48,997 results on '"Williams, J."'
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2. 11 Approaching, Contextualizing, and Embodying Interpretive Practice in Subcultural Studies
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Williams, J. Patrick
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- 2024
3. Part IV Conclusion
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Williams, J. Patrick
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- 2024
4. 10 Intimacy, Exchange, and Friendship as Sensitizing Concepts: Interpreting and Teaching Subcultures through Ethnographic Fieldwork
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Williams, J. Patrick
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- 2024
5. 7 The Dynamic Meaning of Subculture among DIY Indonesian Musicians
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Williams, J. Patrick
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- 2024
6. Part III Embodying Interpretive Practice
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Williams, J. Patrick
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- 2024
7. 9 Let's All Be Friends: Emotional Labor and Insider Research in Punk Subculture
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Williams, J. Patrick
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- 2024
8. 8 That's Not Punk! Authenticity, Older Punk Women, and the ‘Doing' of Punk Scholarship
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Williams, J. Patrick
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- 2024
9. 6 Interpreting Chinese Punk: From Doing Nothing to Hermit Lifestyle
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Williams, J. Patrick
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- 2024
10. 5 Still Crazy After All Those Years: A Trajectory of Discourses on Youth Subcultures in Korea, from Exclusion to Recognition to Legitimization
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Williams, J. Patrick
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- 2024
11. 4 No More Heroes: Portuguese Punk and the Notion of Subculture in the Global South
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Williams, J. Patrick
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- 2024
12. Part II Contextualizing Interpretive Practice
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Williams, J. Patrick
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- 2024
13. 3 Ghosts in the Machine: (Post)subculture and the ‘Problem' of Contemporary Youth
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Williams, J. Patrick
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- 2024
14. 1 Making Sense of Subcultures: Interpretive Practice and/in Subcultural Theory
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Williams, J. Patrick
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- 2024
15. Part I Approaching Interpretive Practice
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Williams, J. Patrick
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- 2024
16. 2 Subculture, Scene, Lifestyle, or Movement? Conceptualizing Straight Edge from Insider and Academic Perspectives
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Williams, J. Patrick
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- 2024
17. Acknowledgments
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Williams, J. Patrick
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- 2024
18. Series Editors' Preface: Interpretive Lenses in Sociology—On the Multidimensional Foundations of Meaning in Social Life
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Williams, J. Patrick
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- 2024
19. Notes on Contributors
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Williams, J. Patrick
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- 2024
20. Table of Contents
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Williams, J. Patrick
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- 2024
21. Series Page, Title Page, Copyright
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Williams, J. Patrick
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- 2024
22. Cover
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Williams, J. Patrick
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- 2024
23. Intermediate mass T Tauri disk masses and a comparison to their Herbig disk descendants
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Stapper, L. M., Hogerheijde, M. R., van Dishoeck, E. F., Vioque, M., Williams, J. P., and Ginski, C.
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Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Solar and Stellar Astrophysics - Abstract
The precursors of Herbig stars are called Intermediate Mass T Tauri (IMTT) stars, which have spectral types later than F, but stellar masses between 1.5 and 5 M_\odot, and will eventually become Herbig stars with spectral types of A and B. ALMA Band 6 and 7 archival data are obtained for 34 IMTT disks with continuum observations, 32 of which have at least 12CO, 13CO, or C18O observations although most of them at quite shallow integrations. The disk integrated flux together with a stellar luminosity scaled disk temperature are used to obtain a total disk dust mass by assuming optically thin emission. Using thermochemical Dust And LInes (DALI) models from previous work, we additionally obtain gas masses of 10/35 of the IMTT disks based on the CO isotopologues. The IMTT disks in this study have the same dust mass and radius distributions as Herbig disks. The dust mass of the IMTT disks is higher compared to that of the T Tauri disks, as is also found for the Herbig disks. No differences in dust mass are found for group I versus group II disks, in contrast to Herbig disks. The disks for which a gas mass could be determined show similar high mass disks as for the Herbig disks. Comparing the disk dust and gas mass distributions to the mass distribution of exoplanets shows that there also is not enough dust mass in disks around intermediate mass stars to form the massive exoplanets. On the other hand there is more than enough gas to form the atmospheres of exoplanets. We conclude that the sampled IMTT disk population is almost indistinguishable compared to Herbig disks, as their disk masses are the same, even though these are younger objects. Based on this, we conclude that planet formation is already well on its way in these objects, and thus planet formation should start early on in the lifetime of Herbig disks., Comment: Accepted for publication in Astronomy and Astrophysics. 16 pages, 12 figures, plus appendices
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- 2024
24. Coulomb Excitation of $^{80}$Sr and the limits of the $N = Z = 40$ island of deformation
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Russell, R., Heery, J., Henderson, J., Wadsworth, R., Kaneko, K., Shimizu, N., Mizusaki, T., Sun, Y., Andreoiu, C., Annen, D. W., Avaa, A. A., Ball, G. C., Bildstein, V., Buck, S., Cousins, C., Garnsworthy, A. B., Gillespie, S. A., Greaves, B., Grimes, A., Hackman, G., Hughes, R. O., Jenkins, D. G., Kowalewski, T. M., Martin, M. S., Müller-Gatermann, C., Murias, J. R., Murillo-Morales, S., Pascu, S., Rhodes, D. M., Smallcombe, J., Spagnoletti, P., Svensson, C. E., Wallis, B., Williams, J., Wu, C. Y., and Yates, D.
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Nuclear Experiment ,Nuclear Theory - Abstract
The region of $N\approx Z\approx 40$ has long been associated with strongly deformed nuclear configurations. The presence of this strong deformation was recently confirmed through lifetime measurements in $N\approx Z$ Sr and Zr nuclei. Theoretically, however, these nuclei present a challenge due to the vast valence space required to incorporate all deformation driving interactions. Recent state-of-the-art predictions indicate a near axial prolate deformation for $N=Z$ and $N=Z+2$ nuclei between $N=Z=36$ and $N=Z=40$. In this work we investigate the shores of this island of deformation through a sub-barrier Coulomb excitation study of the $N=Z+4$ nucleus, \textsuperscript{80}Sr. Extracting a spectroscopic quadrupole moment of $Q_s(2^+_1) = 0.45^{+0.83}_{-0.88}$~eb, we find that \textsuperscript{80}Sr is inconsistent with significant axial prolate deformation. This indicates that the predicted region of strong prolate deformation around $N=Z=40$ is tightly constrained to the quartet of nuclei: \textsuperscript{76,78}Sr and \textsuperscript{78,80}Zr., Comment: Submitted to Physics Letters B
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- 2024
25. Discovery of an accretion streamer and a slow wide-angle outflow around FU Orionis
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Hales, A. S., Gupta, A., Ruiz-Rodriguez, D., Williams, J. P., Perez, S., Cieza, L., Gonzalez-Ruilova, C., Pineda, J. E., Santamaria-Miranda, A., Tobin, J., Weber, P., Zhu, Z., and Zurlo, A.
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Astrophysics - Solar and Stellar Astrophysics ,Astrophysics - Astrophysics of Galaxies - Abstract
We present ALMA 12-m, 7-m & Total Power (TP) Array observations of the FU Orionis outbursting system, covering spatial scales ranging from 160 to 25,000 au. The high-resolution interferometric data reveals an elongated $^{12}$CO(2-1) feature previously observed at lower resolution in $^{12}$CO(3-2). Kinematic modeling indicates that this feature can be interpreted as an accretion streamer feeding the binary system. The mass infall rate provided by the streamer is significantly lower than the typical stellar accretion rates (even in quiescent states), suggesting that this streamer alone is not massive enough to sustain the enhanced accretion rates characteristic of the outbursting class prototype. The observed streamer may not be directly linked to the current outburst but rather a remnant of a previous, more massive streamer that may have contributed enough to the disk mass to render it unstable and trigger FU Ori's outburst. The new data detects, for the first time, a vast, slow-moving carbon monoxide molecular outflow emerging from this object. To accurately assess the outflow properties (mass, momentum, kinetic energy), we employed $^{13}$CO(2-1) data to correct for optical depth effects. The analysis indicates that the outflow corresponds to swept-up material not associated with the current outburst, similar to slow-molecular outflows observed around other FUor and Class I protostellar objects.
