the-french-artist/wikipedia_20220301.simple_sentence_embeddings huggingface dataset:
Radcliffe Line 
 The line was decided by the Border Commissions headed by Sir Cyril Radcliffe, who was to divide equitably  of territory with 88 million people.
Radcliffe Line 
 The Chittagong Hill Tracts had a moslty Buddhist population, but they were given to East Pakistan (now Bangladesh).
Radcliffe Line 
 To counterbalance the relatively small share of Gurdaspur district awarded to Pakistan, Radcliffe attempted to instead transfer Ferozpur and Zira tehsils in Muslim-Majority Ferozpur District to Pakistan.
Radcliffe Line 
 This was opposed by the Maharaja of Bikaner because Harike headworks on the confluence of the Sutlej and the Beas rivers, from where a canal originated, was the only source of water for his desert state was in Ferozepore.
Radcliffe Line 
 It was only after he threatened Lord Louis Mountbatten, that he would accede his princely state to Pakistan if Firozpur was awarded to West Punjab province, that the award was changed at the last minute and all of Firozpur District was awarded to East Punjab in the Republic of India.
Radcliffe Line 
 At other instances, it went through houses, different rooms of the same house were in different countries.
Dipsacales 
 Under the APG II definition some well-known members of Dipsacales are honeysuckle, elder, viburnum, and valerian.
Planetary nebula 
 At the end of a normal-sized star's life, in the red giant phase, the outside layers of a star are ejected.
Planetary nebula 
 The ultraviolet radiation given off by the center of the star ionizes the gas and plasma that was thrown out from the star.
Planetary nebula 
 Scientists think that binary stars, stellar winds and magnetic fields might be some of the reasons planetary nebulae can look so varied.
Planetary nebula 
 In the early 21st century some astronomers began calling them “globular nebulas” to avoid confusing them with the Protoplanetary nebulas that make planets.
Planetary nebula 
 Astronomers did not know what these objects were until the first spectroscopic experiments were done in the 1800's.
Planetary nebula 
 Later, physicists showed that it is possible for gasses with a very low density to look like something else.
Planetary nebula 
 This meant that they were caused by a star's outer layers being thrown into space at the end of its life.
Planetary nebula 
 When it runs out of hydrogen, the smaller core will cause it to rise to about 100 million degrees Kelvin.
Planetary nebula 
 The outer layers of the star become much bigger because of the heat of the core, and become much cooler.
Planetary nebula 
 Helium burning soon forms a core of carbon and oxygen, with both a helium and a hydrogen shell surrounding it.
Planetary nebula 
 Because helium in fusion reactions is not very stable, the core starts to grow and shrink very quickly.
Planetary nebula 
 As more and more of the gas moves away from the star, deeper and deeper layers at higher and higher temperatures are sent out.
Planetary nebula 
 We know of about 3,000 of these nebulae in our galaxy, compared to 200 billion stars.<ref>Parker Q.A. et al.
Planetary nebula 
 The Macquarie/AAO/Strasbourg H-alpha Planetary Nebulae Catalogue: MASH, MNRAS 373, 79</ref> Their very short lifetime compared to a star is why there are not that many compared to stars.
Planetary nebula 
 They are found mostly in the plane of the Milky Way, and there are more and more the closer you get to the center of the Milky Way.
Planetary nebula 
 It may be because of the gravitational pull of secondary stars (for example, if it is a binary star system).
Planetary nebula 
 A problem in studying planetary nebulae is that astronomers can not always work out how far away they are.
Planetary nebula 
 When they are close, astronomers use something called expansion parallax'' to  estimate how far away they are, but this takes a long time.
Emission nebula 
 If the nebula is very hot, other types of gas will be heated and the it might also glow blue and green.
Emission nebula 
 This is because clouds of dust block the light when it is traveling between the nebula and the Earth.
Reflection nebula 
 In astronomy, a reflection nebula is a cloud of dust which reflects the light of a star or many stars.
Reflection nebula 
 The light from the nearby stars is not hot enough to ionize the gas of the nebula to make an emission nebula.
Reflection nebula 
 Reflection nebulae are usually blue because the scattering works better for blue light than red (this is the same reason that the sky is blue and sunsets are red).
Reflection nebula 
 Reflection nebulae and emission nebulae are usually seen together and sometimes are called 'diffuse nebulae'.
