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Production by macrofauna associated with oyster reefs offers a multi-purpose indicator of ecosystem function, ecological integrity, and restoration success. We examined responses by oyster-reef-associated macrofauna to a hypoxic event across three subtidal oyster-reef complexes in western Mississippi Sound as part of a large-scale restoration program. Four hypotheses within the context of a Linear mixed model examined differences in the following: (1) the macrofauna relative to the hypoxic event; (2) subregions relative to the severity of hypoxia; (3) responses by key macrofaunal taxa; and (4) short-term macrofaunal recovery. Densities and production potential of the entire oyster-reef macrofaunal community as well as for six key taxa all abruptly decreased in connection with the hypoxic event. Overall, total production potential and total density were four-fold lower in the summer of 2015 during the hypoxic event than in the summer of 2014. The degree of macrofaunal impact corresponded with the severity of hypoxia on the landscape scale. Total density and total production averaged nearly three-fold lower and more than eight-fold lower respectively across two critically hypoxic reef complexes compared to the least affected reef complex. Taxon-specific responses depended on tolerances to hypoxia as well as modes of reproduction and dispersal. Short-term macrofaunal recovery indicated surprising ecological resilience relative to the hypoxic interruption. Detrimental macrofaunal effects ameliorated substantially within several months when total production potential was comparable to that of the previous year. However, the short-term recovery of key taxa varied with respect to the hypoxic event. Hypoxia-induced seasonal directionality reversed between summer 2015 and fall 2015, as evidenced by lower values for total density, total production, and the density and production of the larger-bodied crustaceans, Eurypanopeus and Palaemonetes. Secondary production offers a key functional indicator of multiple ecosystem services and an informative gauge of ecological disturbance. Associated macrofauna should be used more widely to assess the ecological function and recovery of oyster reefs. This study expands our understanding of a productive oyster reef ecosystem that is threatened by multiple environmental challenges. [ABSTRACT FROM AUTHOR]

We investigate the occurrence of the "extended solar cycle" (ESC) as it occurs in a host of observational data spanning 140 years. Investigating coronal, chromospheric, photospheric, and interior diagnostics, we develop a consistent picture of solar activity migration linked to the 22-year Hale (magnetic) cycle using superposed epoch analysis (SEA) and previously identified Hale cycle termination events as the key time for the SEA. Our analysis shows that the ESC and Hale cycle, as highlighted by the terminator-keyed SEA, is strongly recurrent throughout the entire observational record studied, some 140 years. Applying the same SEA method to the sunspot record confirms that Maunder's butterfly pattern is a subset of the underlying Hale cycle, strongly suggesting that the production of sunspots is not the fundamental feature of the Hale cycle, but the ESC is. The ESC (and Hale cycle) pattern highlights the importance of 55 ∘ latitude in the evolution, and possible production, of solar magnetism. [ABSTRACT FROM AUTHOR]

Booth (Solar Phys.296, 108, 2021; hereafter B21) is essentially a critique of the Hilbert transform techniques used in our paper (Leamon et al., Solar Phys.295, 36, 2020; hereafter L20) to predict the termination of solar cycles. Here we respond to his arguments; our methodology and parameter choices do extract a mathematically robust signature of terminators from the historical sunspot record. We agree that the attempt in L20 to extrapolate beyond the sunspot record gives a failed prediction for the next terminator of May 2020, and we identify both a possible cause and remedy here. However, we disagree with the B21 assessment that the likely termination of Solar Cycle 24 is two years after the date predicted in L20, and we show why. [ABSTRACT FROM AUTHOR]

