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Background: There has been rapid growth of chiropractors pursuing career opportunities in both public and private hospitals and other integrated care settings. Chiropractors that prosper in integrated care settings deliver patient-centered care, focus on the institutional mission, understand and adhere to organizational rules, and are proficient in navigating complex systems. The Council on Chiropractic Education Accreditation Standards do not outline specific meta-competencies for integrated care clinical training. Objective: The purpose of this study was to develop preliminary integrated health care competencies for DC programs to guide the advancement of clinical chiropractic education. Methods: A systematic literature search was performed. Articles were screened for eligibility and extracted in duplicate. Domains and seed statements were generated from this literature, piloted at a conference workshop, and evaluated via a modified Delphi consensus process. Of 42 invited, 36 chiropractors participated as panelists. Public comment period yielded 20 comments, none resulting in substantive changes to the competencies. Results: Of 1718 citations, 23 articles met eligibility criteria. After 2 modified Delphi rounds, consensus was reached on all competency statements. A total of 78 competency statements were agreed upon, which encompassed 4 domains and 11 subdomains. The 4 domains were: 1) Collaboration, (2) Clinical Excellence, (3) Communication, and (4) Systems Administration. Conclusion: We identified 78 preliminary competencies appropriate for preparing DC students and early career chiropractors for clinical practice in integrated healthcare settings. Educational programs may consider these competencies for curricular design and reform to strengthen DC program graduates for integrated practice, advanced training, and employment. [ABSTRACT FROM AUTHOR]

Observations from NASA's Solar Dynamic Observatory Atmospheric Imaging Assembly were employed to investigate targeted physical properties of coronal active region structures across the majority of solar cycle 24 (From 2010 May to end of 2020 December). This is the largest consistent study to date which analyses emergent trends in structural width, location, and occurrence rate by performing an automatic and long-term examination of observable coronal and chromospheric limb features within equatorial active region belts across four extreme ultraviolet wavelengths (171, 193, 211, and 304 Å). This has resulted in over 30 000 observed coronal structures and hence allows for the production of spatial and temporal distributions focused upon the rise, peak, and decay activity phases of solar cycle 24. Employing a self-organized-criticality approach as a descriptor of coronal structure formation, power-law slopes of structural widths versus frequency are determined, ranging from -1.6 to -3.3 with variations of up to 0.7 found between differing periods of the solar cycle, compared to a predicted Fractal Diffusive Self-Organized Criticality (FD-SOC) value of -1.5. The North–South hemispheric asymmetry of these structures was also examined with the Northern hemisphere exhibiting activity that is peaking earlier and decaying slower than the Southern hemisphere, with a characteristic 'butterfly' pattern of coronal structures detected. This represents the first survey of coronal structures performed across an entire solar cycle, demonstrating new techniques available to examine the composition of the corona by latitude in varying wavelengths. [ABSTRACT FROM AUTHOR]

Nanoflares are thought to be one of the prime candidates that can heat the solar corona to its multimillion kelvin temperature. Individual nanoflares are difficult to detect with the present generation of instruments, but their presence can be inferred by comparing simulated nanoflare-heated plasma emissions with the observed emission. Using HYDRAD coronal loop simulations, we model the emission from an X-ray bright point (XBP) observed by the Marshall Grazing Incidence X-ray Spectrometer (MaGIXS), along with the nearest available observations from the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO) and the X-Ray Telescope (XRT) on board the Hinode observatory. The length and magnetic field strength of the coronal loops are derived from the linear force-free extrapolation of the observed photospheric magnetogram by the Helioseismic and Magnetic Imager on board SDO. Each loop is assumed to be heated by random nanoflares, whose magnitude and frequency are determined by the loop length and magnetic field strength. The simulation results are then compared and matched against the measured intensity from AIA, XRT, and MaGIXS. Our model results indicate the observed emission from the XBP under study could be well matched by a distribution of nanoflares with average delay times 1500–3000 s. Further, we demonstrate the high sensitivity of MaGIXS and XRT for diagnosing the heating frequency using this method, while AIA passbands are found to be the least sensitive. [ABSTRACT FROM AUTHOR]