Variable nebula 
 A Variable nebula is a reflection nebula that gets brighter and darker because of changes in its star.
Ionization 
 In the process of ionization, an electrically neutral atom becomes either positively or negatively charged.
Nucleosynthesis 
 This usually happens in the center of a star, both during its life and especially during its violent death.
Stellar wind 
 Most stars, especially very bright ones, show continuous outflows of gas from their surfaces making the stellar wind.
Stellar wind 
 Radiation pressure is thought to be the main force that pushes the gas away, but modern research uses computer simulations and observations with the most powerful telescopes to understand it further.
Dumbbell nebula 
 The Dumbbell nebula (sometimes called Messier 27, M 27, or NGC 6853) is a planetary nebula in the constellation Vulpecula.
Charles Messier 
 Charles Messier (June 26, 1730 – April 12, 1817) was a French astronomer who is remembered for publishing a list of famous objects in space that came to be called the 103 "Messier objects".
Charles Messier 
 Charles became interested in astronomy after he saw the great six-tailed comet in 1744 and by a solar eclipse on July 25, 1748.
Charles Messier 
 In 1751 he started working for Joseph Nicolas Delisle, the astronomer of the French Navy, who told him to write down everything he saw.
Astronomical spectroscopy 
 Astronomical spectroscopy is the science of using spectroscopy to figure out what elements astronomical bodies, such as stars, planets and nebulae, are made of.
Astronomical spectroscopy 
 The study of spectroscopy and spectra is used in astronomy to help scientists study the whole spectrum of electromagnetic radiation, including visible light, which radiates from stars and other hot celestial objects.
Astronomical spectroscopy 
 It can find out their chemical composition, temperature, density, mass, distance, luminosity, and relative motion using doppler effect measurements.
Astronomical spectroscopy 
 Isaac Newton used a prism to split white light into a spectrum of color, and Fraunhofer's high-quality prisms allowed scientists to see dark lines of an unknown origin.
Astronomical spectroscopy 
 Hot solid objects produce light with a continuous spectrum, and hot gasses emit light at specific wavelengths.
Astronomical spectroscopy 
 However, hot solid objects surrounded by cooler gasses show a near-continuous spectrum with dark lines corresponding to the emission lines of the gasses.
William Huggins 
 Sir William Huggins, KCB, OM, FRS, (7 February 1824–12 May 1910) was an English astronomer best known for his work in astronomical spectroscopy.
William Huggins 
 Huggins built his own observatory from where he and his wife looked at spectral emission lines and absorption lines of astronomical objects.
Emission spectrum 
 The emission spectrum of an element or compound is how bright certain frequencies are when energy is added to the atoms or molecules.
Emission spectrum 
 Each atom's emission spectrum has different spectral lines and can be used to figure out if that atom is part of a compound
Luminosity 
 Apparent magnitude is contrasted with absolute magnitude, which is an object's intrinsic brightness at visible wavelengths, irrespective of distance.
Luminosity 
 When talking about the total power output across all wavelengths, that is called bolometric magnitude.
Solar mass 
 It is equal to the mass of the Sun, about 332,950 times the mass of the Earth, or 1,048 times the mass of Jupiter.
Interstellar medium 
 In astronomy, the interstellar medium (sometimes called the ISM) is the tenuous gas and dust that fills the void between stellar systems in galaxies, that consisting mainly of huge clouds of ionized, neutral, or molecular hydrogen.
Interstellar medium 
 This gas and dust not distributed uniformly in interstellar space, but displays significant variations in density, temperature, and ionisation state.
Myopia 
 Myopia, also called near-sightedness or short-sightedness, is a problem with the focusing ability of the eye.
Myopia 
 It happens when the lens becomes a different shape (too curved) from usual, or when the eye is longer than normal, so light entering the eye focuses on a point in front of the retina, rather than right on it.
Luster (mineralogy) 
 Luster (or lustre) is a description of the way light interacts with the surface of a crystal, rock, or mineral.
Luster (mineralogy) 
 The term is also used to describe other items with some kind of sheen (for example, fabric, especially silk and satin, or metals).
Luster (mineralogy) 
 The word lustre comes from the Latin word lux, meaning "light", and generally implies radiance, gloss, or brilliance.