The Interface Region Imaging Spectrograph (IRIS) has been obtaining near- and far-ultraviolet images and spectra of the solar atmosphere since July 2013. IRIS is the highest resolution observatory to provide seamless coverage of spectra and images from the photosphere into the low corona. The unique combination of near- and far-ultraviolet spectra and images at sub-arcsecond resolution and high cadence allows the tracing of mass and energy through the critical interface between the surface and the corona or solar wind. IRIS has enabled research into the fundamental physical processes thought to play a role in the low solar atmosphere such as ion–neutral interactions, magnetic reconnection, the generation, propagation, and dissipation of waves, the acceleration of non-thermal particles, and various small-scale instabilities. IRIS has provided insights into a wide range of phenomena including the discovery of non-thermal particles in coronal nano-flares, the formation and impact of spicules and other jets, resonant absorption and dissipation of Alfvénic waves, energy release and jet-like dynamics associated with braiding of magnetic-field lines, the role of turbulence and the tearing-mode instability in reconnection, the contribution of waves, turbulence, and non-thermal particles in the energy deposition during flares and smaller-scale events such as UV bursts, and the role of flux ropes and various other mechanisms in triggering and driving CMEs. IRIS observations have also been used to elucidate the physical mechanisms driving the solar irradiance that impacts Earth's upper atmosphere, and the connections between solar and stellar physics. Advances in numerical modeling, inversion codes, and machine-learning techniques have played a key role. With the advent of exciting new instrumentation both on the ground, e.g. the Daniel K. Inouye Solar Telescope (DKIST) and the Atacama Large Millimeter/submillimeter Array (ALMA), and space-based, e.g. the Parker Solar Probe and the Solar Orbiter, we aim to review new insights based on IRIS observations or related modeling, and highlight some of the outstanding challenges. [ABSTRACT FROM AUTHOR]

We study the solar wind helium-to-hydrogen abundance's ( A He ) relationship to solar cycle onset. Using OMNI/Lo data, we show that A He increases prior to sunspot number (SSN) minima. We also identify a rapid depletion and recovery in A He that occurs directly prior to cycle onset. This A He shutoff happens at approximately the same time across solar wind speeds ( v sw ) and the time between successive A He shutoffs is typically on the order of the corresponding solar cycle length. In contrast to A He 's v sw -dependent phase lag with respect to SSN (Alterman and Kasper, 2019), A He shutofff's concurrence across v sw likely implies it is independent of solar wind acceleration and driven by a mechanism near or below the photosphere. Using brightpoint (BP) measurements to provide context, we infer that A He shutoff is likely related to the overlap of adjacent solar cycles and the equatorial flux cancelation of the older, extended solar cycle during solar minima. [ABSTRACT FROM AUTHOR]

The Sun exhibits a well-observed modulation in the number of spots on its disk over a period of about 11 years. From the dawn of modern observational astronomy, sunspots have presented a challenge to understanding—their quasi-periodic variation in number, first noted 175 years ago, has stimulated community-wide interest to this day. A large number of techniques are able to explain the temporal landmarks, (geometric) shape, and amplitude of sunspot "cycles," however, forecasting these features accurately in advance remains elusive. Recent observationally-motivated studies have illustrated a relationship between the Sun's 22-year (Hale) magnetic cycle and the production of the sunspot cycle landmarks and patterns, but not the amplitude of the sunspot cycle. Using (discrete) Hilbert transforms on more than 270 years of (monthly) sunspot numbers we robustly identify the so-called "termination" events that mark the end of the previous 11-yr sunspot cycle, the enhancement/acceleration of the present cycle, and the end of 22-yr magnetic activity cycles. Using these we extract a relationship between the temporal spacing of terminators and the magnitude of sunspot cycles. Given this relationship and our prediction of a terminator event in 2020, we deduce that sunspot Solar Cycle 25 could have a magnitude that rivals the top few since records began. This outcome would be in stark contrast to the community consensus estimate of sunspot Solar Cycle 25 magnitude. [ABSTRACT FROM AUTHOR]

