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Silvotti, R.,Schuh, S.,Kim, S.-L.,Lutz, R.,Reed, M.,Benatti, S.,Janulis, R.,Lanteri, L.,Østensen, R.,Marsh, T. R.,Dhillon, V. S.,Paparo, M.,Molnar, L. Springer-Verlag 2018 Astronomy and astrophysics Vol.611 No.-
<P>V391 Peg (alias HS 2201+2610) is a subdwarf B (sdB) pulsating star that shows both <I>p</I>- and <I>g</I>-modes. By studying the arrival times of the <I>p</I>-mode maxima and minima through the O-C method, in a previous article the presence of a planet was inferred with an orbital period of 3.2 years and a minimum mass of 3.2 <I>M</I>Jup. Here we present an updated O-C analysis using a larger data set of 1066 h of photometric time series (~2.5× larger in terms of the number of data points), which covers the period between 1999 and 2012 (compared with 1999-2006 of the previous analysis). Up to the end of 2008, the new O-C diagram of the main pulsation frequency (<I>f</I>1) is compatible with (and improves) the previous two-component solution representing the long-term variation of the pulsation period (parabolic component) and the giant planet (sine wave component). Since 2009, the O-C trend of <I>f</I>1 changes, and the time derivative of the pulsation period (<I>p</I><SUP>.</SUP>) passes from positive to negative; the reason of this change of regime is not clear and could be related to nonlinear interactions between different pulsation modes. With the new data, the O-C diagram of the secondary pulsation frequency (<I>f</I>2) continues to show two components (parabola and sine wave), like in the previous analysis. Various solutions are proposed to fit the O-C diagrams of <I>f</I>1 and <I>f</I>2, but in all of them, the sinusoidal components of <I>f</I>1 and <I>f</I>2 differ or at least agree less well than before. The nice agreement found previously was a coincidence due to various small effects that are carefully analyzed. Now, with a larger dataset, the presence of a planet is more uncertain and would require confirmation with an independent method. The new data allow us to improve the measurement of <I>p</I><SUP>.</SUP> for <I>f</I>1 and <I>f</I>2: using only the data up to the end of 2008, we obtain <I>p</I><SUP>.</SUP>1 = (1.34 ± 0.04) × 10<SUP>−12</SUP> and <I>p</I><SUP>.</SUP>2 = (1.62 ± 0.22) × 10<SUP>−12</SUP>. The long-term variation of the two main pulsation periods (and the change of sign of <I>p</I><SUP>.</SUP>1) is visible also in direct measurements made over several years. The absence of peaks near <I>f</I>1 in the Fourier transform and the secondary peak close to <I>f</I>2 confirm a previous identification as <I>l</I> = 0 and <I>l</I> = 1, respectively, and suggest a stellar rotation period of about 40 days. The new data allow constraining the main <I>g</I>-mode pulsation periods of the star.</P>
Lutz, M.F.M.,Lange, J.S.,Pennington, M.,Bettoni, D.,Brambilla, N.,Crede, V.,Eidelman, S.,Gillitzer, A.,Gradl, W.,Lang, C.B.,Metag, V.,Nakano, T.,Nieves, J.,Neubert, S.,Oka, M.,Olsen, S.L.,Pappagallo, North Holland Pub. Co 2016 Nuclear physics. A Vol.948 No.-
<P>We report on the EMMI Rapid Reaction Task Force meeting 'Resonances in QCD', which took place at GSI October 12-14,2015. A group of 26 people met to discuss the physics of resonances in QCD. The aim of the meeting was defined by the following three key questions: What is needed to understand the physics of resonances in QCD? Where does QCD lead us to expect resonances with exotic quantum numbers? What experimental efforts are required to arrive at a coherent picture? For light mesons and baryons only those with up, down and strange quark content were considered. For heavy-light and heavy-heavy meson systems, those with charm quarks were the focus. This document summarizes the discussions by the participants, which in turn led to the coherent conclusions we present here. (C) 2016 Elsevier B.V. All rights reserved.</P>
Tiwari Anshul,Wang Alberta L.,Li Jiang,Lutz Sharon M.,Kho Alvin T,Weiss Scott T,Tantisira Kelan G,McGeachie Michael J. 대한천식알레르기학회 2021 Allergy, Asthma & Immunology Research Vol.13 No.4
Objective MicroRNAs (miRs) are small non-coding RNA molecules of around 18–22 nucleotides that are key regulators of many biologic processes, particularly inflammation. The purpose of this study was to determine the association of circulating miRs from asthmatic children with seasonal variation in allergic inflammation and asthma symptoms. Methods We used available small RNA sequencing on blood serum from 398 children with mild-to-moderate asthma from the Childhood Asthma Management Program. We used seasonal asthma symptom data at the study baseline and allergen affection status from baseline skin prick tests as primary outcomes. We identified differentially expressed (DE) miRs between pairs of seasons using DESeq2. Regression analysis was used to identify associations between allergy status to specific seasonal allergens and DE miRs in 4 seasons and between seasonal asthma symptom data and DE miRs. We performed pathway enrichment analysis for target genes of the DE miRs using DAVID. Results After quality control, 398 samples underwent differential analysis between the 4 seasons. We found 52 unique miRs from a total of 81 DE miRs across seasons. Further investigation of the association between these miRs and sensitization to seasonal allergens using skin prick tests revealed that 26 unique miRs from a total of 38 miRs were significantly associated with a same-season allergen. Comparison between seasonal asthma symptom data revealed that 2 of these 26 miRs also had significant associations with asthma symptoms in the same seasons: miR-328-3p (P < 0.03) and let-7d-3p (P < 0.05). Enrichment analysis showed that the most enriched pathway clusters were Rap1, Ras, and MAPK signaling pathways. Conclusion Our results show seasonal variation in miR-328-3p and let-7d-3p are significantly associated with seasonal asthma symptoms and seasonal allergies. These indicate a potentially protective role for let-7d-3p and a deleterious role for miR-328-3p in asthmatics sensitized to mulberry. Further work will determine whether these miRs are drivers or results of the allergic response.