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- 2024
26. Numerical Simulations for Fractional Differential Equations of Higher Order and a Wright-Type Transformation
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Nacianceno, M., Oraby, T., Rodrigo, H., Sepulveda, Y., Sifuentes, J., Suazo, E., Stuck, T., and Williams, J.
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Mathematics - Numerical Analysis ,Mathematical Physics - Abstract
In this work, a new relationship is established between the solutions of higher fractional differential equations and a Wright-type transformation. Solutions could be interpreted as expected values of functions in a random time process. As applications, we solve the fractional beam equation, fractional electric circuits with special functions as external sources, and derive dAlemberts formula for the fractional wave equation. Due to this relationship, we present two methods for simulating solutions of fractional differential equations. The two approaches use the interpretation of the Caputo derivative of a function as a Wright-type transformation of the higher derivative of the function. In the first approach, we use the Runge-Kutta method of hybrid orders 4 and 5 to solve ordinary differential equations combined with the Monte Carlo integration to conduct the Wrighttype transformation. The second method uses a feedforward neural network to simulate the fractional differential equation.
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- 2024
27. Anatomy of the Class I protostar L1489 IRS with NOEMA -- I. Disk, streamers, outflow(s) and bubbles at 3mm
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Tanious, M., Gal, R. Le, Neri, R., Faure, A., Gupta, A., Law, C. J., Huang, J., Cuello, N., Williams, J. P., and Ménard, F.
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Astrophysics - Solar and Stellar Astrophysics - Abstract
Over the past few years, chemical studies have revealed multiple structures in the vicinity of young stellar objects (YSOs). It has become evident that specific physical conditions are associated with the emission of particular molecular lines, allowing us to use molecular probes of the YSO physics. Consequently, chemical surveys are now necessary to fully constrain the origin of the observed structures. Several surveys have been conducted to explore the chemistry of YSOs, focusing on Class 0 and Class II objects. However, our knowledge of intermediate objects, that are Class I objects, remains limited. To bridge the gap and establish the relationship between observed structures and molecular line emission at the Class I evolutionary stage, we investigate the spatial distribution of key molecular gas species in the low-mass Class I protostar L1489 IRS (IRAS 04016+2610), a source part of the ChemYSO survey. We performed a 3mm line survey at high spatial and high spectral resolution using the NOEMA interferometer and the IRAM-30m telescope. We present here the ten brightest lines of our survey, in which we identified a new ~ 3 000 au long streamer in HC3N, C2H, and c-C3H2 emission, likely associated with more localized accretion shocks probed in SO. In addition, two ~ 10 000 au bubbles are seen with the dense molecular tracers HCO+, CS, and HCN around the YSO. Additionally, potential indicators of a second outflow appear in CS and HCN emission, but its nature remains to be confirmed. The late infall identified at large scales may originate from the nearby prestellar core L1489 and is likely responsible for the formation of an external warped disk in this system. The detection of a potential second outflow could be the direct evidence of a binary system. Finally, we hypothesize that the bubbles may result from the magnetic pressure as observed in numerical simulations., Comment: 16 pages, 12 figures, accepted for publication in Astronomy & Astrophysics
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- 2024
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28. The SPHERE view of the Taurus star-forming region
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Garufi, A., Ginski, C., van Holstein, R. G., Benisty, M., Manara, C. F., Pérez, S., Pinilla, P., Ribas, Á., Weber, P., Williams, J., Cieza, L., Dominik, C., Facchini, S., Huang, J., Zurlo, A., Bae, J., Hagelberg, J., Henning, Th., Hogerheijde, M. R., Janson, M., Ménard, F., Messina, S., Meyer, M. R., Pinte, C., Quanz, S. P., Rigliaco, E., Roccatagliata, V., Schmid, H. M., Szulágyi, J., van Boekel, R., Wahhaj, Z., Antichi, J., Baruffolo, A., and Moulin, T.
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Astrophysics - Astrophysics of Galaxies ,Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Solar and Stellar Astrophysics - Abstract
The sample of planet-forming disks observed by high-contrast imaging campaigns over the last decade is mature enough to enable the demographical analysis of individual star-forming regions. We present the full census of Taurus sources with VLT/SPHERE polarimetric images available. The whole sample sums up to 43 targets (of which 31 have not been previously published) corresponding to one-fifth of the Class II population in Taurus and about half of such objects that are observable. A large fraction of the sample is apparently made up of isolated faint disks (equally divided between small and large self-shadowed disks). Ambient signal is visible in about one-third of the sample. This probes the interaction with the environment and with companions or the outflow activity of the system. The central portion of the Taurus region almost exclusively hosts faint disks, while the periphery also hosts bright disks interacting with their surroundings. The few bright disks are found around apparently older stars. The overall picture is that the Taurus region is in an early evolutionary stage of planet formation. Yet, some objects are discussed individually, as in an intermediate or exceptional stage of the disk evolution. This census provides a first benchmark for the comparison of the disk populations in different star forming regions., Comment: Accepted by A&A
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- 2024
29. The SPHERE view of the Orion star-forming region
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Valegard, P. -G., Ginski, C., Derkink, A., Garufi, A., Dominik, C., Ribas, A., Williams, J. P., Benisty, M., Birnstiel, T., Facchini, S., Columba, G., Hogerheijde, M., Van Holstein, R. G., Huang, J., Kenworthy, M., Manara, C. F., Pinilla, P., Rab, Ch., Sulaiman, R., and Zurlo, A.
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Astrophysics - Solar and Stellar Astrophysics ,Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Astrophysics of Galaxies - Abstract
We present SPHERE/IRDIS H-band data for a sample of 23 stars in the Orion Star forming region observed within the DESTINYS (Disk Evolution Study Through Imaging of Nearby Young Stars) program. We use polarization differential imaging in order to detect scattered light from circumstellar dust. From the scattered light observations we characterize the disk orientation, radius and contrast. We analyse the disks in context of the stellar parameters and the environment of the Orion star-forming region. We use ancillary X-shooter spectroscopic observations to characterize the central stars in the systems. We furthermore use a combination of new and archival ALMA mm-continuum observations to characterize the dust masses present in the circumstellar disks. Within our sample we detect extended circumstellar disks in 10 of 23 systems. Of these, three are exceptionally extended (V351 Ori, V599 Ori and V1012 Ori) and show scattered light asymmetries which may indicate perturbations by embedded planets or (in the case of V599 Ori) by an outer stellar companion. Our high resolution imaging observations are also sensitive to close (sub)stellar companions and we detect 9 such objects in our sample of which 5 were previously unknown. We find in particular a possible sub-stellar companion (either a very low mass star or a high mass brown dwarf) 137 au from the star RY Ori. We find a strong anti-correlation between disk detection and multiplicity, with only 2 of our 10 disk detections located in stellar multiple systems. We also find a correlation between scattered light contrast and the millimetre flux suggesting that disks that have a high dust content are typically bright in near-infrared scattered light. Conversely we do not find significant correlations between scattered light contrast of the disks and the stellar mass or age., Comment: Accepted by A&A
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- 2024
30. The SPHERE view of the Chamaeleon I star-forming region
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Ginski, C., Garufi, A., Benisty, M., Tazaki, R., Dominik, C., Ribas, A., Engler, N., Birnstiel, T., Chauvin, G., Columba, G., Facchini, S., Goncharov, A., Hagelberg, J., Henning, T., Hogerheijde, M., van Holstein, R. G., Huang, J., Muto, T., Pinilla, P., Kanagawa, K., Kim, S., Kurtovic, N., Langlois, M., Manara, C., Milli, J., Momose, M., Orihara, R., Pawellek, N., Pinte, C., Rab, C., Schmidt, T. O. B., Snik, F., Wahhaj, Z., Williams, J., and Zurlo, A.