Using the McIntosh Archive of solar features, we analyze the evolution of coronal holes over more than three solar cycles. We demonstrate that coronal-hole positions and lifetimes change significantly on time scales from months to years, and that the pattern of these changes is clearly linked to the solar-activity cycle. We demonstrate that the lifetimes of low-latitude coronal holes are usually less than one rotation but may extend to almost three years. When plotted over time, the positions of low-latitude coronal holes that remain visible for over one rotation track the sunspot butterfly diagram in terms of their positions on the Sun over a solar cycle. Finally, we confirm that coronal holes do not in general rigidly rotate. [ABSTRACT FROM AUTHOR]

Purpose: Cervical cancer disproportionately burdens low-resource populations where access to quality screening services is limited. A greater understanding of sustainable approaches to implement cervical cancer screening services is needed.Methods: We conducted a systematized literature review of evaluations from cervical cancer screening programs implemented in resource-limited settings globally that included a formal evaluation and intention of program sustainment over time. We categorized the included studies using the continuum of implementation research framework which categorizes studies progressively from "implementation light" to more implementation intensive.Results: Fifty-one of 13,330 initially identified papers were reviewed with most study sites in low-resource settings of middle-income countries (94.1%) ,while 9.8% were in low-income countries. Across all studies, visual inspection of the cervix with acetic acid (58.8%) was the most prevalent screening method followed by cytology testing (39.2%). Demand-side (client and community) considerations were reported in 86.3% of the articles, while 68.6% focused scientific inquiry on the supply side (health service). Eighteen articles (35.3%) were categorized as "Informing Scale-up" along the continuum of implementation research.Conclusions: The number of cervical cancer screening implementation reports is limited globally, especially in low-income countries. The 18 papers we classified as Informing Scale-up provide critical insights for developing programs relevant to implementation outcomes. We recommend that program managers report lessons learnt to build collective implementation knowledge for cervical cancer screening services, globally. [ABSTRACT FROM AUTHOR]

Recent research has demonstrated the existence of a new type of solar event, the "terminator." Unlike the Sun's signature events, flares and coronal mass ejections, the terminator most likely originates in the solar interior, at or near the tachocline. The terminator signals the end of a magnetic activity cycle at the Sun's equator and the start of a sunspot cycle at mid-latitudes. Observations indicate that the time difference between these events is very short, less than a solar rotation, in the context of the sunspot cycle. As the (definitive) start and end point of solar activity cycles the precise timing of terminators should permit new investigations into the meteorology of our star's atmosphere. In this article we use a standard method in signal processing, the Hilbert transform, to identify a mathematically robust signature of terminators in sunspot records and in radiative proxies. Using a linear extrapolation of the Hilbert phase of the sunspot number and F10.7 cm solar radio flux time series we can achieve higher fidelity historical terminator timing than previous estimates have permitted. Further, this method presents a unique opportunity to project, from analysis of sunspot data, when the next terminator will occur, May 2020 (+ 4 , −1.5 months), and trigger the growth of Sunspot Cycle 25. [ABSTRACT FROM AUTHOR]

We present a new tool, the Solar Eclipse Image Standardisation and Sequencing (SEISS), developed to process multi-source total solar eclipse images by adjusting them to the same standard of size, resolution, and orientation. Furthermore, by analysing the eclipse images, we can determine the relative time between the observations and order them to create a movie of the observed total solar eclipse sequence. We successfully processed images taken at the 14 November 2012 total solar eclipse that occurred in Queensland, Australia, and created a short eclipse proto-movie. The SEISS tool was developed for the Eclipse Megamovie Project (EMP: ), with the goal of processing thousands of images taken by the public during solar eclipse events. EMP is a collaboration among multiple institutes aiming to engage and advance the public interest in solar eclipses and the science of the Sun-Earth connection. [ABSTRACT FROM AUTHOR]

