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1. SN 2019zrk, a bright SN 2009ip analog with a precursor

   https://doi.org/10.1051/0004-6361/202243452  

   Fransson, Claes; Sollerman, Jesper; Strotjohann, Nora L.; Yang, Sheng; Schulze, Steve; Barbarino, Cristina; Kool, Erik C.; Ofek, Eran O.; Crellin-Quick, Arien; De, Kishalay; et al (October 2022, Astronomy & Astrophysics)

   We present photometric and spectroscopic observations of the Type IIn supernova SN 2019zrk (also known as ZTF 20aacbyec). The SN shows a > 100 day precursor, with a slow rise, followed by a rapid rise to M  ≈ −19.2 in the r and g bands. The post-peak light-curve decline is well fit with an exponential decay with a timescale of ∼39 days, but it shows prominent undulations, with an amplitude of ∼1 mag. Both the light curve and spectra are dominated by an interaction with a dense circumstellar medium (CSM), probably from previous mass ejections. The spectra evolve from a scattering-dominated Type IIn spectrum to a spectrum with strong P-Cygni absorptions. The expansion velocity is high, ∼16 000 km s −1 , even in the last spectra. The last spectrum ∼110 days after the main eruption reveals no evidence for advanced nucleosynthesis. From analysis of the spectra and light curves, we estimate the mass-loss rate to be ∼4 × 10 −2   M ⊙ yr −1 for a CSM velocity of 100 km s −1 , and a CSM mass of 1  M ⊙ . We find strong similarities for both the precursor, general light curve, and spectral evolution with SN 2009ip and similar SNe, although SN 2019zrk displays a brighter peak magnitude. Different scenarios for the nature of the 09ip-class of SNe, based on pulsational pair instability eruptions, wave heating, and mergers, are discussed. 

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2. Isoscaling in central Sn+Sn collisions at 270 MeV/u

   https://doi.org/10.1140/epja/s10050-022-00851-2  

   Lee, J. W.; Tsang, M. B.; Tsang, C. Y.; Wang, R.; Barney, J.; Estee, J.; Isobe, T.; Kaneko, M.; Kurata-Nishimura, M.; Lynch, W. G.; et al (October 2022, The European Physical Journal A)
3. SN 2019yvq Does Not Conform to SN Ia Explosion Models

   https://doi.org/10.3847/1538-4357/abf93b  

   Tucker, M. A.; Ashall, C.; Shappee, B. J.; Vallely, P. J.; Kochanek, C. S.; Huber, M. E.; Anand, G. S.; Keane, J. V.; Hsiao, E. Y.; Holoien, T. W.-S. (June 2021, The Astrophysical Journal)

   null (Ed.)
4. SN 2022jox: An Extraordinarily Ordinary Type II SN with Flash Spectroscopy

   https://doi.org/10.3847/1538-4357/ad2a49  

   Andrews, Jennifer E.; Pearson, Jeniveve; Hosseinzadeh, Griffin; Bostroem, K. Azalee; Dong 董, Yize 一泽; Shrestha, Manisha; Jencson, Jacob E.; Sand, David J.; Valenti, S.; Hoang, Emily; et al (April 2024, The Astrophysical Journal)

   Abstract We present high-cadence optical and ultraviolet (UV) observations of the Type II supernova (SN), SN 2022jox which exhibits early spectroscopic high-ionization flash features of Hi, Heii, Civ, and Nivthat disappear within the first few days after explosion. SN 2022jox was discovered by the Distance Less Than 40 Mpc survey ∼0.75 day after explosion with follow-up spectra and UV photometry obtained within minutes of discovery. The SN reached a peak brightness ofM_V∼ −17.3 mag, and has an estimated⁵⁶Ni mass of 0.04M_⊙, typical values for normal Type II SNe. The modeling of the early light curve and the strong flash signatures present in the optical spectra indicate interaction with circumstellar material (CSM) created from a progenitor with a mass-loss rate of $\dot{M}\sim {10}^{-3}\text{–}{10}^{-2}{M}_{\odot }{\mathrm{y}\mathrm{r}}^{-1}$. There may also be some indication of late-time CSM interaction in the form of an emission line blueward of Hαseen in spectra around 200 days. The mass-loss rate of SN 2022jox is much higher than the values typically associated with quiescent mass loss from red supergiants, the known progenitors of Type II SNe, but is comparable to inferred values from similar core-collapse SNe with flash features, suggesting an eruptive event or a superwind in the progenitor in the months or years before explosion. 

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5. Multifaceted Sn–Sn bonding in the solid state. Synthesis and structural characterization of four new Ca–Li–Sn compounds

   https://doi.org/10.1039/C9DT02803J  

   Ovchinnikov, Alexander; Bobev, Svilen (October 2019, Dalton Transactions)

   null (Ed.)

   Four novel ternary phases have been prepared in the system Ca–Li–Sn using both the metal flux method and conventional high-temperature synthesis. Each of the obtained compositions represents its own (new) structure type, and the structures feature distinct polyanionic Sn units. Ca 4 LiSn 6 (space group Pbcm , Pearson symbol oP 44) accommodates infinite chains, made up of cyclopentane-like [Sn 5 ]-rings, which are bridged by Sn atoms. The Sn atoms in this structure are two- and three-bonded. The anionic substructure of Ca 9 Li 6+x Sn 13–x ( x ≈ 0.28, space group C 2/ m , Pearson symbol mS 56) displays extensive mixing of Li and Sn and combination of single-bonded and hypervalent interactions between the Sn atoms. Hypervalent bonding is also pronounced in the structure of the third compound, Ca 2 LiSn 3 (space group Pmm 2, Pearson symbol oP 18) with quasi-two-dimensional polyanionic subunits and a variety of coordination environments of the Sn atoms. One-dimensional [Sn 10 ]-chains with an intricate topology of cis - and trans -Sn–Sn bonds exist in the structure of Ca 9–x Li 2 Sn 10 ( x ≈ 0.16, space group C 2/ m , Pearson symbol mS 42), and the Sn–Sn bonding in this case demonstrates the characteristics of an intermediate between single- and double- bond-order. The peculiarities of the bonding are discussed in the context of the Zintl approach, which captures the essence of the main chemical interactions. The electronic structures of all four compounds have also been analyzed in full detail using first-principles calculations. 

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