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Astrophysics - Astrophysics of Galaxies ,Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Solar and Stellar Astrophysics - Abstract
We used VLT/SPHERE to observe 20 systems in the Cha I cloud in polarized scattered light in the near-infrared. We combined the scattered light observations with existing literature data on stellar properties and with archival ALMA continuum data to study trends with system age and dust mass. We also connected resolved near-infrared observations with the spectral energy distributions of the systems. In 13 of the 20 systems included in this study we detected resolved scattered light signals from circumstellar dust. For the CR Cha, CT Cha, CV Cha, SY Cha, SZ Cha, and VZ Cha systems we present the first detailed descriptions of the disks in scattered light. The observations found typically smooth or faint disks, often with little substructure, with the notable exceptions of SZ Cha, which shows an extended multiple-ringed disk, and WW Cha, which shows interaction with the cloud environment. New high S/N K- band observations of the HD 97048 system in our survey reveal a significant brightness asymmetry that may point to disk misalignment and subsequent shadowing of outer disk regions, possibly related to the suggested planet candidate in the disk. We resolve for the first time the stellar binary in the CS Cha system. Multiple wavelength observations of the disk around CS Cha have revealed that the system contains small, compact dust grains that may be strongly settled, consistent with numerical studies of circumbinary disks. We find in our sample that there is a strong anti-correlation between the presence of a (close) stellar companion and the detection of circumstellar material with five of our seven nondetections located in binary systems., Comment: Accepted by A&A
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- 2024
31. Cross-shell excited configurations in the structure of 34Si
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Lubna, R. S., Garnsworthy, A. B., Tripathi, Vandana, Ball, G. C., Natzke, C. R., Rocchini, M., Andreoiu, C., Bhattacharjee, S. S., Dillmann, I., Garcia, F. H., Gillespie, S. A., Hackman, G., Griffin, C. J., Leckenby, G., Miyagi, T., Olaizola, B., Porzio, C., Rajabali, M. M., Saito, Y., Spagnoletti, P., Tabor, S. L., Umashankar, R., Vedia, V., Volya, A., Williams, J., and Yates, D.
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Nuclear Experiment - Abstract
The cross-shell excited states of $^{34}$Si have been investigated via $\beta$-decays of the $4^-$ ground state and the $1^+$ isomeric state of $^{34}$Al. Since the valence protons and valence neutrons occupy different major shells in the ground state as well as the intruder $1^+$ isomeric state of $^{34}$Al, intruder levels of $^{34}$Si are populated via allowed $\beta$ decays. Spin assignments to such intruder levels of $^{34}$Si were established through $\gamma$-$\gamma$ angular correlation analysis for the negative parity states with dominant configurations $(\nu d_{3/2})^{-1} \otimes (\nu f_{7/2})^{1}$ as well as the positive parity states with dominant configurations $(\nu sd)^{-2} \otimes (\nu f_{7/2}p_{3/2})^2$. The configurations of such intruder states play crucial roles in our understanding of the $N=20$ shell gap evolution. A configuration interaction model derived from the FSU Hamiltonian was utilized in order to interpret the intruder states in $^{34}$Si. Shell model interaction derived from a more fundamental theory with the Valence Space In Medium Similarity Renormalization Group (VS-IMSRG) method was also employed to interpret the structure of $^{34}$Si.
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- 2024
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32. Comparing indirect methods for black hole masses in AGN: the good, the bad, and the ugly
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Gliozzi, M., Williams, J. K., Akylas, A., Papadakis, I. E., Shuvo, O. I., Halavatkar, A., and Alt, A.
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Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics - Astrophysics of Galaxies - Abstract
The black hole mass MBH is crucial in constraining the growth of supermassive BHs within their host galaxies. Since direct measurements of MBH with dynamical methods are restricted to a limited number of nearly quiescent nearby galaxies and a small minority of active galactic nuclei (AGN), we must rely on indirect methods. In this work, we utilize an unbiased, volume-limited, hard X-ray selected sample of AGN to compare the reliability of some commonly used indirect methods, emphasising those that can be applied to obscured AGN. Based on a subsample of AGN with MBH determined via dynamical methods, our study suggests that X-ray based techniques, such as the scaling method and the one based on the variability measured through the excess variance, are in good agreement with the dynamical methods. On the other hand, the M-sigma correlation based on inactive galaxies tends to systematically overestimate MBH, regardless of the level of obscuration. We provide a correcting factor that produces an acceptable agreement with dynamical values and can be used to quickly correct the MBH computed with this method. We also derive an alternative M-sigma correlation based on this unbiased sample of AGN with a slope considerably shallower than the ones obtained using inactive galaxies, suggesting that the latter correlation may not be appropriate to compute the MBH in AGN. Finally, we find that no quick fix can be applied to correct the MBH obtained from the fundamental plane of black hole activity, casting doubts on the reliability of this method., Comment: 15 pages, 9 figures, 3 tables, Accepted for publication in MNRAS
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- 2023
33. Identifying the spin trapped character of the $^{32}$Si isomeric state
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Williams, J., Hackman, G., Starosta, K., Lubna, R. S., Choudhary, Priyanka, Srivastava, P. C., Andreoiu, C., Annen, D., Asch, H., Badanage, M. D. H. K. G., Ball, G. C., Beuschlein, M., Bidaman, H., Bildstein, V., Coleman, R., Garnsworthy, A. B., Greaves, B., Leckenby, G., Karayonchev, V., Martin, M. S., Natzke, C., Petrache, C. M., Radich, A., Raleigh-Smith, E., Rhodes, D., Russell, R., Satrazani, M., Spagnoletti, P., Svensson, C. E., Tam, D., Wu, F., Yates, D., and Yu, Z.
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Nuclear Experiment - Abstract
The properties of a nanosecond isomer in $^{32}$Si, disputed in previous studies, depend on the evolution of proton and neutron shell gaps near the `island of inversion'. We have placed the isomer at 5505.2(2) keV with $J^{\pi} = 5^-$, decaying primarily via an $E3$ transition to the $2^+_1$ state. The $E3$ strength of 0.0841(10) W.u. is unusually small and suggests that this isomer is dominated by the $(\nu d_{3/2})^{-1} \otimes (\nu f_{7/2})^{1}$ configuration, which is sensitive to the $N=20$ shell gap. A newly observed $4^+_1$ state is placed at 5881.4(13) keV; its energy is enhanced by the $Z=14$ subshell closure. This indicates that the isomer is located in a `yrast trap', a feature rarely seen at low mass numbers., Comment: Accepted, Physical Review C
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- 2023
34. Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): HD 34700 A unveils an inner ring
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Columba, G., Rigliaco, E., Gratton, R., Mesa, D., D'Orazi, V., Ginski, C., Engler, N., Williams, J. P., Bae, J., Benisty, M., Birnstiel, T., Delorme, P., Dominik, C., Facchini, S., Menard, F., Pinilla, P., Rab, C., Ribas, Á., Squicciarini, V., van Holstein, R. G., and Zurlo, A.
