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1. Phosphorescence in Mn ⁴⁺ -Doped R ⁺ / R ²⁺ Germanates ( R ⁺ = Na ⁺ or K ⁺ , R ²⁺ = Sr ²⁺ )

   https://doi.org/10.1021/acs.inorgchem.2c01364  

   Novikov, Sergei A.; Lu, Yimin; Zhang, Weiguo; Halasyamani, P. Shiv; Hariyani, Shruti; Brgoch, Jakoah; Klepov, Vladislav V.; zur Loye, Hans-Conrad; Mozharivskyj, Yurij (June 2022, Inorganic Chemistry)
2. Grids of stellar models with rotation: VIII. Models from 1.7 to 500 M _⊙ at metallicity Z = 10 ⁻⁵

   https://doi.org/10.1051/0004-6361/202450180  

   Sibony, Yves; Shepherd, Kendall G; Yusof, Norhasliza; Hirschi, Raphael; Chambers, Caitlan; Tsiatsiou, Sophie; Nandal, Devesh; Sciarini, Luca; Moyano, Facundo D; Bétrisey, Jérôme; et al (October 2024, Astronomy & Astrophysics)

   Context.Grids of stellar evolution models with rotation using the Geneva stellar evolution code (GENEC) have been published for a wide range of metallicities. Aims.We introduce the last remaining grid of GENECmodels, with a metallicity ofZ = 10⁻⁵. We study the impact of this extremely metal-poor initial composition on various aspects of stellar evolution, and compare it to the results from previous grids at other metallicities. We provide electronic tables that can be used to interpolate between stellar evolution tracks and for population synthesis. Methods.Using the same physics as in the previous papers of this series, we computed a grid of stellar evolution models with GENECspanning masses between 1.7 and 500M_⊙, with and without rotation, at a metallicity ofZ = 10⁻⁵. Results.Due to the extremely low metallicity of the models, mass-loss processes are negligible for all except the most massive stars. For most properties (such as evolutionary tracks in the Hertzsprung-Russell diagram, lifetimes, and final fates), the present models fit neatly between those previously computed at surrounding metallicities. However, specific to this metallicity is the very large production of primary nitrogen in moderately rotating stars, which is linked to the interplay between the hydrogen- and helium-burning regions. Conclusions.The stars in the present grid are interesting candidates as sources of nitrogen-enrichment in the early Universe. Indeed, they may have formed very early on from material previously enriched by the massive short-lived Population III stars, and as such constitute a very important piece in the puzzle that is the history of the Universe. 

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3. Layered and Cubic Semiconductors A Ga M ′ Q ₄ ( A ⁺ = K ⁺ , Rb ⁺ , Cs ⁺ , Tl ⁺ ; M ′ ⁴⁺ = Ge ⁴⁺ , Sn ⁴⁺ ; Q ^2– = S ^2– , Se ^2– ) and High Third-Harmonic Generation

   https://doi.org/10.1021/jacs.0c08638  

   Friedrich, Daniel; Byun, Hye Ryung; Hao, Shiqiang; Patel, Shane; Wolverton, Chris; Jang, Joon Ik; Kanatzidis, Mercouri G. (October 2020, Journal of the American Chemical Society)

   null (Ed.)
4. The Matrix Equation X ³ + Y ³ = 2 Z ³

   https://doi.org/10.1080/00029890.2024.2409065  

   Garcia, Stephan Ramon; Rajkhowa, Juganta; Sarma, Kuldeep (January 2025, The American Mathematical Monthly)
5. Spectroscopic study of the 4 f ⁷ 6 s ^{2 8} S 7/2∘−4 f ⁷ ( ⁸ S ^∘ )6 s 6 p ( ¹ P ^∘ ) ⁸ P _9/2 transition in neutral europium-151 and europium-153: absolute frequency and hyperfine structure

   https://doi.org/10.1364/JOSAB.467968  

   Herd, M_T; Maruko, C.; Herzog, M_M; Brand, A.; Cannon, G.; Duah, B.; Hollin, N.; Karani, T.; Wallace, A.; Whitmore, M.; et al (September 2022, Journal of the Optical Society of America B)

   We report on spectroscopic measurements on the $4f^{7}6s^2{}^8{S}_{7/2}^{\circ <\#comment/>}\to <\#comment/>4f^7{(}^8{S}^{\circ <\#comment/>}\left)6s6p{(}^1{P}^{\circ <\#comment/>}\right){}^8{P}_{9/2}$transition in neutral europium-151 and europium-153 at 459.4 nm. The center of gravity frequencies for the 151 and 153 isotopes, reported for the first time in this paper, to our knowledge, were found to be 652,389,757.16(34) MHz and 652,386,593.2(5) MHz, respectively. The hyperfine coefficients for the $6s6p{(}^1{P}^{\circ <\#comment/>}){}^8{P}_{9/2}$state were found to be $\mathrm{A}\left(151\right)=-<\#comment/>228.84\left(2\right)\mathrm{M}\mathrm{H}\mathrm{z}$, $\mathrm{B}\left(151\right)=226.9\left(5\right)\mathrm{M}\mathrm{H}\mathrm{z}$and $\mathrm{A}\left(153\right)=-<\#comment/>101.87\left(6\right)\mathrm{M}\mathrm{H}\mathrm{z}$, $\mathrm{B}\left(153\right)=575.4\left(1.5\right)\mathrm{M}\mathrm{H}\mathrm{z}$, which all agree with previously published results except for A(153), which shows a small discrepancy. The isotope shift is found to be 3163.8(6) MHz, which also has a discrepancy with previously published results. 

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