the high specificity and affinity of the S9 | https://en.wikipedia.org/wiki?curid=45461558 |
DRIP-seq 6 monoclonal antibody (mAb) towards DNA-RNA hybrids of various lengths. S9.6 mAb was first created and characterized in 1986 and is currently used for the selective immunoprecipitation of R-loops. Since then, it was used in diverse immunoprecipitation methods for R-loop characterization. The concept behind is similar to ChIP-sequencing; R-loop fragments are the main immunoprecipitated material in DRIP-seq. is mainly used for genome-wide mapping of R-loops. Identifying R-loop formation sites allows the study of diverse cellular events, such as the function of R-loop formation at specific regions, the characterization of these regions, and the impact on gene expression. It can also be used to study the influence of R-loops in other processes like DNA replication and synthesis. Indirectly, can be performed on mutant cell lines deficient in genes involved in R-loop resolution. These types of studies provide information about the roles of the mutated gene in suppressing DNA-RNA formation and potentially about the significance of R-loops in genome instability. was first used for genome-wide profiling of R-loops in humans, which showed widespread R-loop formation at CpG island promoters. Particularly, the researchers found that R-loop formation is associated with the unmethylated state of CpG islands. was later used to profile R-loop formation at transcription start and termination sites in human pluripotent Ntera2 cells | https://en.wikipedia.org/wiki?curid=45461558 |
DRIP-seq In this study, the researchers revealed that R-loops on 3' ends of genes may be correlated with transcription termination. First, genomic DNA (gDNA) is extracted from cells of interest by proteinase K treatment followed by phenol-chloroform extraction and ethanol precipitation. Additional zymolyase digestion is necessary for yeast cells to remove the cell wall prior to proteinase K treatment. gDNA can also be extracted with a variety of other methods, such as column-based methods. gDNA is treated with S1 nuclease to remove undesired ssDNA and RNA, followed by ethanol precipitation to remove the S1 nuclease. Then, gDNA is fragmented with restriction endonuclease, yielding double-stranded DNA (dsDNA) fragments of different sizes. Alternatively, gDNA fragments can be generated by sonication. Fragmented gDNA is incubated with the DNA-RNA structure-specific S9.6 mAb. This step is unique for the protocol, since it entirely relies on the high specificity and affinity of the S9.6 mAb for DNA-RNA hybrids. The antibody will recognize and bind these regions dispersed across the genome and will be used for immunoprecipitation. The S9.6 antibodies are bound to magnetic beads by interacting with specific ligands (i.e. protein A or protein G) on the surface of the beads. Thus, the DNA-RNA containing fragments will bind to the beads by means of the antibody. The magnetic beads are washed to remove any gDNA not bound to the beads by a series of washes and DNA-RNA hybrids are recovered by elution | https://en.wikipedia.org/wiki?curid=45461558 |
DRIP-seq To remove the antibody bound to the nucleic acid hybrids, proteinase K treatment is performed followed by phenol-chloroform extraction and ethanol precipitation. This results in the isolation of purified DNA-RNA hybrids of different sizes. For massive parallel sequencing of these fragments, the immunoprecipitated material is sonicated, size selected and ligated to barcoded oligonucleotide adaptors for cluster enrichment and sequencing. To detect sites of R-loop formation, the hundreds of millions of sequencing reads from are first aligned to a reference genome with a short-read sequence aligner, then peak calling methods designed for ChIP-seq can be used to evaluate DRIP signals. If different cocktails of restriction enzymes were used for different experiments of the same sample, consensus peaks are called. Typically, peaks are compared against those from a corresponding RNase H1-treated sample, which serves as an input control. Due to the absence of another antibody-based method for R-loop immunoprecipitation, validation of results is difficult. However, results of other R-loop profiling methods, such as DRIVE-seq, may be used to measure consensus. On the other hand, relies on existing short-read sequencing platforms for the sequencing of R-loops. In other words, all inherent limitations of these platform also apply to DRIP-seq. In particular, typical short-read sequencing platforms would produce uneven read coverage in GC-rich regions | https://en.wikipedia.org/wiki?curid=45461558 |
DRIP-seq Sequencing long R-loops might pose a challenge because R-loops are predominantly formed in cytosine-rich DNA regions. Moreover, GC-rich regions tend to have low complexity by nature, which is difficult for short read aligners to produce unique alignments. Although there are several other methods for analysis and profiling of R-loop formation, only few provide coverage and robustness at the genome-wide scale. | https://en.wikipedia.org/wiki?curid=45461558 |
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