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Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Solar and Stellar Astrophysics - Abstract
Context. The study of protoplanetary disks is fundamental to understand their evolution and interaction with the surrounding environment, and to constrain planet formation mechanisms. Aims. We aim at characterising the young binary system HD 34700 A, which shows a wealth of structures. Methods. Taking advantage of the high-contrast imaging instruments SPHERE at the VLT, LMIRCam at the LBT, and of ALMA observations, we analyse this system at multiple wavelengths. We study the rings and spiral arms morphology and the scattering properties of the dust. We discuss the possible causes of all the observed features. Results. We detect for the first time, in the H${\alpha}$ band, a ring extending from $\sim$65 au to ${\sim}$120 au, inside the ring already known from recent studies. These two have different physical and geometrical properties. Based on the scattering properties, the outer ring may consist of grains of typical size $a_{out} > 4 {\mu}m$, while the inner ring of smaller grains ($a_{in} <= 0.4 {\mu m}$). Two extended logarithmic spiral arms stem from opposite sides of the disk. The outer ring appears as a spiral arm itself, with a variable radial distance from the centre and extended substructures. ALMA data confirm the presence of a millimetric dust substructure centred just outside the outer ring, and detect misaligned gas rotation patterns for HD 34700 A and B. Conclusions. The complexity of HD 34700 A, revealed by the variety of observed features, suggests the existence of one or more disk-shaping physical mechanisms. Possible scenarios, compatible with our findings, involve the presence inside the disk of a yet undetected planet of several Jupiter masses and the system interaction with the surroundings by means of gas cloudlet capture or flybys. Further observations with JWST/MIRI or ALMA (gas kinematics) could shed more light on these., Comment: Accepted for publication on A&A. 14 + 5 pages, 9 + 7 figures (text + appendix)
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- 2023
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35. Testing external photoevaporation in the $\sigma$-Orionis cluster with spectroscopy and disk mass measurements
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Maucó, K., Manara, C. F., Ansdell, M., Bettoni, G., Claes, R., Alcala, J., Miotello, A., Facchini, S., Haworth, T. J., Lodato, G., and Williams, J. P.
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Astrophysics - Solar and Stellar Astrophysics ,Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Astrophysics of Galaxies - Abstract
The evolution of protoplanetary disks is regulated by an interplay of several processes, either internal to the system or related to the environment. As most of the stars and planets have formed in massive stellar clusters, studying the effects of UV radiation on disk evolution is of paramount importance. Here we test the impact of external photoevaporation on the evolution of disks in the $\sigma$ Orionis cluster by conducting the first combined large-scale UV to IR spectroscopic and mm-continuum survey of this region. We study a sample of 50 targets located at increasing distances from the central, OB system $\sigma$ Ori. We combine new VLT/X-Shooter spectra with new and previously published ALMA measurements of disk dust and gas fluxes and masses. We confirm the previously found decrease of $M_{\rm dust}$ in the inner $\sim$0.5 pc of the cluster. This is particularly evident when considering the disks around the more massive stars ($\ge$ 0.4 $M_{\odot}$), where those located in the inner part ($<$ 0.5 pc) have $M_{\rm dust}$ about an order of magnitude lower than the more distant ones. About half of the sample is located in the region of the $\dot{M}_{\rm acc}$ vs $M_{\rm disk}$ expected by models of external photoevaporation, namely showing shorter disk lifetimes. These are observed for all targets with projected separation from $\sigma$ Ori $<$ 0.5 pc, proving that the presence of a massive stellar system affects disk evolution. External photoevaporation is a viable mechanism to explain the observed shorter disk lifetimes and lower $M_{\rm dust}$ in the inner $\sim$0.5 pc of the cluster. Follow-up observations of the low stellar mass targets are crucial to confirm the dependence of the external photoevaporation process with stellar host mass. This work confirms that the effects of external photoevaporation are significant down to impinging radiation as low as $\sim 10^{4}$ G$_0$., Comment: Accepted for publication on Astronomy & Astrophysics. 13 pages, 7 figures + appendix. Abstract abridged to meet arXiv requirements
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- 2023
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36. Cross-shell excited configurations in the structure of Si34
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Lubna, RS, Garnsworthy, AB, Tripathi, Vandana, Ball, GC, Natzke, CR, Rocchini, M, Andreoiu, C, Bhattacharjee, SS, Dillmann, I, Garcia, FH, Gillespie, SA, Hackman, G, Griffin, CJ, Leckenby, G, Miyagi, T, Olaizola, B, Porzio, C, Rajabali, MM, Saito, Y, Spagnoletti, P, Tabor, SL, Umashankar, R, Vedia, V, Volya, A, Williams, J, and Yates, D
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Nuclear and Plasma Physics ,Synchrotrons and Accelerators ,Physical Sciences ,Nuclear and plasma physics - Abstract
The cross-shell excited states of Si34 have been investigated via β decays of the 4- ground state and the 1+ isomeric state of Al34. Since the valence protons and valence neutrons occupy different major shells in the ground state as well as the intruder 1+ isomeric state of Al34, intruder levels of Si34 are populated via allowed β decays. Spin assignments to such intruder levels of Si34 were established through γ-γ angular correlation analysis for the negative-parity states with dominant configurations (νd3/2)-1⊗ - (νf7/2)1 as well as the positive-parity states with dominant configurations (νsd)-2⊗ - (νf7/2p3/2)2. The configurations of such intruder states play crucial roles in our understanding of the N=20 shell gap evolution. A configuration interaction model derived from the FSU Hamiltonian was utilized in order to interpret the intruder states in Si34. Shell model interaction derived from a more fundamental theory with the valence space in medium similarity renormalization group method was also employed to interpret the structure of Si34.
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- 2024
37. Customary Law and Chieftainship in Southern Africa
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Williams, J. Michael
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- 2024
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38. Spirals and clumps in V960 Mon: signs of planet formation via gravitational instability around an FU Ori star?
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Weber, P., Pérez, S., Zurlo, A., Miley, J., Hales, A., Cieza, L., Principe, D., Cárcamo, M., Garufi, A., Kóspál, Á., Takami, M., Kastner, J., Zhu, Z., and Williams, J.
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Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Solar and Stellar Astrophysics - Abstract
The formation of giant planets has traditionally been divided into two pathways: core accretion and gravitational instability. However, in recent years, gravitational instability has become less favored, primarily due to the scarcity of observations of fragmented protoplanetary disks around young stars and low occurrence rate of massive planets on very wide orbits. In this study, we present a SPHERE/IRDIS polarized light observation of the young outbursting object V960 Mon. The image reveals a vast structure of intricately shaped scattered light with several spiral arms. This finding motivated a re-analysis of archival ALMA 1.3 mm data acquired just two years after the onset of the outburst of V960 Mon. In these data, we discover several clumps of continuum emission aligned along a spiral arm that coincides with the scattered light structure. We interpret the localized emission as fragments formed from a spiral arm under gravitational collapse. Estimating the mass of solids within these clumps to be of several Earth masses, we suggest this observation to be the first evidence of gravitational instability occurring on planetary scales. This study discusses the significance of this finding for planet formation and its potential connection with the outbursting state of V960 Mon., Comment: Published in ApJL. 11 pages, 4 figures. Images available as fits files at https://github.com/yemsnucleus/V960_Mon_ApJL
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- 2023
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39. Differing needs for Advance Care Planning in the Veterans Health Administration: use of latent class analysis to identify subgroups to enhance Advance Care Planning via Group Visits for veterans
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Matthieu, Monica M., Ounpraseuth, Songthip T., Williams, J. Silas, Hu, Bo, Adkins, David A., Oliver, Ciara M., Taylor, Laura D., McCullough, Jane Ann, Mallory, Mary J., Smith, Ian D., Suarez, Jack H., and Garner, Kimberly K.
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- 2024
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40. Interpersonal symptoms in adolescence depression across Asian and European regions: a network approach
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Cheung, H. N., Asgarabad, M. Habibi, Ho, W. S., Zibetti, M. R., Li, S. T. K., Stella, W. Y. Chan, and Williams, J. M.
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- 2024
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41. Mindfulness Intervention with African-American Caregivers at a Head Start Program: An Acceptability and Feasibility Study
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Mathis, Erin T., Hawkins, Jay, Charlot-Swilley, Dominique, Spencer, Travis, Lingo, Kaira Jewel, Trachtenberg, Dave, McPherson, Satyani K. L., Domitrovich, Celene E., Shapiro, Amanda, Williams, J. Corey, and Biel, Matthew G.
