Iron hydride - Laboratory studies and solar identification

Carroll, Paula; McCormack, Paula; O'Connor, Seamus

doi:10.1086/154679

Cited by 58 publications

(17 citation statements)

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“…[11][12][13][14][15][16] Transition metal-containing molecules are also of astrophysical importance and several transition metal oxides and hydrides have been observed in the spectra of the sun and other stars. For example, TiH 17 and FeH 18,19 have been iden-tified in the spectra of M-type stars; NiH 20 and CrH 21 have been seen in the spectra of sunspots.…”

mentioning

confidence: 99%

Fourier transform emission spectroscopy of the B 1Π–X 1Σ+, C 1Σ+–X 1Σ+, and G 1Π–X 1Σ+ systems of ScH and ScD

Ram

Bernath

1996

The Journal of Chemical Physics

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The emission spectra of ScH and ScD have been observed in the 380 nm-2.5 m spectral region using a Fourier transform spectrometer. The molecules were excited in a scandium hollow cathode lamp operated with neon gas and a trace of hydrogen or deuterium. Three transitions with a common lower state, assigned as the ground X 1 ⌺ ϩ state, have been observed in the near infrared and visible regions. The ScH bands with 0-0 band origins at 5404, 13 574, and 20 547 cm Ϫ1 have been assigned as the B 1 ⌸ -X 1 ⌺ ϩ , C 1 ⌺ ϩ -X 1 ⌺ ϩ , and G 1 ⌸ -X 1 ⌺ ϩ transitions, respectively. A rotational analysis of the 0-0, 1-1, 1-0, and 2-1 bands of the B 1 ⌸ -X 1 ⌺ ϩ system, the 0-0 and 1-1 bands of the C 1 ⌺ ϩ -X 1 ⌺ ϩ system and the 0-0 band of the G 1 ⌸ -X 1 ⌺ ϩ system has been obtained. The principal molecular constants for the X 1 ⌺ ϩ state of ScH are ⌬G(1/2)ϭ1546.9730(14) cm Ϫ1 , B e ϭ5.425 432(48) cm Ϫ1 , ␣ e ϭ0.124 802(84) cm Ϫ1 and r e ϭ1.775 427(8) Å. The corresponding band systems of ScD have also been analyzed. A rotational analysis of the 0-0, 1-1, and 1-0 bands of the B 1 ⌸ -X 1 ⌺ ϩ system, the 0-0, 1-1, 0-1, and 1-2 bands of the C 1 ⌺ ϩ -X 1 ⌺ ϩ system and the 0-0 band of the G 1 ⌸ -X 1 ⌺ ϩ system has been obtained. The equilibrium molecular constants determined for the ground state of ScD are e ϭ1141.2650 (31) cm Ϫ1 , e x e ϭ12.3799(15) cm Ϫ1 , B e ϭ2.787 432(41) cm Ϫ1 , ␣ e ϭ0.045 321(73) cm Ϫ1 , and r e ϭ1.771 219(13) Å. The ScH assignments are supported by recent theoretical predictions made by Anglada et al. ͓Mol. Phys. 66, 541 ͑1989͔͒ as well as the experimental results available for ScF and the isovalent YH and LaH molecules. Although some unassigned bands have been attributed to ScH and ScD by previous workers, there have been no previous analyses of ScH or ScD spectra.

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confidence: 99%

Fourier transform emission spectroscopy of the B 1Π–X 1Σ+, C 1Σ+–X 1Σ+, and G 1Π–X 1Σ+ systems of ScH and ScD

Ram

Bernath

1996

The Journal of Chemical Physics

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“…The FeH molecule has been discussed in the astrophysical literature. It was proposed that FeH forms in the Sun and some other stars (Carroll, McCormack & O'Connor 1976). The spectrum of several stars in the ultraviolet, visible, and near-infrared region was compared with laboratory measurements of FeH and good agreement for some lines was obtained.…”

Section: Introductionmentioning

confidence: 87%

Missing Fe: hydrogenated iron nanoparticles

Bilalbegović

Maksimović

Mohaček-Grošev

2016

Monthly Notices of the Royal Astronomical Society: Letters

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Although it was found that the FeH lines exist in the spectra of some stars, none of the spectral features in the ISM have been assigned to this molecule. We suggest that iron atoms interact with hydrogen and produce Fe-H nanoparticles which sometimes contain many H atoms. We calculate infrared spectra of hydrogenated iron nanoparticles using density functional theory methods and find broad, overlapping bands. Desorption of H 2 could induce spinning of these small Fe-H dust grains. Some of hydrogenated iron nanoparticles posses magnetic and electric moments and should interact with electromagnetic fields in the ISM. Fe n H m nanoparticles could contribute to the polarization of the ISM and the anomalous microwave emission. We discuss the conditions required to form FeH and Fe n H m in the ISM.

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“…Klynning & Lindgren (1973) reported that lines of the (0−0) band of FeH extend from 9 896Å to at least 10 205Å. Carroll et al (1976) detected a number of coincidences between laboratory lines of FeH and weak unidentified solar lines, again in the blue and green wavelength region, in addition to the infrared. Wing et al (1977) confirmed the presence of the (0−0) and (1−0) bands of iron hydride in sunspots and cool stars.…”

Section: Introductionmentioning

confidence: 96%