We take stock of recent observations that identify the episodic plasma heating and injection of Alfvénic energy at the base of fast solar wind (in coronal holes). The plasma heating is associated with the occurrence of chromospheric spicules that leave the lower solar atmosphere at speeds of order 100 km/s, the hotter coronal counterpart of the spicule emits radiation characteristic of root heating that rapidly reaches temperatures of the order of 1 MK. Furthermore, the same spicules and their coronal counterparts (“Propagating Coronal Disturbances”; PCD) exhibit large amplitude, high speed, Alfvénic (transverse) motion of sufficient energy content to accelerate the material to high speeds. We propose that these (disjointed) heating and accelerating components form a one-two punch to supply, and then accelerate, the fast solar wind. We consider some compositional constraints on this concept, extend the premise to the slow solar wind, and identify future avenues of exploration. [ABSTRACT FROM AUTHOR]

large 2-campus Medical Center in Western New York, along with several other large area hospitals, planned for and simultaneously implemented successful 'Smoke-Free Campus' initiatives in November of 2006. This coordinated initiative required that each system plan accordingly for the development and implementation of policies, training of employees, clinicians, support staff and provision of tobacco treatment services (directly or via referral). In order to efficiently and competently inform each of these aspects of a system-wide initiative, accurate information was needed on the prevalence of tobacco use among employees, staff, faculty, and clinicians in each system. A multi-system surveillance initiative was implemented, using a brief survey for all employees of several of the partnering institutions. Summary data from the baseline measures are discussed. Also presented are Lessons Learned from the year-long planning and implementation phases, including details on topics categorized by the specific sub-committees that coordinated each area (e.g., Policy and Procedure, Communication, Faculty/Staff/Student Issues, Patient Issues (Inpatient and Outpatient), Tobacco Dependence Treatment and Provider/Staff Training). The effort was effective in instituting system-wide changes in all of the participating hospitals in the greater metropolitan area. A community-wide consortium convened each month for a year, and subcommittees within each hospital allowed planners to break up the initiative into manageable pieces. The extended timeline of 1 year was appropriate for overcoming fears, biases, and barriers which then enabled 'buy-in' and support from leadership as well as employees. [ABSTRACT FROM AUTHOR]

Energy is required to heat the outer solar atmosphere to millions of degrees (refs 1, 2) and to accelerate the solar wind to hundreds of kilometres per second (refs 2-6). Alfvén waves (travelling oscillations of ions and magnetic field) have been invoked as a possible mechanism to transport magneto-convective energy upwards along the Sun's magnetic field lines into the corona. Previous observations of Alfvénic waves in the corona revealed amplitudes far too small (0.5?km?s?1) to supply the energy flux (100-200?W?m?2) required to drive the fast solar wind or balance the radiative losses of the quiet corona. Here we report observations of the transition region (between the chromosphere and the corona) and of the corona that reveal how Alfvénic motions permeate the dynamic and finely structured outer solar atmosphere. The ubiquitous outward-propagating Alfvénic motions observed have amplitudes of the order of 20?km?s?1 and periods of the order of 100-500?s throughout the quiescent atmosphere (compatible with recent investigations), and are energetic enough to accelerate the fast solar wind and heat the quiet corona. [ABSTRACT FROM AUTHOR]

Modern dancers suffer a high rate of musculoskeletal injuries. Preventing injury prolongs dance careers and eases financial burden on both individual dancers and dance companies alike. A medical student partnered with Garth Fagan Dance to develop a curriculum to teach principles of injury prevention specific to preprofessional and professional modern dancers. Quantitative assessments showed a significant increase in participant injury prevention knowledge after completion of the course ( P < 0.0001). Participants' concern that injury may end their careers showed no significant change after the course ( P = 0.35). Injury prevention and dance-related injuries were reported the most often as useful topics while weight management was reported the least often as a useful topic. Qualitative evaluations showed that participants' found a course on injury prevention valuable and desired a course of longer duration that includes a greater number of topics. These findings show that modern dancers perceive an educational course on injury prevention as valuable and retain information presented in the course in the short-term. Further study is warranted to assess changes in injury rates after the course and to continue to improve curriculum content and implementation. [ABSTRACT FROM AUTHOR]