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- 2024
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42. Cross Sections of the $^{83}$Rb(p,$\gamma)^{84}$Sr and $^{84}$Kr(p,$\gamma)^{85}$Rb Reactions at Energies Characteristic of the Astrophysical $\gamma$ Process
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Williams, M., Davids, B., Lotay, G., Nishimura, N., Rauscher, T., Gillespie, S. A., Alcorta, M., Amthor, A. M., Ball, G. C., Bhattacharjee, S. S., Bildstein, V., Catford, W. N., Doherty, D. T., Esker, N. E., Garnsworthy, A. B., Hackman, G., Hudson, K., Lennarz, A., Natzke, C., Olaizola, B., Psaltis, A., Svensson, C. E., Williams, J., Walter, D., and Yates, D.
- Subjects
Nuclear Experiment ,Astrophysics - Solar and Stellar Astrophysics - Abstract
We have measured the cross section of the $^{83}$Rb(p,$\gamma)^{84}$Sr radiative capture reaction in inverse kinematics using a radioactive beam of $^{83}$Rb at incident energies of 2.4 and $2.7 A$ MeV. Prior to the radioactive beam measurement, the $^{84}$Kr(p,$\gamma)^{85}$Rb radiative capture reaction was measured in inverse kinematics using a stable beam of $^{84}$Kr at an incident energy of $2.7 A$ MeV. The effective relative kinetic energies of these measurements lie within the relevant energy window for the $\gamma$ process in supernovae. The central values of the measured partial cross sections of both reactions were found to be $0.17-0.42$ times the predictions of statistical model calculations. Assuming the predicted cross section at other energies is reduced by the same factor leads to a slightly higher calculated abundance of the $p$ nucleus $^{84}$Sr, caused by the reduced rate of the $^{84}$Sr($\gamma$,p)$^{83}$Rb reaction derived from the present measurement., Comment: 11 pages, 11 figures. arXiv admin note: text overlap with arXiv:2109.06775
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- 2023
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43. Light-cone cuts and metricity conditions for a power-law spacetime in 2+1 and 3+1 dimensions
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Harriott, Tina A. and Williams, J. G.
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- 2024
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44. Search for central exclusive production of top quark pairs in proton-proton collisions at s = 13 TeV with tagged protons
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Tumasyan, A., Adam, W., Andrejkovic, J. W., Bergauer, T., Chatterjee, S., Damanakis, K., Dragicevic, M., Escalante Del Valle, A., Hussain, P. S., Jeitler, M., Krammer, N., Lechner, L., Liko, D., Mikulec, I., Paulitsch, P., Pitters, F. M., Schieck, J., Schöfbeck, R., Schwarz, D., Templ, S., Waltenberger, W., Wulz, C.-E., Darwish, M. R., Janssen, T., Kello, T., Rejeb Sfar, H., Van Mechelen, P., Bols, E. S., D’Hondt, J., De Moor, A., Delcourt, M., El Faham, H., Lowette, S., Moortgat, S., Morton, A., Müller, D., Sahasransu, A. R., Tavernier, S., Van Doninck, W., Vannerom, D., Clerbaux, B., De Lentdecker, G., Favart, L., Hohov, D., Jaramillo, J., Lee, K., Mahdavikhorrami, M., Makarenko, I., Malara, A., Paredes, S., Pétré, L., Postiau, N., Starling, E., Thomas, L., Vanden Bemden, M., Vander Velde, C., Vanlaer, P., Dobur, D., Knolle, J., Lambrecht, L., Mestdach, G., Niedziela, M., Rendón, C., Roskas, C., Samalan, A., Skovpen, K., Tytgat, M., Van Den Bossche, N., Vermassen, B., Wezenbeek, L., Benecke, A., Bruno, G., Bury, F., Caputo, C., David, P., Delaere, C., Donertas, I. S., Giammanco, A., Jaffel, K., Jain, Sa., Lemaitre, V., Mondal, K., Prisciandaro, J., Taliercio, A., Tran, T. T., Vischia, P., Wertz, S., Alves, G. A., Coelho, E., Hensel, C., Moraes, A., Rebello Teles, P., Aldá Júnior, W. L., Alves Gallo Pereira, M., Barroso Ferreira Filho, M., Brandao Malbouisson, H., Carvalho, W., Chinellato, J., Da Costa, E. M., Da Silveira, G. G., De Jesus Damiao, D., Dos Santos Sousa, V., Fonseca De Souza, S., Martins, J., Mora Herrera, C., Mota Amarilo, K., Mundim, L., Nogima, H., Santoro, A., Silva Do Amaral, S. M., Sznajder, A., Thiel, M., Torres Da Silva De Araujo, F., Vilela Pereira, A., Bernardes, C. A., Calligaris, L., Fernandez Perez Tomei, T. R., Gregores, E. M., Mercadante, P. G., Novaes, S. F., Padula, Sandra S., Aleksandrov, A., Hadjiiska, R., Iaydjiev, P., Misheva, M., Rodozov, M., Shopova, M., Sultanov, G., Dimitrov, A., Ivanov, T., Litov, L., Pavlov, B., Petkov, P., Petrov, A., Shumka, E., Cheng, T., Javaid, T., Mittal, M., Yuan, L., Ahmad, M., Bauer, G., Hu, Z., Lezki, S., Yi, K., Chen, G. M., Chen, H. S., Chen, M., Iemmi, F., Jiang, C. H., Kapoor, A., Liao, H., Liu, Z.-A., Milosevic, V., Monti, F., Sharma, R., Tao, J., Thomas-Wilsker, J., Wang, J., Zhang, H., Zhao, J., Agapitos, A., An, Y., Ban, Y., Chen, C., Levin, A., Li, C., Li, Q., Lyu, X., Mao, Y., Qian, S. J., Sun, X., Wang, D., Xiao, J., Yang, H., Li, J., Lu, M., You, Z., Gao, X., Leggat, D., Okawa, H., Zhang, Y., Lin, Z., Lu, C., Xiao, M., Avila, C., Barbosa Trujillo, D. A., Cabrera, A., Florez, C., Fraga, J., Mejia Guisao, J., Ramirez, F., Rodriguez, M., Ruiz Alvarez, J. D., Giljanovic, D., Godinovic, N., Lelas, D., Puljak, I., Antunovic, Z., Kovac, M., Sculac, T., Brigljevic, V., Chitroda, B. K., Ferencek, D., Majumder, D., Roguljic, M., Starodumov, A., Susa, T., Attikis, A., Christoforou, K., Kole, G., Kolosova, M., Konstantinou, S., Mousa, J., Nicolaou, C., Ptochos, F., Razis, P. A., Rykaczewski, H., Saka, H., Finger, M., Finger, Jr., M., Kveton, A., Ayala, E., Carrera Jarrin, E., Elgammal, S., Ellithi Kamel, A., Mahmoud, M. A., Mohammed, Y., Bhowmik, S., Dewanjee, R. K., Ehataht, K., Kadastik, M., Lange, T., Nandan, S., Nielsen, C., Pata, J., Raidal, M., Tani, L., Veelken, C., Eerola, P., Kirschenmann, H., Voutilainen, M., Bharthuar, S., Brücken, E., Havukainen, J., Kim, M. S., Kinnunen, R., Lampén, T., Lassila-Perini, K., Lehti, S., Lindén, T., Lotti, M., Martikainen, L., Myllymäki, M., Ott, J., Rantanen, M. m., Siikonen, H., Tuominen, E., Tuominiemi, J., Luukka, P., Petrow, H., Tuuva, T., Amendola, C., Besancon, M., Couderc, F., Dejardin, M., Denegri, D., Faure, J. L., Ferri, F., Ganjour, S., Gras, P., Hamel de Monchenault, G., Jarry, P., Lohezic, V., Malcles, J., Rander, J., Rosowsky, A., Sahin, M. Ö., Savoy-Navarro, A., Simkina, P., Titov, M., Beaudette, F., Buchot Perraguin, A., Busson, P., Cappati, A., Charlot, C., Damas, F., Davignon, O., Diab, B., Falmagne, G., Fontana Santos Alves, B. A., Ghosh, S., Granier de Cassagnac, R., Hakimi, A., Harikrishnan, B., Liu, G., Motta, J., Nguyen, M., Ochando, C., Portales, L., Rembser, J., Salerno, R., Sarkar, U., Sauvan, J. B., Sirois, Y., Tarabini, A., Vernazza, E., Zabi, A., Zghiche, A., Agram, J.