Carbonation 
 For example, carbon dioxide is added to flavored water under pressure to make it "fizz" as a carbonated water soft drink.
Carbonation 
 When rain passes through the atmosphere, it takes in or mixes with carbon dioxide, turning it into a weak carbonic acid.
Carbonation 
 When the rain falls in limestone, it dissolves the calcium carbonate in the rock, turning it into calcium bicarbonate and taking it away.
Carbonation 
 The process of carbon dioxide bubbling out (effervescing) from a solution is represented by the following chemical reaction.
Carbonation 
 Carbon-based life originates from a carbonation reaction that is most often catalysed by the enzyme RuBisCO.
Carbonation 
 This carbonation process is so important that a significant fraction of leaf mass consists of this carbonating enzyme.
Feynman diagram 
 A Feynman diagram has lines in different shapes—straight, dotted, and squiggly—which meet up at points called vertices.
Feynman diagram 
 The points in Feynman diagrams where the lines meet represent two or more particles that happen to be at the same point in space at the same time.
Feynman diagram 
 The lines in a Feynman diagram represent the probability amplitude for a particle to go from one place to another.
Feynman diagram 
 The meeting points for the lines can also be interpreted forward or backwards in time, so that if a particle disappears into a meeting point, that means that the particle was either created or destroyed, depending on the direction in time that the particle came in from.
Feynman diagram 
 When you multiply the probability amplitude for the lines, the amplitude for the particles to go from wherever they start to wherever they meet, and to the next meeting point, and so on, and also multiply by the amplitude for each meeting point, you get a number that tells you the total amplitude for the particles to do what the diagram says they do.
Feynman diagram 
 If you add up all these probability amplitudes over all the possible meeting points, and over all the starting and ending points with an appropriate weight, you get the total probability amplitude for a collision in a particle accelerator, which tells you the total probability of these particles to bounce off one another in any particular direction.
Feynman diagram 
 His diagrams are very simple in the case of quantum electrodynamics (QED), where there are only two kinds of particles: electrons (little particles inside atoms) and photons (particles of light).
Feynman diagram 
 In QED, the only thing that can happen is that an electron (or its antiparticle) can emit (or absorb) a photon, so there is only one building block for any collision.
Feynman diagram 
 The probability amplitude for the emission is very simple—it has no real part, and the imaginary part is the charge of the electron.
Raymond VII, Count of Toulouse 
 Raymond VII of Saint-Gilles (July 1197 – 27 September 1249) was Count of Toulouse, Duke of Narbonne and Marquis of Provence from 1222 until his death.
Raymond VII, Count of Toulouse 
 During the Albigensian Crusade in May of 1216, he set out from Marseille and besieged Beaucaire, which he captured on August 24.
Raymond VII, Count of Toulouse 
 He fought to get the county of Toulouse back from Simon de Montfort, 5th Earl of Leicester and later Simon's son Amaury VI of Montfort.
Raymond VII, Count of Toulouse 
 When Raymond died, Alphonse became count of Toulouse, and after Alphonse's death the county was captured by France.
Rival 
 A rival is a  person or group of people who are trying to do the same thing as someone else, and trying to do it better.
Seneschal 
 In the French administrative system of the Middle Ages, the sénéchal was also a royal officer in charge of justice and control of the administration in southern provinces, equal to the northern French bailli.
Seneschal 
 Grand maître de France - the Great Officer of the Crown of France in charge of the Royal Household (the "Maison du Roi")
Stoke 
 Originally from the Old English  'stoc' meaning 'place', it came to be used in two special senses, i) a religious place and ii) a secondary settlement (see Roome )
Bon Scott 
 He was the lead singer of hard rock band AC/DC from 1974 until he died of alcohol poisoning in 1980.
Bon Scott 
 Their next albums were Let There Be Rock, Powerage, and a live album called If You Want Blood You've Got It.
Hubble Deep Field 
 The image was taken in the direction of the constellation Ursa Major by the Hubble Space Telescope in 1995.
Hubble Deep Field 
 It is important because it shows some of the earliest (farthest away) galaxies ever seen, over 3000 in total.
Hubble Deep Field 
 The area of the sky the HDF was taken in makes up less than 1/10th the width of a full Moon, yet it contains over 3,000 galaxies.
Hubble Deep Field 
 Because of the time it takes for light from these galaxies to reach Earth, many in the picture look exactly as they did over 10 billion (10,000,000,000) years ago.
