How was nitrogen discovered?
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All you need to know (probably).
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nitrogen+hydrogen=ammonia\n               N2+ 3H2=2NH3\nthis is called the "Haber Process".the raw materials used for the process are: \n1)air-which supplies nitrogen\n2)natural gas(methane)-which is reacted with steam to produce hydrogen & is also used as the heating fuel for the system\n3)iron-which is used in a finely divided form as the catalyst\n\nuses of ammonia:\n1)fertilisers -75%\n2)nitric acid -10%\n3)nylon -5%\n4)others -10%\n\nproperties of ammonia:\n1)colourless gas\n2)distinctive smell\n3)less dense than air\n4)very soluble in water to give an alkaline solution\n\nhope that helped-cheers!
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Go to google or wikipidia and type in nitrogen regulators and tons of available info will pop up.....word....take care and good luck
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It's not nitrogen... It's hydrogen. They called my car the "Hindenburg" after it burst into flames when I pumped in a few pounds too many way back when in Lakehurst, New Jersey... Oh, the humanity!
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Not sure you can get an exact ranking, because three were researched simultaneously:\n\nHelium was discovered on Earth in 1895 by Scottish chemist Sir William Ramsay, though some credit the discovery of helium (in the sun's spectrum) to Janssen and Lockyear in 1868. Ramsay discovered most of the remaining noble gases--argon in 1894 (with Lord Rayleigh) and krypton, neon, and xenon in 1898 (with Morris M. Travers). Radon was discovered in 1898 by Fredrich Ernst Dorn.
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The elements don't match up, so it can't be done.  Nitrogen does not appear on the right side, nor oxygen on the left.
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When Sir William Ramsey discovered neon in June 1898, his 13-year old son William asked him, "What are you going to call the new gas? I should like to call it novum." His father liked the idea, but thought that neon, which meant the same thing, would sound better.
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YOU WOULD HAVE TO USE THE BOND ENTHALPIES TO WORK OUT WHICH ONE. SEEING THOUGH N2 MAKES UP 78%OF THE EARTHS ATMOSPHERE ITS SEEMS VERY INERT SO MOST PEOPLE WOULD ASSUME THAT IS THE ONE
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Wolfgang Pauli was the first to propose it in 1930, but Enrico Fermi named it.\nIn 1932 James Chadwick discovers the neutron.\n But it wasn't until 1956 that Reines and Cowan actually discovered neutrino reactions in their atomic experiments.
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www.google.com  \n"info on nitrogen"
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Helium is a basic element, atomic weight 2. It's a noble gas. Because it's a basic element, it can't be broken down into anything else besides what it is.\n\nHelium, the second most abundant element in the universe, was discovered on the sun before it was found on the earth. Pierre-Jules-César Janssen, a French astronomer, noticed a yellow line in the sun's spectrum while studying a total solar eclipse in 1868. Sir Norman Lockyer, an English astronomer, realized that this line, with a wavelength of 587.49 nanometers, could not be produced by any element known at the time. It was hypothesized that a new element on the sun was responsible for this mysterious yellow emission. This unknown element was named helium by Lockyer.
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Water, nitrogen and carbon.
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Nitrogen is important to plant growth.
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There is some dispute over who discovered oxygen.  Joseph Priestley and Antoine Lavoisier both worked on the discovery of oxygen.  Lavoisier published his work first, but I believe that Priestly did his work first.\n\nAntoine Lavoisier named hydrogen, but it was generated and described in earlier experiments by Theophrastus Bombastus von Hohenheim, Robert Boyle, and Henry Cavendish.
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He discovered the urea cycle in 1932. The urea cycle is a cycle of biochemical reactions occurring in many animal organisms that produces urea from ammonia. This cycle, also known as ornithine cycle, was the first metabolic cycle discovered (Krebs and Hensenleit, 1932). \n\nUrea is much less toxic than ammonia; therefore, organisms that cannot easily and quickly remove ammonia usually have to convert it to some other substance, like urea or uric acid. Insufficiency of the urea cycle occurs in some genetic disorders (inborn errors of metabolism), and in liver failure. The result in liver failure is accumulation of nitrogenous waste, mainly ammonia, which leads to hepatic encephalopathy. and the citric acid cycle in 1937, which is still often called Krebs cycle. He was awarded the Nobel Prize in Physiology or Medicine in 1953. The citric acid cycle (also known as the tricarboxylic acid cycle, the TCA cycle, or the Krebs cycle) is a series of chemical reactions of central importance in all living cells that utilize oxygen as part of cellular respiration. In these aerobic organisms, the citric acid cycle is a metabolic pathway that forms part of the break down of carbohydrates, fats and proteins into carbon dioxide and water in order to generate energy. It is the second of three metabolic pathways that are involved in fuel molecule catabolism and ATP production, the other two being glycolysis and oxidative phosphorylation. \n\nThe citric acid cycle also provides precursors for many compounds such as certain amino acids, and some of its reactions are therefore important even in cells performing fermentation.