-L., Andrea, J., Apparu, D., Bloch, D., Bourgatte, G., Brom, J.-M., Chabert, E. C., Collard, C., Darej, D., Goerlach, U., Grimault, C., Le Bihan, A.-C., Van Hove, P., Beauceron, S., Bernet, C., Blancon, B., Boudoul, G., Carle, A., Chanon, N., Choi, J., Contardo, D., Depasse, P., Dozen, C., El Mamouni, H., Fay, J., Gascon, S., Gouzevitch, M., Grenier, G., Ille, B., Laktineh, I. B., Lethuillier, M., Mirabito, L., Perries, S., Sordini, V., Torterotot, L., Vander Donckt, M., Verdier, P., Viret, S., Adamov, G., Lomidze, I., Tsamalaidze, Z., Botta, V., Feld, L., Klein, K., Lipinski, M., Meuser, D., Pauls, A., Röwert, N., Teroerde, M., Diekmann, S., Dodonova, A., Eich, N., Eliseev, D., Erdmann, M., Fackeldey, P., Fasanella, D., Fischer, B., Hebbeker, T., Hoepfner, K., Ivone, F., Lee, M. y., Mastrolorenzo, L., Merschmeyer, M., Meyer, A., Mondal, S., Mukherjee, S., Noll, D., Novak, A., Nowotny, F., Pozdnyakov, A., Rath, Y., Redjeb, W., Reithler, H., Schmidt, A., Schuler, S. C., Sharma, A., Vigilante, L., Wiedenbeck, S., Zaleski, S., Dziwok, C., Flügge, G., Haj Ahmad, W., Hlushchenko, O., Kress, T., Nowack, A., Pooth, O., Stahl, A., Ziemons, T., Zotz, A., Aarup Petersen, H., Aldaya Martin, M., Asmuss, P., Baxter, S., Bayatmakou, M., Behnke, O., Bermúdez Martínez, A., Bhattacharya, S., Bin Anuar, A. A., Blekman, F., Borras, K., Brunner, D., Campbell, A., Cardini, A., Cheng, C., Colombina, F., Consuegra Rodríguez, S., Correia Silva, G., De Silva, M., Didukh, L., Eckerlin, G., Eckstein, D., Estevez Banos, L. I., Filatov, O., Gallo, E., Geiser, A., Giraldi, A., Greau, G., Grohsjean, A., Guglielmi, V., Guthoff, M., Jafari, A., Jomhari, N. Z., Kaech, B., Kasem, A., Kasemann, M., Kaveh, H., Kleinwort, C., Kogler, R., Komm, M., Krücker, D., Lange, W., Leyva Pernia, D., Lipka, K., Lohmann, W., Mankel, R., Melzer-Pellmann, I.-A., Mendizabal Morentin, M., Metwally, J., Meyer, A. B., Milella, G., Mormile, M., Mussgiller, A., Nürnberg, A., Otarid, Y., Pérez Adán, D., Raspereza, A., Ribeiro Lopes, B., Rübenach, J., Saggio, A., Saibel, A., Savitskyi, M., Scham, M., Scheurer, V., Schnake, S., Schütze, P., Schwanenberger, C., Shchedrolosiev, M., Sosa Ricardo, R. E., Stafford, D., Tonon, N., Van De Klundert, M., Vazzoler, F., Ventura Barroso, A., Walsh, R., Walter, D., Wang, Q., Wen, Y., Wichmann, K., Wiens, L., Wissing, C., Wuchterl, S., Yang, Y., Zimermmane Castro Santos, A., Aggleton, R., Albrecht, A., Albrecht, S., Antonello, M., Bein, S., Benato, L., Bonanomi, M., Connor, P., De Leo, K., Eich, M., El Morabit, K., Feindt, F., Fröhlich, A., Garbers, C., Garutti, E., Hajheidari, M., Haller, J., Hinzmann, A., Jabusch, H. R., Kasieczka, G., Klanner, R., Korcari, W., Kramer, T., Kutzner, V., Lange, J., Lobanov, A., Matthies, C., Mehta, A., Moureaux, L., Mrowietz, M., Nigamova, A., Nissan, Y., Paasch, A., Pena Rodriguez, K. J., Rieger, M., Rieger, O., Schleper, P., Schröder, M., Schwandt, J., Stadie, H., Steinbrück, G., Tews, A., Wolf, M., Bechtel, J., Brommer, S., Burkart, M., Butz, E., Caspart, R., Chwalek, T., Dierlamm, A., Droll, A., Faltermann, N., Giffels, M., Gosewisch, J. O., Gottmann, A., Hartmann, F., Horzela, M., Husemann, U., Keicher, P., Klute, M., Koppenhöfer, R., Maier, S., Mitra, S., Müller, Th., Neukum, M., Quast, G., Rabbertz, K., Rauser, J., Savoiu, D., Schnepf, M., Seith, D., Shvetsov, I., Simonis, H. J., Trevisani, N., Ulrich, R., van der Linden, J., Von Cube, R. F., Wassmer, M., Weber, M., Wieland, S., Wolf, R., Wozniewski, S., Wunsch, S., Anagnostou, G., Assiouras, P., Daskalakis, G., Kyriakis, A., Stakia, A., Diamantopoulou, M., Karasavvas, D., Kontaxakis, P., Manousakis-Katsikakis, A., Panagiotou, A., Papavergou, I., Saoulidou, N., Theofilatos, K., Tziaferi, E., Vellidis, K., Vourliotis, E., Zisopoulos, I., Bakas, G., Chatzistavrou, T., Kousouris, K., Papakrivopoulos, I., Tsipolitis, G., Zacharopoulou, A., Adamidis, K., Bestintzanos, I., Evangelou, I., Foudas, C., Gianneios, P., Kamtsikis, C., Katsoulis, P., Kokkas, P., Kosmoglou Kioseoglou, P. G., Manthos, N., Papadopoulos, I., Strologas, J., Csanád, M., Farkas, K., Gadallah, M. M. A., Lökös, S., Major, P., Mandal, K., Pásztor, G., Rádl, A. J., Surányi, O., Veres, G. I., Bartók, M., Bencze, G., Hajdu, C., Horvath, D., Sikler, F., Veszpremi, V., Beni, N., Czellar, S., Karancsi, J., Molnar, J., Szillasi, Z., Teyssier, D., Raics, P., Ujvari, B., Csorgo, T., Novak, T., Babbar, J., Bansal, S., Beri, S. B., Bhatnagar, V., Chaudhary, G., Chauhan, S., Dhingra, N., Gupta, R., Kaur, A., Kaur, A., Kaur, H., Kaur, M., Kumar, S., Kumari, P., Meena, M., Sandeep, K., Sheokand, T., Singh, J. B., Singla, A., Virdi, A. K., Ahmed, A., Bhardwaj, A., Choudhary, B. C., Gola, M., Keshri, S., Kumar, A., Naimuddin, M., Priyanka, P., Ranjan, K., Saumya, S., Shah, A., Baradia, S., Barman, S., Bhattacharya, S., Bhowmik, D., Dutta, S., Dutta, S., Gomber, B., Maity, M., Palit, P., Rout, P. K., Saha, G., Sahu, B., Sarkar, S., Behera, P. K., Behera, S. C., Kalbhor, P., Komaragiri, J. R., Kumar, D., Muhammad, A., Panwar, L., Pradhan, R., Pujahari, P. R., Sharma, A., Sikdar, A. K., Tiwari, P. C., Verma, S., Naskar, K., Aziz, T., Das, I., Dugad, S., Kumar, M., Mohanty, G. B., Suryadevara, P., Banerjee, S., Chudasama, R., Guchait, M., Karmakar, S., Kumar, S., Majumder, G., Mazumdar, K., Mukherjee, S., Thachayath, A., Bahinipati, S., Das, A. K., Kar, C., Mal, P., Mishra, T., Muraleedharan Nair Bindhu, V. K., Nayak, A., Saha, P., Sur, N., Swain, S. K., Vats, D., Alpana, A., Dube, S., Kansal, B., Laha, A., Pandey, S., Rastogi, A., Sharma, S., Bakhshiansohi, H., Khazaie, E., Zeinali, M., Chenarani, S., Etesami, S. M., Khakzad, M., Mohammadi