Hidrogen deuterida

Hidrogen deuterida
Rumus kerangka hidrogen deuterida
Nama
Nama IUPAC
Hidrogen deuterida
Nama IUPAC (sistematis)
(2H)Dihidrogen[butuh rujukan]
Penanda
Model 3D (JSmol)
3DMet {{{3DMet}}}
ChEBI
ChemSpider
Nomor EC
Nomor RTECS {{{value}}}
Nomor UN 1049
  • InChI=1S/H2/h1H/i1+1 YaY
    Key: UFHFLCQGNIYNRP-OUBTZVSYSA-N YaY
  • InChI=1/H2/h1H/i1+1
    Key: UFHFLCQGNIYNRP-OUBTZVSYED
  • [2H][H]
Sifat
H[2H]
Massa molar 3,02204 g mol−1
Titik lebur −259 °C (−434,2 °F; 14,1 K)
Titik didih −253 °C (−423,4 °F; 20,1 K)
Bahaya
Mudah terbakar F+
Frasa-R R12
Frasa-S S16, S33, S36, S38
571 °C (1.060 °F; 844 K)
Senyawa terkait
Related Hidrogen
 Deuterium

Hidrogen
Tritium

Kecuali dinyatakan lain, data di atas berlaku pada suhu dan tekanan standar (25 °C [77 °F], 100 kPa).
YaY verifikasi (apa ini YaYN ?)
Referensi

Hidrogen deuterida adalah sebuah molekul diatomik atau senyawa dua isotop hidrogen: isotop utama 1H (protium) dan 2H (deuterium). Rumus kimianya adalah H2H, tetapi biasanya disingkat HD.

Ketersediaan

Spektrum H NMR dari larutan HD (ditandai dengan batang merah) dan H2 (batang biru). Triplet 1:1:1 muncul dari penggandengan inti 1H (I = 1/2) ke inti 2H (I = 1).

Hidrogen deuterida dibuat dari reaksi natrium hidrida dengan air berat:[1]

NaH + D2O → HD + NaOD

Hidrogen deuterida adalah komponen kecil dari molekul hidrogen alami sekaligus merupakan komponen yang terdapat di atmosfer semua planet raksasa, dengan kelimpahan berkisar antara 30 ppm hingga 200 ppm. HD juga ditemukan pada sisa-sisa supernova.[2]

Ketersediaan HD versus H2 di atmosfer planet raksasa
Planet HD H2[butuh rujukan]
Jupiter ~0,003% 89,8% ±2,0%
Uranus ~0,007% 83,0% ±3,0%
Neptunus ~0,019% 80,0% ±3,2%

Spektra emisi radio

HD dan H2 memiliki spektra emisi yang sangat mirip, tetapi frekuensi emisinya berbeda.[3]

Frekuensi transisi rotasi HD J = 1-0 yang penting dalam bidang astronomi pada 2,7 THz telah diukur dengan radiasi FIR yang dapat disesuaikan dengan akurasi 150 kHz.[4]

Referensi

  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: 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. arXiv:0704.2179 alt=Dapat diakses gratis. Bibcode:2007ApJ...664..890N. doi:10.1086/518857. 
  3. ^ 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. 
  4. ^ 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. 

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