We present the application of novel diagnostics to the spectroscopic observation of a Coronal Mass Ejection (CME) on disk by the Extreme Ultraviolet Imaging Spectrometer (EIS) on the Hinode spacecraft. We apply a recently developed line profile asymmetry analysis to the spectroscopic observation of NOAA AR 10930 on 14 – 15 December 2006 to three raster observations before and during the eruption of a 1000 km s−1 halo CME. We see the impact that the observer’s line-of-sight and magnetic field geometry have on the diagnostics used. Further, and more importantly, we identify the on-disk signature of a high-speed outflow behind the CME in the dimming region arising as a result of the eruption. Supported by recent coronal observations of the STEREO spacecraft, we speculate about the momentum flux resulting from this outflow as a secondary momentum source to the CME. The results presented highlight the importance of spectroscopic measurements in relation to CME kinematics, and the need for full-disk synoptic spectroscopic observations of the coronal and chromospheric plasmas to capture the signature of such explosive energy release as a way of providing better constraints of CME propagation times to L1, or any other point of interest in the heliosphere. [ABSTRACT FROM AUTHOR]

We consider the problem of automatically (and robustly) isolating and extracting information about waves and oscillations observed in EUV image sequences of the solar corona with a view to near real-time application to data from the Atmospheric Imaging Array (AIA) on the Solar Dynamics Observatory (SDO). We find that a simple coherence/travel-time based approach detects and provides a wealth of information on transverse and longitudinal wave phenomena in the test sequences provided by the Transition Region and Coronal Explorer (TRACE). The results of the search are pruned (based on diagnostic errors) to minimize false-detections such that the remainder provides robust measurements of waves in the solar corona, with the calculated propagation speed allowing automated distinction between various wave modes. In this paper we discuss the technique, present results on the TRACE test sequences, and describe how our method can be used to automatically process the enormous flow of data (≈1 Tb day−1) that will be provided by SDO/AIA. [ABSTRACT FROM AUTHOR]

Background: Tobacco dependence counseling is recommended to be included as core curriculum for US medical students. To date, there has been little information on students' self-reported skills and practice opportunities to provide 5A's (Ask, Advise, Assess, Assist, and Arrange) counseling for tobacco cessation.Methods: We conducted anonymous surveys of second year and fourth year students at multiple US medical schools between February 2004 and March 2005 (overall response rate 70%). We report on the tobacco control practices of the 860 second year and 827 fourth year students completing the survey.Measurements and Main Results: Fourth year students reported multiple opportunities to learn tobacco counseling in case-based discussions, simulated patient encounters, and clinical skills courses. They reported more instruction in family medicine (79%) and Internal Medicine (70%) than Pediatrics (54%), Obstetrics/Gynecology (41%), and Surgery clerkships (16%). Compared with asking patients about smoking, advising smokers to quit, and assessing patient willingness to quit, fourth year students were less likely to have multiple practice opportunities to assist the patient with a quit plan and arrange follow-up contact. More than half of second year students reported multiple opportunities for asking patients about smoking but far fewer opportunities for practicing the other 4 As.Conclusions: By the beginning of their fourth year, most students in this group of medical schools reported multiple opportunities for training and practicing basic 5A counseling, although clear deficits for assisting patients with a quit plan and arranging follow-up care exist. Addressing these deficits and integrating tobacco teaching through tailored specific instruction across all clerkships, particularly in Surgery, Pediatrics, and Obstetrics/Gynecology is a challenge for medical school education. [ABSTRACT FROM AUTHOR]

Background: Online learning can be an excellent method for presenting clinical skills to address health behaviors.Methods: Medical students pilot tested a skills-building course consisting of an online component and a practical application.Results: A total of 38 students were registered, 25 (66%) completed the online component, and 22 (58%) completed both course components. Students reported they were adequately trained to administer the brief 5A intervention to patients who smoke and they intended to deliver the intervention routinely.Conclusions: Online skills-building courses can have a positive effect on students' knowledge and skills and can be used across health behaviors promote healthy lifestyles. [ABSTRACT FROM AUTHOR]