Najafabadi, M., Grunewald, M., Abbrescia, M., Aly, R., Aruta, C., Colaleo, A., Creanza, D., De Filippis, N., De Palma, M., Di Florio, A., Elmetenawee, W., Errico, F., Fiore, L., Iaselli, G., Ince, M., Maggi, G., Maggi, M., Margjeka, I., Mastrapasqua, V., My, S., Nuzzo, S., Pellecchia, A., Pompili, A., Pugliese, G., Radogna, R., Ramos, D., Ranieri, A., Selvaggi, G., Silvestris, L., Simone, F. M., Sözbilir, Ü., Stamerra, A., Venditti, R., Verwilligen, P., Abbiendi, G., Battilana, C., Bonacorsi, D., Borgonovi, L., Brigliadori, L., Campanini, R., Capiluppi, P., Castro, A., Cavallo, F. R., Cuffiani, M., Dallavalle, G. M., Diotalevi, T., Fabbri, F., Fanfani, A., Giacomelli, P., Giommi, L., Grandi, C., Guiducci, L., Lo Meo, S., Lunerti, L., Marcellini, S., Masetti, G., Navarria, F. L., Perrotta, A., Primavera, F., Rossi, A. M., Rovelli, T., Siroli, G. P., Costa, S., Di Mattia, A., Potenza, R., Tricomi, A., Tuve, C., Barbagli, G., Camaiani, B., Cassese, A., Ceccarelli, R., Ciulli, V., Civinini, C., D’Alessandro, R., Focardi, E., Latino, G., Lenzi, P., Lizzo, M., Meschini, M., Paoletti, S., Seidita, R., Sguazzoni, G., Viliani, L., Benussi, L., Bianco, S., Meola, S., Piccolo, D., Ferro, F., Mulargia, R., Robutti, E., Tosi, S., Benaglia, A., Boldrini, G., Brivio, F., Cetorelli, F., De Guio, F., Dinardo, M. E., Dini, P., Gennai, S., Ghezzi, A., Govoni, P., Guzzi, L., Lucchini, M. T., Malberti, M., Malvezzi, S., Massironi, A., Menasce, D., Moroni, L., Paganoni, M., Pedrini, D., Pinolini, B. S., Ragazzi, S., Redaelli, N., Tabarelli de Fatis, T., Zuolo, D., Buontempo, S., Carnevali, F., Cavallo, N., De Iorio, A., Fabozzi, F., Iorio, A. O. M., Lista, L., Paolucci, P., Rossi, B., Sciacca, C., Azzi, P., Bacchetta, N., Biasotto, M., Bortignon, P., Bragagnolo, A., Carlin, R., Checchia, P., Ciano, L., Dorigo, T., Fantinel, S., Gasparini, U., Grosso, G., Layer, L., Lusiani, E., Margoni, M., Meneguzzo, A. T., Pazzini, J., Ronchese, P., Rossin, R., Simonetto, F., Strong, G., Tosi, M., Yarar, H., Zanetti, M., Zotto, P., Zucchetta, A., Abu Zeid, S., Aimè, C., Braghieri, A., Calzaferri, S., Fiorina, D., Montagna, P., Re, V., Riccardi, C., Salvini, P., Vai, I., Vitulo, P., Asenov, P., Bilei, G. M., Ciangottini, D., Fanò, L., Magherini, M., Mantovani, G., Mariani, V., Menichelli, M., Moscatelli, F., Piccinelli, A., Presilla, M., Rossi, A., Santocchia, A., Spiga, D., Tedeschi, T., Azzurri, P., Bagliesi, G., Bertacchi, V., Bhattacharya, R., Bianchini, L., Boccali, T., Bruschini, D., Castaldi, R., Ciocci, M. A., D’Amante, V., Dell’Orso, R., Di Domenico, M. R., Donato, S., Giassi, A., Ligabue, F., Manca, E., Mandorli, G., Matos Figueiredo, D., Messineo, A., Musich, M., Palla, F., Parolia, S., Ramirez-Sanchez, G., Rizzi, A., Rolandi, G., Roy Chowdhury, S., Sarkar, T., Shafiei, N., Spagnolo, P., Tenchini, R., Tonelli, G., Venturi, A., Verdini, P. 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W., Mengke, T., Muthumuni, S., Peltola, T., Volobouev, I., Wang, Z., Whitbeck, A., Appelt, E., Greene, S., Gurrola, A., Johns, W., Melo, A., Romeo, F., Sheldon, P., Tuo, S., Velkovska, J., Viinikainen, J., Cardwell, B., Cox, B., Cummings, G., Hakala, J., Hirosky, R., Joyce, M., Ledovskoy, A., Li, A., Neu, C., Perez Lara, C. E., Tannenwald, B., Karchin, P. E., Poudyal, N., Banerjee, S., Black, K., Bose, T., Dasu, S., De Bruyn, I., Everaerts, P., Galloni, C., He, H., Herndon, M., Herve, A., Koraka, C. K., Lanaro, A., Loeliger, A., Loveless, R., Madhusudanan Sreekala, J., Mallampalli, A., Mohammadi, A., Mondal, S., Parida, G., Pinna, D., Savin, A., Shang, V., Sharma, V., Smith, W. H., Teague, D., Tsoi, H. F., Vetens, W., Afanasiev, S., Andreev, V., Andreev, Yu., Aushev, T., Azarkin, M., Babaev, A., Belyaev, A., Blinov, V., Boos, E., Budkouski, D., Bunichev, V., Bychkova, O., Chadeeva, M., Chekhovsky, V., Dermenev, A., Dimova, T., Dremin, I., Dubinin, M., Dudko, L., Epshteyn, V., Gavrilov, G., Gavrilov, V., Gninenko, S., Golovtcov, V., Golubev, N., Golutvin, I., Gorbunov, I., Gribushin, A., Ivanov, Y., Kachanov, V., Kardapoltsev, L., Karjavine, V., Karneyeu, A., Kim, V., Kirakosyan, M., Kirpichnikov, D., Kirsanov, M., Klyukhin, V., Konstantinov, D., Korenkov, V., Kozyrev, A., Krasnikov, N., Kuznetsova, E., Lanev, A., Levchenko, P., Litomin, A., Lukina, O., Lychkovskaya, N., Makarenko, V., Malakhov, A., Matveev, V., Murzin, V., Nikitenko, A., Obraztsov, S., Okhotnikov, V., Ovtin, I., Palichik, V., Parygin, P., Perelygin, V., Perfilov, M., Pivovarov, G., Popov, V., Popova, E., Radchenko, O., Rusinov, V., Savina, M., Savrin, V., Selivanova, D., Shalaev, V., Shmatov, S., Shulha, S., Skovpen, Y., Slabospitskii, S., Smirnov, V., Sosnov, D., Stepennov, A., Sulimov, V., Terkulov, A., Teryaev, O., Tlisova, I., Toms, M., Toropin, A., Uvarov, L., Uzunian, A., Vlasov, E., Volkov, P., Vorobyev, A., Voytishin, N., Yuldashev, B. S., Zarubin, A., Zhizhin, I., Zhokin, A., Antchev, G., Aspell, P., Atanassov, I., Avati, V., Baechler, J., Baldenegro Barrera, C., Berardi, V., Berretti, M., Borshch, V., Bossini, E., Bottigli, U., Bozzo, M., Burkhardt, H., Cafagna, F. S., Catanesi, M. G., Deile, M., De Leonardis, F., Doubek, M., Druzhkin, D., Eggert, K., Eremin, V., Fiergolski, A., Garcia, F., Georgiev, V., Giani, S., Grzanka, L., Hammerbauer, J., Isidori, T., Ivanchenko, V., Janda, M., Karev, A., Kašpar, J., Kaynak, B., Kopal, J., Kundrát, V., Lami, S., Linhart, R., Lindsey, C., Lokajíček, M. V., Losurdo, L., Lucas Rodríguez, F., Macrí, M., Malawski, M., Minafra, N., Minutoli, S., Misan, K., Naaranoja, T., Nemes, F., Niewiadomski, H., Oliveri, E., Oljemark, F., Oriunno, M., Österberg, K., Ozkorucuklu, S., Palazzi, P., Passaro, V., Peroutka, Z., Potok, O., Procházka, J., Quinto, M., Radermacher, E., Radicioni, E., Ravotti, F., Royon, C., Ruggiero, G., Saarikko, H., Samoylenko, V. D., Scribano, A., Široký, J., Smajek, J., Snoeys, W., Stefanovitch, R., Taylor, C., Tcherniaev, E., Turini, N., Urban, O., Vacek, V., Vavroch, O., Welti, J., Williams, J., and Zich, J.