Coronal loop observations have existed for many decades yet the precise shape of these fundamental coronal structures is still widely debated since the discovery that they appear to undergo negligible expansion between their footpoints and apex. In this work a selection of eight EUV loops and their 22 sub-element strands are studied from the second successful flight of NASA's High-resolution Coronal Imager (Hi-C 2.1). Four of the loops correspond to open fan structures with the other four considered to be magnetically closed loops. Width analysis is performed on the loops and their sub-resolution strands using our method of fitting multiple Gaussian profiles to cross-sectional intensity slices. It is found that while the magnetically closed loops and their sub-element strands do not expand along their observable length, open fan structures may expand an additional 150% of their initial width. Following recent work, the Pearson correlation coefficient between peak intensity and loop/strand width are found to be predominantly positively correlated for the loops (≈88%) and their sub-element strands (≈80%). These results align with the hypothesis of Klimchuk & DeForest that loops and—for the first time—their sub-element strands have approximately circular cross-sectional profiles. [ABSTRACT FROM AUTHOR]

Previous work utilizing NASA's High-resolution Coronal Imager (Hi-C 2.1) 172 Å observations revealed that, even at the increased spatial scales available in the dataset, there may be evidence for coronal structures that are still not fully resolved. In this follow-up study, cross-section slices of coronal strands are taken across the Hi-C 2.1 field of view. Following previous loop-width studies, the background emission is removed to isolate the coronal strands. The resulting intensity variations are reproduced by simultaneously fitting multiple Gaussian profiles using a nonlinear least-squares curve-fitting method. In total, 183 Gaussian profiles are examined for possible structures that are hinted at in the data. The full width at half maximum is determined for each Gaussian, which are then collated and analyzed. The most frequent structural widths are ≈450–575 km with 47% of the strand widths beneath NASA's Solar Dynamics Observatory Atmospheric Imaging Assembly (AIA) resolving scale (600–1000 km). Only 17% reside beneath an AIA pixel width (435 km) with just 6% of the strands at the Hi-C 2.1 resolving scale (≈220–340 km). These results suggest that non-Gaussian shaped cross-sectional emission profiles observed by Hi-C 2.1 are the result of multiple strands along the integrated line of sight that can be resolved, rather than being the result of even finer sub-resolution elements. [ABSTRACT FROM AUTHOR]

The High-resolution Coronal Imager (Hi-C) flew aboard a NASA sounding rocket on 2012 July 11 and captured roughly 345 s of high-spatial and temporal resolution images of the solar corona in a narrowband 193 Å channel. In this paper, we analyze a set of rapidly evolving loops that appear in an inter-moss region. We select six loops that both appear in and fade out of the Hi-C images during the short flight. From the Hi-C data, we determine the size and lifetimes of the loops and characterize whether these loops appear simultaneously along their length or first appear at one footpoint before appearing at the other. Using co-aligned, co-temporal data from multiple channels of the Atmospheric Imaging Assembly on the Solar Dynamics Observatory, we determine the temperature and density of the loops. We find the loops consist of cool (∼105 K), dense (∼1010 cm-3) plasma. Their required thermal energy and their observed evolution suggest they result from impulsive heating similar in magnitude to nanoflares. Comparisons with advanced numerical simulations indicate that such dense, cold and short-lived loops are a natural consequence of impulsive magnetic energy release by reconnection of braided magnetic field at low heights in the solar atmosphere. [ABSTRACT FROM AUTHOR]

The article presents the efforts of Mayor Michael R. Bloomberg to link the economic and workforce development in New York City. Bloomberg consolidated the adult workforce development programs with the Department of Small Business Services (SBS). He then established the New York City (NYC) Business Solutions under SBS to help employers in the competition. An overview of the three NYC Business Solutions programs is offered.

The article reflects on the Union Square Park Business Improvement District (BID) and the clean-up and revitalization effort which has brought the neighborhood back to life. It cites the strong corporate and institutional leadership of active stakeholders which anchored the renewal of the neighborhood from a virtual no-man's land to become a strong commercial and residential area.