We discuss early results derived from an algorithm that automates the detection, cataloging, and analysis of extreme-ultraviolet (EUV) “bright points” (BP) from 9 years of data acquired by the Extreme-ultraviolet Imaging Telescope (EIT) on the Solar and Heliospheric Observatory (SOHO). The algorithm relies upon the computation of a map of “intensity significance”; this then contains the location of the EUV BPs. By mapping the location of BPs in each image and linking them through long sequences of EIT images we can describe the temporal and spatial variations of the 1.3× 108 EUV BPs observed by SOHO to date. We suggest that there is a considerable amount of physical information about the solar coronal plasma that can be readily gleamed from the BP detection database. In this paper we discuss only a small portion of the possible correlations, but we point to the possibility of BP lifetime distributions that are well described by modified power-laws; the components of which vary with the different temperature filters and with time over the present solar cycle. [ABSTRACT FROM AUTHOR]

Background. Training medical students in tobacco prevention and treatment skills is critical if we are to have competent physicians prepared to address the grave levels of morbidity and mortality associated with tobacco use. Tobacco Prevention and Cessation Education at US Medical Schools (PACE), a National Cancer Institute funded project, was launched to assess and improve curriculum content and teaching at 12 US medical schools. Methods. The 2003 survey was completed by faculty and administrators. The survey was divided into four main sections: tobacco content and skills, curricular evaluation, faculty perceptions of barriers and promoters, and educational vision. Results. Thirty-six percent of all medical school courses had some tobacco-related content. Five schools provided a total of between 4 and 8 hours of teaching, 5 schools provided 10-13 hours, and 2 schools provided 17 and 18 hours of teaching. Of the12 schools, 8 had fewer hours devoted to tobacco teaching in the clerkships than during the 1st-year courses. Only 2 schools noted any tobacco content for Obstetrics/Gynecology clerkships, and only 4 schools provided teaching in the pediatric setting (range 5-201 minutes). Conclusion. In comparison to earlier studies, it appears that more tobacco content is now integrated into medical school courses. More improvement is necessary, however, particularly in tobacco use prevention. Institutions need to examine the role of faculty in prioritizing tobacco information and promoting a culture that builds competency in tobacco control and treatment. [ABSTRACT FROM AUTHOR]

This paper is a pedagogical introduction to avalanche models of solar flares, including a comprehensive review of recent modeling efforts and directions. This class of flare model is built on a recent paradigm in statistical physics, known as self-organized criticality. The basic idea is that flares are the result of an ‘avalanche’ of small-scale magnetic reconnection events cascading through a highly stressed coronal magnetic structure, driven to a critical state by random photospheric motions of its magnetic footpoints. Such models thus provide a natural and convenient computational framework to examine Parker's hypothesis of coronal heating by nanoflares. [ABSTRACT FROM AUTHOR]

We focus on the deceptively simple question: how can we use the emitted photons to extract meaningful information on the transition region and corona? Using examples, we conclude that the only safe way to proceed is through forward models. In this way, inherent non-uniqueness is handled by adding information through explicit physical assumptions and restrictions made in the modeling procedure. The alternative, `inverse' approaches, including (as a restricted subset) many standard '`spectral diagnostic techniques', rely on more subjective choices that have, as yet, no clear theoretical support. Emphasis is on the solar transition region, but necessarily discussing the corona, and with implications for more general problems concerning the use of photons to diagnose plasma conditions. [ABSTRACT FROM AUTHOR]