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- 2024
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45. Genotype-by-Sex Interaction in the Regulation of High-Density Lipoprotein: The Framingham Heart Study
- Author
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Mosher, M. J, Martin, L. J, Cupples, L. A, Yang, Qiong, Dyer, Thomas D, Williams, J. T, and North, K. E
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- 2006
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46. An elongated quantum dot as a distributed charge sensor
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Patomäki, S. M., Williams, J., Berritta, F., Laine, C., Fogarty, M. A., Leon, R. C. C., Jussot, J., Kubicek, S., Chatterjee, A., Govoreanu, B., Kuemmeth, F., Morton, J. J. L., and Gonzalez-Zalba, M. F.
- Subjects
Condensed Matter - Mesoscale and Nanoscale Physics ,Physics - Applied Physics ,Quantum Physics - Abstract
Increasing the separation between semiconductor quantum dots offers scaling advantages by fa- cilitating gate routing and the integration of sensors and charge reservoirs. Elongated quantum dots have been utilized for this purpose in GaAs heterostructures to extend the range of spin-spin interactions. Here, we study a metal-oxide-semiconductor (MOS) device where two quantum dot arrays are separated by an elongated quantum dot (340 nm long, 50 nm wide). We monitor charge transitions of the elongated quantum dot by measuring radiofrequency single-electron currents to a reservoir to which we connect a lumped-element resonator. We operate the dot as a single electron box to achieve charge sensing of remote quantum dots in each array, separated by a distance of 510 nm. Simultaneous charge detection on both ends of the elongated dot demonstrates that the charge is well distributed across its nominal length, supported by the simulated quantum-mechanical electron density. Our results illustrate how single-electron boxes can be realised with versatile foot- prints that may enable novel and compact quantum processor layouts, offering distributed charge sensing in addition to the possibility of mediated coupling., Comment: 14 pages, 9 figures
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- 2023
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47. 15 Lunar Surface Processes
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Plescia, J. B., primary, Cahill, J., additional, Greenhagen, B., additional, Hayne, P., additional, Mahanti, P., additional, Robinson, M. S., additional, Spudis, P. D., additional, Siegler, M., additional, Stickle, A., additional, Williams, J. P., additional, Zanetti, M., additional, and Zellner, N., additional
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- 2024
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48. A fleet for the unmanned era
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Williams, J. Noel, LtCol, Ret
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SEA CONTROL SHIPS - Design ,PROCUREMENT - Navy - United States ,STRATEGY, NAVAL - United States - Abstract
illus tab bibliog
- Published
- 2014
49. Wide Variability in Dysplasia Detection Rate and Adherence to Seattle Protocol and Surveillance Recommendations in Barretts Esophagus: A Population-Based Analysis Using the GIQuIC National Quality Benchmarking Registry.
- Author
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Kolb, Jennifer, Davis, Christian, Williams, J, Holub, Jennifer, Shaheen, Nicholas, and Wani, Sachin
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Humans ,Barrett Esophagus ,Benchmarking ,Esophagoscopy ,Hyperplasia ,Registries ,Esophageal Neoplasms - Abstract
INTRODUCTION: Variability in adherence rates to the Seattle protocol and to surveillance interval recommendations, established quality indicators (QIs) in Barretts esophagus (BE), is unknown. METHODS: We evaluated endoscopist and site-based adherence rates to these QIs from January 2018 to May 2021 using the GI Quality Improvement Consortium national registry with matched endoscopy and pathology data. RESULTS: Across 153 practices with 572 endoscopists performing 20,155 endoscopies, adherence to the Seattle protocol varied by endoscopists (median 93.8%, IQR 18.9%) and by site (median 90.0%, IQR 20.1%). Adherence to appropriate surveillance intervals for nondysplastic BE also varied by endoscopist (median 82.4%, IQR 36.3%) and site (median 77.2%, IQR 29.8%). The overall dysplasia detection rate was 3.1% and varied among endoscopists and sites. DISCUSSION: These US population-based results can serve as a benchmark for quality initiatives and intervention trials aimed at improving outcomes for patients with BE.
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- 2023
50. Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): Scattered light detection of a possible disk wind in RY Tau
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Valegård, P. -G., Ginski, C., Dominik, C., Bae, J., Benisty, M., Birnstiel, T., Facchini, S., Garufi, A., Hogerheijde, M., van Holstein, R. G., Langlois, M., Manara, C. F., Pinilla, P., Rab, Ch., Ribas, Á., Waters, L. B. F. M., and Williams, J.
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Astrophysics - Solar and Stellar Astrophysics - Abstract
Disk winds are an important mechanism for accretion and disk evolution around young stars. The accreting intermediate-mass T-Tauri star RY Tau has an active jet and a previously known disk wind. Archival optical and new near-infrared observations of the RY Tau system show two horn-like components stretching out as a cone from RY Tau. Scattered light from the disk around RY Tau is visible in near-infrared but not seen at optical wavelengths. In the near-infrared, dark wedges that separates the horns from the disk, indicating we may see the scattered light from a disk wind. We use archived ALMA and SPHERE/ZIMPOL I-band observations combined with newly acquired SPEHRE/IRDIS H-band observations and available literature to build a simple geometric model of the RY Tau disk and disk wind. We use Monte Carlo radiative transfer modelling \textit{MCMax3D} to create comparable synthetic observations that test the effect of a dusty wind on the optical effect in the observations. We constrain the grain size and dust mass needed in the disk wind to reproduce the effect from the observations. A model geometrically reminiscent of a dusty disk wind with small micron to sub-micron size grains elevated above the disk can reproduce the optical effect seen in the observations. The mass in the obscuring component of the wind has been constrained to $1\times10^{-9} M_{\odot} \leq M \leq 5\times10^{-8} M_{\odot}$ which corresponds to a lower limit mass loss rate in the wind of about $\sim 1\times10^{-8}M_{\odot}\mathrm{yr}^{-1}$. While an illuminate dust cavity cannot be ruled out without measurements of the gas velocity, we argue that a magnetically launched disk wind is the most likely scenario., Comment: 11 pages, 5 figures
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- 2022
- Full Text
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