Hubble Deep Field 
 Because of this it allows scientists to look at what the Universe was like at that time, and how it changed to become what it is now.
Hubble Deep Field 
 Add to this the cosmological principle, which suggests that on large scales the Universe is roughly the same no matter what direction you look, and the HDF becomes a very important tool for astronomers studying how the Universe has changed.
Ranunculaceae 
 Ranunculaceae is a family of flowering plants also known as the "buttercup family" or "crowfoot family".
Interlingue 
 De Wahl was from the city of Tallinn in Estonia, which was in the Russian Empire but later became its own country.
Interlingue 
 He spoke German, Russian, Estonian and French since he was a child and had natural ability in languages.
Interlingue 
 Interlingue looks a lot like languages in the Romance language family: French, Spanish, Italian, and so on.
Interlingue 
 De Wahl made a rule called De Wahl's rule that made changing verbs to nouns easier and more regular.
Interlingue 
 For example, the change of d in the word exploder (to explode) to s (making explosion and explosiv) is a regular change when following this rule.
Interlingue 
 Some of them, like Esperanto and Ido, are called schematic because they follow their own design even if the words look more artificial.
Interlingue 
 Others, like Latino sine flexione and Idiom Neutral, are called naturalistic because they try to look like natural languages.
Interlingue 
 Louis Couturat, the creator of Ido, wrote the same thing in 1903, and called it a paradox: "The international words are not regular, and the regular words are not international."
Interlingue 
 The language that de Wahl made had a goal to be a language that was both regular and natural at the same time.
Interlingue 
 De Wahl announced his language in the magazine Kosmoglott in 1922, and this is where the Occidental activities can be seen.
Interlingue 
 He actually wanted to wait a bit longer, but there was big news in 1921: the League of Nations was looking at the idea of an international language.
Interlingue 
 De Wahl had also sent a letter and got a positive reply from the League of Nations in September 1921.
Interlingue 
 People began using Occidental because it was easy to read and understand, even without grammars and dictionaries.
Interlingue 
 Kosmoglott changed its name to Cosmoglotta in 1927 and began promoting Occidental over other languages.
Interlingue 
 In January of the same year, they moved Cosmoglotta's office to Vienna in the region of Mauer (now part of Liesing).
Interlingue 
 This helped Occidental have success during this period because the office was now in a central location.
Interlingue 
 Engelbert Pigal, who is also from Austria, helped too with his article Li Ovre de Edgar de Wahl (The Work of Edgar de Wahl) which convinced some users of the Ido language to try Occidental.
Interlingue 
 By early 1930, people were using Occidental in Germany, Austria, Sweden, Czechoslovakia, Switzerland, and most recently in France.
Interlingue 
 When the magazine Cosmoglotta was based in Vienna, the users of the language had enough money for the first time.
Interlingue 
 The world economy was not doing well at this time, but with the help of people like Hörbiger and Moore, Cosmoglotta was able to do well and gained readers.
Interlingue 
 After this Cosmoglotta had to find money from other places: subscriptions, books, magazines, and so on.
Interlingue 
 The growing movement began a stronger campaign for the language in the early 1930s in which it promoted Occidental's easy understanding at first sight.
Interlingue 
 They contacted organizations with letters completely in Occidental, and these organizations often understood the letters and sent responses.
Interlingue 
 The Occidentalists also introduced the idea of Occidental being the answer to Europe's "tower of Babel".
Interlingue 
 The second edition first had the name Cosmoglotta-Informationes, but was soon called Cosmoglotta B. Cosmoglotta B had more discussions that were interesting to the users of Occidental such as the language's development, Occidental in the news, and how much money they had.
Interlingue 
 Meanwhile, the years before the World War II led to problems for Occidental and other planned languages because they were made illegal in Germany, Austria and Czechoslovakia.
Interlingue 
 Their groups were forced to break up, the Gestapo watched their activities, and their educational materials were destroyed.
Interlingue 
 Germany had the largest number of Occidentalists, so making planned languages illegal in Germany was especially damaging.
Interlingue 
 World War Two suddenly started in 1939, and this stopped the publications of both Cosmoglottas until 1940.
Interlingue 
 One Cosmoglotta A or B was published every month between January 1937 and September 1939 when the war started.
