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Title: Line Identification of Atomic and Ionic Spectra of Holmium in the Near-UV. II. Spectra of Ho ii and Ho iii

Abstract

Fourier Transform spectra of holmium (Ho) in the UV spectral range from 31,530 to 25,000 cm{sup −1} (317 to 400 nm) have been investigated, particularly focusing on the ionic lines. The distinction between the different degrees of ionization (I, II, and III) is based on differences in signal-to-noise ratios from two Ho spectra, which have been measured with different buffer gases, i.e., neon and argon. Based on 106 known Ho ii and 126 known Ho iii energy levels, 97 lines could be classified as transitions of singly ionized Ho and 9 lines could be classified as transitions of doubly ionized Ho. Of the 97 Ho ii lines, 6 have not been listed in the extant literature. Another 215 lines have been assigned to Ho ii, though they could not be classified on the basis of the known energy levels.

Authors:
; ; ;  [1]; ;  [2]; ;  [3]; ;  [4];  [5]
  1. Faculty of Science, Department of Physics, Istanbul University, TR-34134 Vezneciler, Istanbul (Turkey)
  2. Graduate School of Engineering and Sciences, Istanbul University, TR-34452 Beyazat, Istanbul (Turkey)
  3. Faculty of Science, Department of Astronomy and Space Sciences, Istanbul University, 34119, Istanbul (Turkey)
  4. Laser Centre, The University of Latvia, Rainis Boulevard 19, LV-1586 Riga (Latvia)
  5. Hochschule für Technik und Wirtschaft Berlin, Wilhelminenhofstr. 75A, D-12459 Berlin (Germany)
Publication Date:
OSTI Identifier:
22661354
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal, Supplement Series; Journal Volume: 228; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
74 ATOMIC AND MOLECULAR PHYSICS; 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ARGON; BUFFERS; EMISSION SPECTRA; ENERGY LEVELS; FOURIER TRANSFORMATION; HOLMIUM; HOLMIUM IONS; IONIZATION; NEON; NOISE; SIGNAL-TO-NOISE RATIO; ULTRAVIOLET RADIATION

Citation Formats

Başar, Gö., Güzelçimen, F., Er, A., Öztürk, I. K., Al-Labady, N., Özdalgiç, B., Ak, T., Bİlİr, S., Tamanis, M., Ferber, R., and Kröger, S., E-mail: ikanat@istanbul.edu.tr. Line Identification of Atomic and Ionic Spectra of Holmium in the Near-UV. II. Spectra of Ho ii and Ho iii. United States: N. p., 2017. Web. doi:10.3847/1538-4365/228/2/17.
Başar, Gö., Güzelçimen, F., Er, A., Öztürk, I. K., Al-Labady, N., Özdalgiç, B., Ak, T., Bİlİr, S., Tamanis, M., Ferber, R., & Kröger, S., E-mail: ikanat@istanbul.edu.tr. Line Identification of Atomic and Ionic Spectra of Holmium in the Near-UV. II. Spectra of Ho ii and Ho iii. United States. doi:10.3847/1538-4365/228/2/17.
Başar, Gö., Güzelçimen, F., Er, A., Öztürk, I. K., Al-Labady, N., Özdalgiç, B., Ak, T., Bİlİr, S., Tamanis, M., Ferber, R., and Kröger, S., E-mail: ikanat@istanbul.edu.tr. Wed . "Line Identification of Atomic and Ionic Spectra of Holmium in the Near-UV. II. Spectra of Ho ii and Ho iii". United States. doi:10.3847/1538-4365/228/2/17.
@article{osti_22661354,
title = {Line Identification of Atomic and Ionic Spectra of Holmium in the Near-UV. II. Spectra of Ho ii and Ho iii},
author = {Başar, Gö. and Güzelçimen, F. and Er, A. and Öztürk, I. K. and Al-Labady, N. and Özdalgiç, B. and Ak, T. and Bİlİr, S. and Tamanis, M. and Ferber, R. and Kröger, S., E-mail: ikanat@istanbul.edu.tr},
abstractNote = {Fourier Transform spectra of holmium (Ho) in the UV spectral range from 31,530 to 25,000 cm{sup −1} (317 to 400 nm) have been investigated, particularly focusing on the ionic lines. The distinction between the different degrees of ionization (I, II, and III) is based on differences in signal-to-noise ratios from two Ho spectra, which have been measured with different buffer gases, i.e., neon and argon. Based on 106 known Ho ii and 126 known Ho iii energy levels, 97 lines could be classified as transitions of singly ionized Ho and 9 lines could be classified as transitions of doubly ionized Ho. Of the 97 Ho ii lines, 6 have not been listed in the extant literature. Another 215 lines have been assigned to Ho ii, though they could not be classified on the basis of the known energy levels.},
doi = {10.3847/1538-4365/228/2/17},
journal = {Astrophysical Journal, Supplement Series},
number = 2,
volume = 228,
place = {United States},
year = {Wed Feb 01 00:00:00 EST 2017},
month = {Wed Feb 01 00:00:00 EST 2017}
}
  • The Fourier Transform spectra of a Holmium hollow cathode discharge lamp have been investigated in the UV spectral range from 25,000 up to 31,530 cm{sup −1} (317 to 400 nm). Two Ho spectra have been measured with neon and argon as buffer gases. Based on the intensity ratios from these two spectra, a distinction was made between atomic and ionic lines (ionic lines are discussed in an accompanying paper). Using the known Ho i energy levels, 71 lines could be classified as transitions of atomic Ho, 34 of which have not been published previously. Another 32 lines, which could notmore » be classified, are listed in the literature and assigned as atomic Ho. An additional 370 spectral lines have been assigned to atomic Ho based on the signal-to-noise ratio in the two spectra measured under different discharge conditions, namely with buffer gases argon and neon, respectively. These 370 lines have not been previously listed in the literature.« less
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  • A comparative analysis of the optical spectra of holmium excited by electron impact and ionic bombardment is given. It is shown that under ionic bombardment, the probability of excitation of screened transitions is significantly higher than under electron impact.
  • Aims. Our aim is to interpret the EUV spectra of the solar corona, one hopes for laboratory data of specific chemical elements obtained under coronal conditions. Methods. EUV spectra of He, C, N, O, F, Ne, S, Ar, Fe, and Ni in a 40 Å wide wavelength interval near λ304 were excited in an electron beam ion trap. Results. We observe some two hundred lines about half of which are not yet identified and included in spectral models. Conclusions. Lastly, our data provide a check on the atomic data bases underlying the spectral models that are used to interpret solarmore » corona data. However, a multitude of mostly weak additional lines taken together represent a flux that is comparable to that of various primary lines.« less