Hyperfine interaction of individual atoms on a surface
Willke, Philip,Bae, Yujeong,Yang, Kai,Lado, Jose L.,Ferró,n, Alejandro,Choi, Taeyoung,Ardavan, Arzhang,Ferná,ndez-Rossier, Joaquí,n,Heinrich, Andreas J.,Lutz, Christopher P. American Association for the Advancement of Scienc 2018 Science Vol.362 No.6412
<P>Taking advantage of nuclear spins for electronic structure analysis, magnetic resonance imaging, and quantum devices hinges on knowledge and control of the surrounding atomic-scale environment. We measured and manipulated the hyperfine interaction of individual iron and titanium atoms placed on a magnesium oxide surface by using spin-polarized scanning tunneling microscopy in combination with single-atom electron spin resonance. Using atom manipulation to move single atoms, we found that the hyperfine interaction strongly depended on the binding configuration of the atom. We could extract atom-and position-dependent information about the electronic ground state, the state mixing with neighboring atoms, and properties of the nuclear spin. Thus, the hyperfine spectrum becomes a powerful probe of the chemical environment of individual atoms and nanostructures.</P>
Electrically controlled nuclear polarization of individual atoms
Yang, Kai,Willke, Philip,Bae, Yujeong,Ferró,n, Alejandro,Lado, Jose L.,Ardavan, Arzhang,Ferná,ndez-Rossier, Joaquí,n,Heinrich, Andreas J.,Lutz, Christopher P. Nature Publishing Group 2018 Nature nanotechnology Vol.13 No.12
Performance of the CREAM-III Calorimeter
Moo Hyun Lee,Ho Seok Ahn,Ganel, O.,Ji Hye Han,Jeon, J.A.,Chan Ho Kim,Ki Chun Kim,Lutz, L.,Malinin, A.,GoWoon Na,Shinwoo Nam,Park, I.H.,Na Hee Park,Eun-Suk Seo,Vartanyan, A.,Walpole, P.,Jayoung Wu,Jong IEEE 2009 IEEE transactions on nuclear science Vol.56 No.3
<P>Cosmic Ray Energetics And Mass (CREAM) is a balloon-borne experiment to directly measure the elemental spectra of protons to iron nuclei with energies up to ~ 10<SUP>15</SUP> eV. Energies of these cosmic-ray particles are measured by an ionization calorimeter comprised of 20 layers of 1 radiation length thick tungsten plates and 20 layers of 0.5 mm diameter scintillating fibers. Each tungsten plate is 500 times 500 times 3.5 mm<SUP>3</SUP> and the fibers are grouped into fifty 1 cm wide ribbons. After construction, the CREAM-III calorimeter was tested at CERN, the European high energy physics lab, in the H2 beam line of the SPS. Following the CERN test, the calorimeter was integrated into the CREAM-III instrument, and flown successfully in the 3rd flight of the project, during the 2007/8 Antarctic campaign. We present the performance of the CREAM-III calorimeter in lab and beam tests.</P>
The First Flight of the CREAM Silicon Charge Detector
N.H. Park,양종만,G. Bigongiari,박환배,김홍주,H.S. Ahn,박일흥,J. A. Jeon,J. H. Han,J. H. Hyun,J. J. Beatty,J. K. Lee,J. T. Childers,K. C. Kim,K. I. Seon,민경욱,L. Lutz,M. A. DuVernois,M. H. Lee,M.G. Begliesi,N. B. Co 한국물리학회 2006 THE JOURNAL OF THE KOREAN PHYSICAL SOCIETY Vol.49 No.2I
The CREAM (Cosmic Ray Energetics And Mass) experiment was constructed for the measurement of high-energy cosmic rays in the energy range between 1012 and 1015 eV. As a long duration balloon payload, the CREAM had its first successful flight in December 2004 from McMurdo Station, Antarctica. For the charge measurement of incident cosmic-ray particles entering the calorimeter module, a layer of the SCD (Silicon Charge Detector) made of 2912 silicon pixels was built with an active area of 779 × 795 mm2. This paper describes the performance of the SCD during the 2004-2005 flight.? The CREAM (Cosmic Ray Energetics And Mass) experiment was constructed for the measurement of high-energy cosmic rays in the energy range between 1012 and 1015 eV. As a long duration balloon payload, the CREAM had its first successful flight in December 2004 from McMurdo Station, Antarctica. For the charge measurement of incident cosmic-ray particles entering the calorimeter module, a layer of the SCD (Silicon Charge Detector) made of 2912 silicon pixels was built with an active area of 779 × 795 mm2. This paper describes the performance of the SCD during the 2004-2005 flight.?