| 词条 | Trihydrogen cation |
| 释义 |
| Name = Trihydrogen cation | ImageFile = Trihydrogen-cation-3D-vdW.png | ImageSize = | ImageName = Space-filling model of the {{chem|H|3|+}} cation | Section1 = {{Chembox Identifiers | CASNo = 28132-48-1 | RTECS = | Section2 = {{Chembox Properties | Formula = {{chem|H|3|+}} | MolarMass = 3.02 | Appearance = | Density = | Solubility = | MeltingPt = | BoilingPt = | ConjugateBase = Dihydrogen | Section3 = {{Chembox Structure | Coordination = | Section7 = {{Chembox Hazards | EUClass = | RPhrases = | SPhrases = | NFPA-H = | NFPA-F = | NFPA-R = | FlashPt = | Section8 = {{Chembox Related | OtherAnions = hydride | OtherCations = hydrogen ion, dihydrogen cation, hydrogen ion cluster | OtherCompounds = trihydrogen }} The trihydrogen cation, also known as protonated molecular hydrogen or {{chem|H|3|+}}, is one of the most abundant ions in the universe. It is stable in the interstellar medium (ISM) due to the low temperature and low density of interstellar space. The role that {{chem|H|3|+}} plays in the gas-phase chemistry of the ISM is unparalleled by any other molecular ion. The cation is also the simplest triatomic molecule, since its two electrons are the only valence electrons in the system. It is also the simplest example of a three-center two-electron bond system. History{{chem|H|3|+}} was first discovered by J. J. Thomson in 1911.[1] While studying the resultant species of plasma discharges, he discovered something very odd. Using an early form of mass spectrometry, he discovered a large abundance of a molecular ion with a mass-to-charge ratio of 3. He stated that the only two possibilities were C4+ or {{chem|H|3|+}}. Since C4+ would be very unlikely and the signal grew stronger in pure hydrogen gas, he correctly assigned the species as {{chem|H|3|+}}.The formation pathway was discovered by Hogness & Lunn in 1925.[2] They also used an early form of mass spectrometry to study hydrogen discharges. They found that as the pressure of hydrogen increased, the amount of {{chem|H|3|+}} increased linearly and the amount of {{chem|H|2|+}} decreased linearly. In addition, there was little H+ at any pressure. This data suggested the proton exchange formation pathway discussed below. In 1961, Martin et al. first suggested that {{chem|H|3|+}} may be present in interstellar space given the large amount of hydrogen in interstellar space and its reaction pathway was exothermic (~1.5 eV).[3] This led to the suggestion of Watson and Herbst & Klemperer in 1973 that {{chem|H|3|+}} is responsible for the formation of many observed molecular ions.[4][5] It was not until 1980 that the first spectrum of {{chem|H|3|+}} was discovered by Takeshi Oka,[6] which was of the ν2 fundamental band using a technique called frequency modulation detection. This started the search for interstellar {{chem|H|3|+}}. Emission lines were detected in the late 1980s and early 1990s in the ionospheres of Jupiter, Saturn, and Uranus.[7][8][9] In 1996, {{chem|H|3|+}} was finally detected in the interstellar medium (ISM) by Geballe & Oka in two molecular interstellar clouds in the sightlines GL2136 and W33A.[10] In 1998, {{chem|H|3|+}} was unexpectedly detected by McCall et al. in a diffuse interstellar cloud in the sightline Cygnus OB2#12.[11] In 2006 Oka announced that {{chem|H|3|+}} was ubiquitous in interstellar medium, and that the Central Molecular Zone contained a million times the concentration of ISM generally.[12] StructureThe three hydrogen atoms in the molecule form an equilateral triangle, with a bond length of 0.90 Å on each side. The bonding among the atoms is a three-centre two-electron bond, a delocalized resonance hybrid type of structure. The strength of the bond has been calculated to be around 4.5 eV (104 kcal/mol).[13] FormationThe main pathway for the production of {{chem|H|3|+}} is by the reaction of {{chem|H|2|+}} and H2.[14]{{chem|H|2|+}} + H2 → {{chem|H|3|+}} + H The concentration of {{chem|H|2|+}} is what limits the rate of this reaction in nature: the only known natural source of it is via ionization of H2 by a cosmic ray in interstellar space by the ionization of H2: H2 + cosmic ray → {{chem|H|2|+}} + e− + cosmic ray The cosmic ray has so much energy, it is almost unaffected by the relatively small energy transferred to the hydrogen when ionizing an H2 molecule. In interstellar clouds, cosmic rays leave behind a trail of {{chem|H|2|+}}, and therefore {{chem|H|3|+}}. In laboratories, {{chem|H|3|+}} is produced by the same mechanism in plasma discharge cells, with the discharge potential providing the energy to ionize the H2. DestructionThe information for this section was also from a paper by Eric Herbst.[14] There are many destruction reactions for {{chem|H|3|+}}. The dominant destruction pathway in dense interstellar clouds is by proton transfer with a neutral collision partner. The most likely candidate for a destructive collision partner is the second most abundant molecule in space, CO. {{chem|H|3|+}} + CO → HCO+ + H2 The significant product of this reaction is HCO+, an important molecule for interstellar chemistry. Its strong dipole and high abundance make it easily detectable by radioastronomy. {{chem|H|3|+}} can also react with atomic oxygen to form OH+ and H2. {{chem|H|3|+}} + O → OH+ + H2 OH+ then usually reacts with more H2 to create further hydrogenated molecules. OH+ + H2 → {{chem|OH|2|+}} + H {{chem|OH|2|+}} + H2 → {{chem|OH|3|+}} + H At this point, the reaction between {{chem|OH|3|+}} and H2 is no longer exothermic in interstellar clouds. The most common destruction pathway for {{chem|OH|3|+}} is dissociative recombination, yielding four possible sets of products: H2O + H, OH + H2, OH + 2H, and O + H2 + H. While water is a possible product of this reaction, it is not a very efficient product. Different experiments have suggested that water is created anywhere from 5–33% of the time. Water formation on grains is still considered the primary source of water in the interstellar medium. The most common destruction pathway of {{chem|H|3|+}} in diffuse interstellar clouds is dissociative recombination. This reaction has multiple products. The major product is dissociation into three hydrogen atoms, which occurs roughly 75% of the time. The minor product is H2 and H, which occurs roughly 25% of the time. Ortho/Para-H3+The most abundant molecule in dense interstellar clouds is H2. When a {{chem|H|3|+}} molecule collides with H2, stoichiometrically there is no net yield. However, a proton transfer still can take place, which can potentially change the total nuclear spin of the two molecules depending on the nuclear spins of the protons. Two different spin configurations for {{chem|H|3|+}} are possible, called ortho and para. Ortho-{{chem|H|3|+}} has all three proton spins parallel, yielding a total nuclear spin of {{sfrac|3|2}}. Para-{{chem|H|3|+}} has two proton spins parallel while the other is anti-parallel, yielding a total nuclear spin of {{sfrac|1|2}}. Similarly, H2 also has ortho and para states, with ortho-H2 having a total nuclear spin 1 and para-H2 having a total nuclear spin of 0. When an ortho-{{chem|H|3|+}} and a para-H2 collide, the transferred proton changes the total spins of the molecules, yielding instead a para//#14'>14]e− Recombination Rate|journal=Nature|volume=422|issue=6931|doi=10.1038/nature01498|pmid=12673244|arxiv = astro-ph/0302106 |bibcode = 2003Natur.422..500M|pages=500–2 }} External links
4 : Astrochemistry|Cations|Hydrogen physics|Cyclic compounds |
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