Hydrogen deuteride

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Wikipedia

Hydrogen deuteride
Skeletal formula of hydrogen deuteride
Skeletal formula of hydrogen deuteride
Names
IUPAC name
Hydrogen deuteride
Systematic IUPAC name
(2H)Dihydrogen[citation needed]
Identifiers
3D model (JSmol)
ChemSpider
ECHA InfoCard 100.034.325 Edit this at Wikidata
EC Number
  • 237-773-0
UN number 1049
  • InChI=1S/H2/h1H/i1+1 checkY
    Key: UFHFLCQGNIYNRP-OUBTZVSYSA-N checkY
  • InChI=1/H2/h1H/i1+1
    Key: UFHFLCQGNIYNRP-OUBTZVSYED
  • [2H][H]
Properties
HD
Molar mass 3.02204 g mol−1
Melting point −259 °C (−434.2 °F; 14.1 K)
Boiling point −253 °C (−423.4 °F; 20.1 K)
Hazards
GHS labelling:
GHS02: FlammableGHS04: Compressed Gas
Danger
H220, H280
P210, P377, P381, P403, P410+P403
NFPA 704 (fire diamond)
NFPA 704 four-colored diamondHealth 0: Exposure under fire conditions would offer no hazard beyond that of ordinary combustible material. E.g. sodium chlorideFlammability 4: Will rapidly or completely vaporize at normal atmospheric pressure and temperature, or is readily dispersed in air and will burn readily. Flash point below 23 °C (73 °F). E.g. propaneInstability 0: Normally stable, even under fire exposure conditions, and is not reactive with water. E.g. liquid nitrogenSpecial hazards (white): no code
0
4
0
571 °C (1,060 °F; 844 K)
Related compounds
Related hydrogens
 Deuterium

Hydrogen
Tritium

Except where otherwise noted, data are given for materials in their standard state (at 25 °C [77 °F], 100 kPa).
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Hydrogen deuteride is an isotopologue of dihydrogen composed of two isotopes of hydrogen: the majority isotope 1H (protium) and 2H (deuterium). Its proper molecular formula is 1H2H, but for simplification, it is usually written as HD.

Preparation and occurrence

In the laboratory it is produced by treating sodium hydride with deuterated water:[1]

NaH + D2O → HD + NaOD

Hydrogen deuteride is a minor component of naturally occurring molecular hydrogen. It is one of the minor but noticeable components of the atmospheres of all the giant planets, with abundances from about 30 ppm to about 200 ppm. HD has also been found in supernova remnants,[2] dense interstellar clouds,[3] and protoplanetary disks.[4][5]

Occurrence of HD vs. H2 in giant planets' atmospheres
PlanetHDH2
Jupiter~0.003%89.8% ±2.0%[6]
Uranus~0.015%82.5% ±3.3%[7]
Neptune~0.019%80.0% ±3.2%[8]
H NMR spectrum of a solution of HD (labeled with red bars) and H2 (blue bar). The 1:1:1 triplet arises from the coupling of the 1H nucleus (I = 1/2) to the 2H nucleus ( I = 1).

Radio emission spectra

HD and H2 have very similar emission spectra, but the emission frequencies differ.[9]

The frequency of the astronomically important J = 1-0 rotational transition of HD at 2.7 THz has been measured with tunable FIR radiation with an accuracy of 150 kHz.[10] In astronomy, this J = 1-0 line has been used to determine the masses of protoplanetary disks surrounding T Tauri stars[4] and Herbig Ae/Be stars.[5]

References

  1. ↑ Bautista, Maria T.; Cappellani, E. Paul; Drouin, Samantha D.; Morris, Robert H.; Schweitzer, Caroline T.; Sella, Andrea; Zubkowski, Jeffery (1991). "Preparation and Spectroscopic Properties of the η2-Dihydrogen Complexes [MH(η2-H2)PR2CH2CH2PR2)2]+ (M = Iron, Ruthenium; R = Ph, Et) and Trends in Properties Down the Iron Group Triad". Journal of the American Chemical Society. 113 (13): 4876–87. doi:10.1021/ja00013a025.
  2. ↑ Neufeld, David A.; Hollenbach, David J.; Kaufman, Michael J.; Snell, Ronald L.; Melnick, Gary J.; Bergin, Edwin A.; Sonnentrucker, Paule (2007). "SpitzerSpectral Line Mapping of Supernova Remnants. I. Basic Data and Principal Component Analysis". The Astrophysical Journal. 664 (2): 890–908. arXiv:0704.2179. Bibcode:2007ApJ...664..890N. doi:10.1086/518857. S2CID 15286019.
  3. ↑ Drapatz, S.; Michel, K. W. (November 1974). "On the intensity of rotational lines of H2 and HD from dense interstellar clouds". Astronomy & Astrophysics. 36 (2): 211-216. Bibcode:1974A&A....36..211D.
  4. 1 2 McClure, M. K.; Bergin, E. A.; Cleeves, L. I.; Dishoeck, E. F. van; Blake, G. A.; Evans II, N. J.; Green, J. D.; Henning, Th.; Öberg, K. I.; Pontoppidan, K. M.; Salyk, C. (2016-11-10). "MASS MEASUREMENTS IN PROTOPLANETARY DISKS FROM HYDROGEN DEUTERIDE". The Astrophysical Journal. 831 (2): 167. arXiv:1608.07817. doi:10.3847/0004-637X/831/2/167. ISSN 0004-637X.
  5. 1 2 Kama, M.; Trapman, L.; Fedele, D.; Bruderer, S.; Hogerheijde, M. R.; Miotello, A.; van Dishoeck, E. F.; Clarke, C.; Bergin, E. A. (2020). "Mass constraints for 15 protoplanetary discs from HD 1–0" (PDF). Astronomy & Astrophysics. 634: A88. doi:10.1051/0004-6361/201937124. ISSN 0004-6361. Retrieved 2025-05-06.
  6. ↑ Williams, David R. (May 22, 2023). "Jupiter Fact Sheet". NASA Space Science Data Coordinated Archive. Retrieved July 31, 2023.
  7. ↑ Williams, David R. (May 22, 2023). "Uranus Fact Sheet". NASA Space Science Data Coordinated Archive. Retrieved July 31, 2023.
  8. ↑ Williams, David R. (May 22, 2023). "Neptune Fact Sheet". NASA Space Science Data Coordinated Archive. Retrieved July 31, 2023.
  9. ↑ Quinn, W.; Baker, J.; Latourrette, J.; Ramsey, N. (1958). "Radio-Frequency Spectra of Hydrogen Deuteride in Strong Magnetic Fields". Phys. Rev. 112 (6): 1929. Bibcode:1958PhRv..112.1929Q. doi:10.1103/PhysRev.112.1929.
  10. ↑ Evenson, K. M.; Jennings, D. A.; Brown, J. M.; Zink, L. R.; Leopold, K. R. (1988). "Frequency measurement of the J = 1-0 rotational transition of HD". Astrophysical Journal. 330: L135. Bibcode:1988ApJ...330L.135E. doi:10.1086/185221.

Further reading