Detection of the mercapto radical SH in the solar atmosphere

Abstract

Abstract. We analyze new high-resolution UV observations of the solar photosphere in the disk center and the limb and report the first detection of SH lines in the solar atmosphere. We perform a synthesis of the solar spectrum including many atomic and molecular lines and find a few relatively unblended SH lines from which we determine the (0, 0) band oscillator strength f00 = 2.2 × 10 −3 . We conclude that these lines are excellent indicators of the sulfur abundance and isotope ratio in G and K stars.

On SH Molecules in Umbral Spectra

“…In contrast to the theoretical f 0,0 = 1.63 x 10 -3 used here and reported by Henneker and Popkie (1971), Berdyugina et al (2002) Gingerich et al (1971), to Grevesse & Sauval (1999), to Holweger & Müller (1974) and to Vernazza et al(1976) photospheric models. Filled circles, filled triangles and crosses refer to micro-turbulence values as 0.85, 1.00 and 2.1 km s -1 respectively.…”

“…Filled circles, filled triangles and crosses refer to micro-turbulence values as 0.85, 1.00 and 2.1 km s -1 respectively. Panels (A), (B) and (C) refer respectively to (i) Q 2 lines arising from J = 1.5 to 11.5, (ii)one line each from the six branches with J = 11.5 and (iii)for the lines reported as present by Berdyugina & Livingston (2002).…”

“…The chosen umbral models are those due to Henoux (1969), Zwaan (1974), Boyer (1980), Avrett et al (1981) and Stellmacher and Wiehr (1981). The calculations were carried out for all the Q 2 lines chosen by Sinha et al (1976, 77), all the five lines investigated by Berdyugina and Livingston (2002) and the six lines arising from J = 10.5 of the P 1 , P 2 , Q 1 , Q 2 , R 1 and the R 2 branches involved in the transition. The chosen micro-turbulence values are 0.85, 1.0 and 2.1 km s -1 .…”

Rotational Energy Transfer of SH(X2Π, v′′=0, J′′=0.5–10.5) by Collision with Ar: Λ‐Doublet Resolved Transition Propensity

“…[1,2] The produced SH has widely attracted studies of its kinetic reactivity with some atmospheric species, [3][4][5][6][7][8][9][10] the related photodissociation dynamics and mechanism, [11][12][13][14][15][16][17] and astrochemical characterization in interstellar space. [18,19] Spectral characterization of SH(X 2 P) radicals yielded the molecular constants and interaction constants for L doublets and hyperfine splitting. [18][19][20][21] In the case of the RgSH(X) (Rg = Ne, Ar, Kr) complexes, several groups have applied various methods to generate the related potential-energy surfaces (PESs).…”

“…[18,19] Spectral characterization of SH(X 2 P) radicals yielded the molecular constants and interaction constants for L doublets and hyperfine splitting. [18][19][20][21] In the case of the RgSH(X) (Rg = Ne, Ar, Kr) complexes, several groups have applied various methods to generate the related potential-energy surfaces (PESs). [22][23][24][25][26][27][28][29][30][31] Miller and co-workers [22][23][24][25] acquired laser-induced excitation and dispersed fluorescence, and then the spectroscopic data of complexes were fitted to empirical PESs.…”