Optical Spectra of Cr3+Impurity Ions in Ferroelectric LiNbO3and LiTaO3

1969 ◽  
Vol 50 (4) ◽  
pp. 1501-1510 ◽  
Author(s):  
A. M. Glass
Keyword(s):  
Optical Spectra ◽  
Impurity Ions

On the effect of overlapping and covalency on the optical spectra of impurity ions in dielectric crystals

1972 ◽  
Vol 49 (1) ◽  
pp. 61-70 ◽  
Author(s):  
V. I. Cherepanov ◽  
A. I. Krotkii ◽  
A. A. Shchetkov
Keyword(s):  
Optical Spectra ◽  
Impurity Ions

Optical Spectra, EPR, and Spin–Lattice Relaxation of Yb3+ Ions in Crystals Having Perovskite-Type Structure

1977 ◽  
Vol 81 (1) ◽  
pp. 287-293 ◽  
Author(s):  
A. A. Antipin ◽  
A. V. Vinokurov ◽  
M. P. Davydova ◽  
S. L. Korableva ◽  
A. L. Stolov ◽  
...  
Keyword(s):  
Lattice Relaxation ◽  
Optical Spectra ◽  
Type Structure ◽  
Spin Lattice Relaxation ◽  
Spin Lattice ◽  
Perovskite Type ◽  
Perovskite Type Structure

scholarly journals Characterization of M dwarfs using optical mid-resolution spectra for exploration of small exoplanets

2020 ◽  
Author(s):  
Yohei Koizumi ◽  
Masayuki Kuzuhara ◽  
Masashi Omiya ◽  
Teruyuki Hirano ◽  
John Wisniewski ◽  
...  
Keyword(s):  
Sample Selection ◽  
Optical Spectra ◽  
Average Error ◽  
Spectral Energy ◽  
M Dwarfs ◽  
Energy Distributions ◽  
Fitting Procedures ◽  
Optical Region ◽  
Selection For

Abstract We present the optical spectra of 338 nearby M dwarfs, and compute their spectral types, effective temperatures (Teff), and radii. Our spectra were obtained using several optical spectrometers with spectral resolutions that range from 1200 to 10000. As many as 97% of the observed M-type dwarfs have a spectral type of M3–M6, with a typical error of 0.4 subtype, among which the spectral types M4–M5 are the most common. We infer the Teff of our sample by fitting our spectra with theoretical spectra from the PHOENIX model. Our inferred Teff is calibrated with the optical spectra of M dwarfs whose Teff have been well determined with the calibrations that are supported by previous interferometric observations. Our fitting procedures utilize the VO absorption band (7320–7570 Å) and the optical region (5000–8000 Å), yielding typical errors of 128 K (VO band) and 85 K (optical region). We also determine the radii of our sample from their spectral energy distributions. We find most of our sample stars have radii of <0.6 R⊙, with the average error being 3%. Our catalog enables efficient sample selection for exoplanet surveys around nearby M-type dwarfs.

scholarly journals Aggregates of polar dyes: beyond the exciton model

2021 ◽  
Vol 23 (14) ◽  
pp. 8282-8291
Author(s):  
Mattia Anzola ◽  
Anna Painelli
Keyword(s):  
Degrees Of Freedom ◽  
Optical Spectra ◽  
Exciton Model

Optical spectra of aggregates of polar dyes are discussed, fully accounting for polarizability of the dyes and for the coupling of electronic and vibrational degrees of freedom.

Optical spectra of lithium vapour zones produced by thermal evaporation in hydrogenating atmosphere

1999 ◽  
Vol 11 (6) ◽  
pp. 1621-1629 ◽  
Author(s):  
Shosuke Mochizuki ◽  
Mie Sasaki ◽  
Raphael Ruppin
Keyword(s):  
Thermal Evaporation ◽  
Optical Spectra

Discovery of five new Galactic symbiotic stars in the VPHAS+ survey

2021 ◽  
Vol 502 (2) ◽  
pp. 2513-2517
Author(s):  
Stavros Akras ◽  
Denise R Gonçalves ◽  
Alvaro Alvarez-Candal ◽  
Claudio B Pereira
Keyword(s):  
Spectroscopic Data ◽  
Selection Criterion ◽  
Optical Spectra ◽  
Emission Lines ◽  
High Rate ◽  
Symbiotic Stars ◽  
Selection Of

ABSTRACT We report the validation of a recently proposed infrared (IR) selection criterion for symbiotic stars (SySts). Spectroscopic data were obtained for seven candidates, selected from the SySt candidates of Akras et al. by employing the new supplementary IR selection criterion for SySts in the VST/OmegaCAM Photometric H-Alpha Survey. Five of them turned out to be genuine SySts after the detection of H α, He ii, and [O iii] emission lines as well as TiO molecular bands. The characteristic O vi Raman-scattered line is also detected in one of these SySts. According to their IR colours and optical spectra, all five newly discovered SySts are classified as S-type. The high rate of true SySts detections of this work demonstrates that the combination of the H α emission and the new IR criterion improves the selection of target lists for follow-up observations by minimizing the number of contaminants and optimizing the observing time.

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