The effects of non-uniform plasma target ionisation on the spectrum of thick-target HXR bremsstrahlung from a non-thermal electron beam are analysed. In particular the effect of the target ionisation structure on beam collisional energy losses, and hence on inversion of an observed photon spectrum to yield the electron injection spectrum, is considered and results compared with those obtained under the usual assumption of a fully ionised target. The problem is formulated and solved in principle for a general target ionisation structure, then discussed in detail for the case of a step function distribution of ionisation with column depth as an approximation to the sharp coronal–chromospheric step structure in solar flare plasmas. It is found that such ionisation structure has very dramatic effects on derivation of the thick-target electron injection spectrum F0(E0) as compared with the result F*0( E0) obtained under the usual assumption of a fully ionised target: (a) Inferred F*0 contain more electrons than F0 and in some cases include electrons at energies where none are actually present. Although the total (energy-integrated) beam fluxes in the two cases do not differ by a factor of more than Aee/AeH, the spectral shapes can differ greatly over finite energy intervals resulting in the danger of misleading results for total fluxes obtained by extrapolation. (b) The unconstrained mathematical solution for F0 for any photon spectrum is never unique, while that for F*0 is unique. When the physical constraint F0 ≥ 0 is added, for some photon spectra solutions for F0 may not exist or may not be unique. (This is not an effect of noise but of real analytic ambiguity.) (c) For data corresponding to F*0 with a low-energy cut-off, or a cut-off or rapid enough exponential decline at high energies, a unique solution F0 does exist and we obtain a recursive summation for its evaluation. Consequently, in future work on the inversion of HXR bremsstrahlung spectra it will be vital for algorithms to include the effects of target ionisation if spurious results on thick-target electron spectra are not to be inferred. Finally it is pointed out that the depth of the transition zone, and its evaporative evolution during flares may be derivable from its effect on the HXR spectrum. [ABSTRACT FROM AUTHOR]

We observe the abrupt end of solar-activity cycles at the Sun's Equator by combining almost 140 years of observations from ground and space. These "terminator" events appear to be very closely related to the onset of magnetic activity belonging to the next solar cycle at mid-latitudes and the polar-reversal process at high latitudes. Using multi-scale tracers of solar activity we examine the timing of these events in relation to the excitation of new activity and find that the time taken for the solar plasma to communicate this transition is of the order of one solar rotation – but it could be shorter. Utilizing uniquely comprehensive solar observations from the Solar Terrestrial Relations Observatory (STEREO) and Solar Dynamics Observatory (SDO) we see that this transitional event is strongly longitudinal in nature. Combined, these characteristics suggest that information is communicated through the solar interior rapidly. A range of possibilities exist to explain such behavior: for example gravity waves on the solar tachocline, or that the magnetic fields present in the Sun's convection zone could be very large, with a poloidal field strengths reaching 50 kG – considerably larger than conventional explorations of solar and stellar dynamos estimate. Regardless of the mechanism responsible, the rapid timescales demonstrated by the Sun's global magnetic-field reconfiguration present strong constraints on first-principles numerical simulations of the solar interior and, by extension, other stars. [ABSTRACT FROM AUTHOR]

When will a new cycle's sunspots appear? We demonstrate a novel physical mechanism, namely, that a "solar tsunami" occurring in the Sun's interior shear-fluid layer can trigger new cycle's magnetic flux emergence at high latitudes, a few weeks after the cessation of old cycle's flux emergence near the equator. This tsunami is excited at the equator when magnetic dams, created by the oppositely-directed old cycle's toroidal field in North and South hemispheres, break due to mutual annihilation of toroidal flux there. The fluid supported by these dams rushes to the equator; the surplus of fluid cannot be contained there, so it reflects back towards high latitudes, causing a tsunami. This tsunami propagates poleward at a speed of ~300 m/s until it encounters the new cycle's spot-producing toroidal fields in mid-latitudes, where it perturbs the fields, triggering their surface-eruption in the form of new cycle spots. A new sunspot cycle is preceded for several years by other forms of high-latitude magnetic activity, such as coronal bright points and ephemeral regions, until the tsunami causes the birth of new cycle's spots. The next tsunami is due by 2020, portending the start of intense 'space weather' that can adversely impact the Earth. [ABSTRACT FROM AUTHOR]

A correction to the article "Injury Prevention for Modern Dancers: A Pilot Study of an Educational Intervention" that was published in the March 13, 2010 issue is presented.