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We don't detect amino acids in stars directly, they need a much cooler environment to form and stay together.  We have found them in asteroids and comets within our own solar system, and have observed them in clouds of insterstellar gas.\n\nThe "we are all made of stardust" comment comes from the relization that all of the elements heavier than hydrogen and helium are created in the cores of stars, or in the violent deaths of some stars.  All the elements that make up you, me, this planet, everything were formed inside of stars and then blown out upon the cosmos to be reincorporated into new structures.  Kind of neat actually.
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helium \n(He), chemical element, inert gas of Group 0 (noble gases) of the periodic table. The second lightest element (only hydrogen is lighter), helium is a colourless, odourless, and tasteless gas that becomes liquid at -268.9 C (-452 F). Only under increased pressure (approximately 25 atmospheres) does helium solidify.\nHelium was discovered in the gaseous atmosphere surrounding the Sun by the French astronomer Pierre Janssen, who detected a bright yellow line in the spectrum of the solar chromosphere during an eclipse in 1868; this line was initially assumed to represent the element sodium. That same year, the English astronomer Joseph Norman Lockyer observed a yellow line in the solar spectrum that did not correspond to the known D1 and D2 lines of sodium, and so he named it the D3 line. Lockyer concluded that the D3 line was caused by an element in the Sun that was unknown on Earth; he and the chemist Edward Frankland used the Greek word for sun, helios, in naming the element. The British chemist Sir William Ramsay discovered the existence of helium on Earth in 1895. Ramsay obtained a sample of the uranium-bearing mineral cleveite, and upon investigating the gas produced by heating the sample, he found that a unique bright-yellow line in its spectrum matched that of the D3 line observed in the spectrum of the Sun; the new element of helium was thus conclusively identified. In 1903 Ramsay and Frederick Soddy further determined that helium is a product of the spontaneous disintegration of radioactive substances. \n\nHelium constitutes about 23 percent of the mass of the universe and is thus second in abundance to hydrogen in the cosmos. Helium is concentrated in stars, where it is synthesized from hydrogen by nuclear fusion. Although helium occurs in the Earth's atmosphere only to the extent of 1 part in 200,000 (0.0005 percent), and small amounts occur in radioactive minerals, meteoric iron, and mineral springs, great volumes of helium are found as a component (up to 7.6 percent) in natural gases in the United States (especially in Texas, New Mexico, Kansas, Oklahoma, Arizona, and Utah). Smaller supplies have been discovered in Canada and South Africa and in the Sahara Desert.\n\nAlthough there are six known isotopes of helium, only two are stable: helium-3 (symbolized 3He) and helium-4 (symbolized 4He). The four other isotopes are all radioactive, decaying very rapidly into other substances. The helium that is present on Earth is not a primordial component of the Earth but has been generated by radioactive decay. Alpha particles, ejected from the nuclei of heavier radioactive substances, are nuclei of the isotope helium-4. Helium does not accumulate in large quantities in the atmosphere because Earth's gravity is not sufficient to prevent its gradual escape into space. The trace of the isotope helium-3 on Earth is attributable to the negative beta decay of the rare hydrogen-3 isotope (tritium). Helium-4 is by far the most plentiful of the stable isotopes: helium-4 atoms outnumber those of helium-3 about 700,000:1 in atmospheric helium and about 7,000,000:1 in certain helium-bearing minerals.\n\nHelium-4 is unique in having two liquid forms (see Figure A). The normal liquid form is called helium I and exists at temperatures from its boiling point of 4.21 K (-268.9 C) down to about 2.18 K (-271 C). Below 2.18 K, helium-4 undergoes superfluidity (i.e., its viscosity, or resistance to flow, nearly vanishes) and its thermal conductivity becomes more than 1,000 times greater than that of copper. This liquid form is called helium II to distinguish it from normal liquid helium I. By contrast, the less plentiful helium-3 forms three distinguishable liquid phases (see Figure B), of which two are superfluids. Superfluidity in helium-4 was discovered by the Russian physicist Pyotr Leonidovich Kapitsa in the mid-1930s, and the same phenomenon in helium-3 was first observed by Douglas D. Osheroff, David M. Lee, and Robert C.