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Jungclaus, A.,Gargano, A.,Grawe, H.,Taprogge, J.,Nishimura, S.,Doornenbal, P.,Lorusso, G.,Shimizu, Y.,Simpson, G. S.,Sö,derströ,m, P.-A.,Sumikama, T.,Xu, Z. Y.,Baba, H.,Browne, F.,Fukuda, N.,G American Physical Society 2016 Physical Review C Vol.93 No.4
<P>For the first time, the gamma decay of excited states has been observed in a nucleus situated in the quadrant south-east of doubly magic Sn-132, a region in which experimental information so far is limited to ground-state properties. Six gamma rays with energies of 50, 86, 103, 227, 357, and 602 keV were observed following the beta-delayed neutron emission from Cd-133(85), populated in the projectile fission of a U-238 beam at the Radioactive Isotope Beam Factory at RIKEN within the EURICA project. The new experimental information is compared to the results of a modern realistic shell-model calculation, the first one in this region very far from stability, focusing in particular on the pi 0g(9/2)(-1) circle times nu 1f(7/2) particle-hole multiplet in In-132(83). In addition, theoretical estimates based on a scaling of the two-body matrix elements for the pi h(11/2)(-1) circle times nu g(9/2) analog multiplet in Tl-208(127), one major proton and one major neutron shell above, are presented.</P>
Quintero Noda, C.,Villanueva, G. L.,Katsukawa, Y.,Solanki, S. K.,Orozco Suá,rez, D.,Ruiz Cobo, B.,Shimizu, T.,Oba, T.,Kubo, M.,Anan, T.,Ichimoto, K.,Suematsu, Y. Springer-Verlag 2018 Astronomy and astrophysics Vol.610 No.-
<P>Of the two solar lines, K I<I>D</I>1 and <I>D</I>2, almost all attention so far has been devoted to the <I>D</I>1 line, as <I>D</I>2 is severely affected by an O2 atmospheric band. This, however, makes the latter appealing for balloon and space observations from above (most of) the Earth’s atmosphere. We estimate the residual effect of the O2 band on the K I<I>D</I>2 line at altitudes typical for stratospheric balloons. Our aim is to study the feasibility of observing the 770 nm window. Specifically, this paper serves as a preparation for the third flight of the Sunrise balloon-borne observatory. The results indicate that the absorption by O2 is still present, albeit much weaker, at the expected balloon altitude. We applied the obtained O2 transmittance to K I<I>D</I>2 synthetic polarimetric spectra and found that in the absence of line-of-sight motions, the residual O2 has a negligible effect on the K I<I>D</I>2 line. On the other hand, for Doppler-shifted K I<I>D</I>2 data, the residual O2 might alter the shape of the Stokes profiles. However, the residual O2 absorption is sufficiently weak at stratospheric levels that it can be divided out if appropriate measurements are made, something that is impossible at ground level. Therefore, for the first time with Sunrise III, we will be able to perform polarimetric observations of the K I<I>D</I>2 line and, consequently, we will have improved access to the thermodynamics and magnetic properties of the upper photosphere from observations of the K I lines.</P>