Trihydrogen cation

context: en: H+3 + CO → HCO+ + H2The 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. H+3 can also react with atomic oxygen to form OH+ and H2.
qas: question: zh_tw: HCO + 是哪類化學中的重要分子？
answers: en: text: interstellar

context: en: H+3 has been detected in two types of celestial environments: Jovian planets and interstellar clouds. In Jovian planets, it has been detected in the planet's ionospheres, the region where the Sun's high energy radiation ionizes the particles in the atmosphere. Since there is a high level of H2 in these atmospheres, this radiation can produce a significant amount of H+3. Also, with a broadband source like the Sun, there is plenty of radiation to pump the H+3 to higher energy states from which it can relax by stimulated and spontaneous emission.
qas: question: zh_tw: H2 經過輻射之後的反應結果生成了什麼？
answers: en: text: H+3

context: en: H+3 was first discovered by J. J. Thomson in 1911. 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 H+3. Since C4+ would be very unlikely and the signal grew stronger in pure hydrogen gas, he correctly assigned the species as H+3.
qas: question: zh_tw: 誰在 1911 年發現了 H3 + 離子？
answers: en: text: J. J. Thomson

context: en: The detection of the first H+3 emission lines was reported in 1989 by Drossart et al., found in the ionosphere of Jupiter. Drossart found a total of 23 H+3 lines with a column density of 1.39×109/cm2. Using these lines, they were able to assign a temperature to the H+3 of around 1,100 K (830 °C), which is comparable to temperatures determined from emission lines of other species like H2. In 1993, H+3 was found in Saturn by Geballe et al. and in Uranus by Trafton et al.
qas: question: zh_tw: 德羅薩爾 t 發現的 23 H=3 線的柱密度是多少？
answers: en: text: 1.39×109/cm2

question: zh_tw: 哪一年發現了 H+3？
answers: en: text: 1993

context: en: To approximate the path length of H+3 in these clouds, Oka used the steady-state model to determine the predicted number densities in diffuse and dense clouds. As explained above, both diffuse and dense clouds have the same formation mechanism for H+3, but different dominating destruction mechanisms. In dense clouds, proton transfer with CO is the dominating destruction mechanism. This corresponds to a predicted number density of 10−4 cm−3 in dense clouds.
qas: question: zh_tw: 他憑藉什麼手段做出了自己的假設？
answers: en: text: the steady-state model

question: zh_tw: 瀰漫和稠密星際雲生成 H+3 的機理與什麼不同？
answers: en: text: dominating destruction mechanisms

context: en: Unexpectedly, three H+3 lines were detected in 1998 by McCall et al. in the diffuse cloud sightline of Cyg OB2 No. 12. Before 1998, the density of H2 was thought to be too low to produce a detectable amount of H+3. McCall detected a temperature of ~27 K (−246 °C) and a column density of ~1014/cm2, the same column density as Geballe & Oka. Since then, H+3 has been detected in many other diffuse cloud sightlines, such as GCS 3-2, GC IRS 3, and ζ Persei.
qas: question: zh_tw: 麥考爾測得什麼溫度？
answers: en: text: ~27 K (−246 °C)