Interlingue 
 The Occidentalists noticed that their telegrams were being sent, especially between Switzerland and Sweden.
Interlingue 
 This meant that the censors could probably understand it and maybe thought the language was Spanish or Romansch.
Interlingue 
 Cosmoglotta had subscribers in 58 cities in Switzerland a few months before the end of World War II in Europe, and Cosmoglotta A started again in 1946.
Interlingue 
 De Wahl had created Occidental with some unchangeable features, but believed that it could follow a "natural evolution".
Interlingue 
 Orthography was another area in which several possibilities existed: etymologic orthography (adtractiv, obpression), historic orthography (attractiv, oppression), or simplified orthography (atractiv, opression).
Interlingue 
 Much of the standardization of the language took place in this way through community preference (e.g. both ac and anc were proposed for the word "also" but the community quickly settled on anc), but not all.
Interlingue 
 As there was a lack of general material destined for the general public, much time during World War II was spend creating courses and standardizing the language.
Interlingue 
 In August 1943, as the war was still going on, it was decided to create an academy to officialize the process.
Interlingue 
 The Swiss Occidentalist, isolated from the rest of the continent, concentrated on developing educational materials.
Interlingue 
 The International Auxiliary Language Association (IALA), founded in 1924 to study and decide the best planned language for international communication, was at first viewed with disbelief by the Occidental community.
Interlingue 
 This made many Occidentalists including de Wahl himself believed that it had been set up as a pretext to give the impressoin of a "neutral and professional" committee that would finally choose Esperanto.
Interlingue 
 Relations soon improved, however, as it became clear that the IALA intended to be as impartial as possible by familiarizing itself with all existing planned languages.
Interlingue 
 Some Occidentalists were happy that the IALA had decided to create a language almost the same as Occidental.
Interlingue 
 The two languages had somewhat different spellings (e.g. filosofie in Occidental and philosophia in Interlingua for 'philosophy'), but besides this both languages had 90% the same vocabulary.
Interlingue 
 De Wahl's Rule in Occidental had eliminated Latin double stem verbs (verbs such as act: ager, act- or send: mitter, miss-), while Interlingua simply accepted them as an important part of a naturalistic system.
Interlingue 
 Interlingua also allowed optional irregular verbal conjugations (such as so, son and sia as the first-person singular, third-person plural and subjunctive form of esser, the verb 'to be') that Occidental had never even considered and viewed as incompatible with an easy international auxiliary language.
Interlingue 
 Besides the economic difficulties that the movement was suffering (not like the well-funded IALA, which was based in New York), the beginning of the Cold War created a difficult situation for the Occidental-Union, which had the same name as an anti-Russian political league.
Interlingue 
 In early 1948 the Czechoslovak Occidentalists had begun asking for the approval for a new name that would allow them to continue their linguistic activities without problems.
Interlingue 
 The Union responded that they were free to introduce the language as "Interlingue (Occidental)", or even remove the mention of Occidental if they felt it necessary.
Interlingue 
 Ric Berger began supporting a change of name from Occidental to Interlingue in 1948 which he also hoped would help in uniting it with Interlingua.
Interlingue 
 With a 91% support in a ballot done by the Occidental Union in 1949, Interlingue was made the official name of the language, with Interlingue (Occidental) also permitted, valid as of 1 September 1949.
Interlingue 
 In fact, Ric Berger, one of the most important Occidentalists, stopped supporting Interlingue to support IALA's project.
Interlingue 
 Interlingue was quite weakened after many users moved to Interlingua, though the drop in activity was gradual and happened over decades.
Interlingue 
 Barandovská-Frank believed that the decrease of interest in Occidental-Interlingue happened at the same time as generation that was first drawn to it from other planned languages was getting older (translated from Esperanto):Most of those interested in Interlingue belonged to the generation that became familiar in turn with Volapük, Esperanto and Ido, later on finding the most aesthetic (basically naturalistic) solution in Occidental-Interlingue.
Interlingue 
 After that, many moved to IALA's Interlingua, which however did not prove to be much more successful despite the impression its scientific origin made, and those who remained loyal to Occidental-Interlingue did not succeed in giving their excitement to a new generation.
Interlingue 
 Activity in Interlingue eventually reached a low during the 1980s and early 1990s, when Cosmoglotta publication stopped for a some years.