Publisher’s Note: Probing the Scale Invariance of the Inflationary Power Spectrum in Expanding Quasi-Two-Dimensional Dipolar Condensates [Phys. Rev. Lett. <b>118</b> , 130404 (2017)]

Ch&auml,, Seok-Yeong,Fischer, Uwe R. American Physical Society 2017 Physical Review Letters Vol.118 No.17

MEASUREMENTS OF THE CORONAL ACCELERATION REGION OF A SOLAR FLARE

Krucker, S&auml,m,Hudson, H. S.,Glesener, L.,White, S. M.,Masuda, S.,Wuelser, J.-P.,Lin, R. P. IOP Publishing 2010 The Astrophysical journal Vol.714 No.2

<P>The Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) and the Nobeyama Radioheliograph (NoRH) are used to investigate coronal hard X-ray and microwave emissions in the partially disk-occulted solar flare of 2007 December 31. The STEREO mission provides EUV images of the flare site at different viewing angles, establishing a two-ribbon flare geometry and occultation heights of the RHESSI and NoRH observations of similar to 16 Mm and similar to 25 Mm, respectively. Despite the occultation, intense hard X-ray emission up to similar to 80 keV occurs during the impulsive phase from a coronal source that is also seen in microwaves. The hard X-ray and microwave source during the impulsive phase is located similar to 6 Mm above thermal flare loops seen later at the soft X-ray peak time, similar in location to the above-the-loop-top source in the Masuda flare. A single non-thermal electron population with a power-law distribution (with spectral index of similar to 3.7 from similar to 16 keV up to the MeV range) radiating in both bremsstrahlung and gyrosynchrotron emission can explain the observed hard X-ray and microwave spectrum, respectively. This clearly establishes the non-thermal nature of the above-the-loop-top source. The large hard X-ray intensity requires a very large number (>5 x 10(35) above 16 keV for the derived upper limit of the ambient density of similar to 8 x 10(9) cm(-3)) of suprathermal electrons to be present in this above-the-loop-top source. This is of the same order of magnitude as the number of ambient thermal electrons. We show that collisional losses of these accelerated electrons would heat all ambient electrons to superhot temperatures (tens of keV) within seconds. Hence, the standard scenario, with hard X-rays produced by a beam comprising the tail of a dominant thermal core plasma, does not work. Instead, all electrons in the above-the-loop-top source seem to be accelerated, suggesting that the above-the-loop-top source is itself the electron acceleration region.</P>

ESTIMATES OF DENSITIES AND FILLING FACTORS FROM A COOLING TIME ANALYSIS OF SOLAR MICROFLARES OBSERVED WITH<i>RHESSI</i>

Baylor, R. N.,Cassak, P. A.,Christe, S.,Hannah, I. G.,Krucker, S&auml,m,Mullan, D. J.,Shay, M. A.,Hudson, H. S.,Lin, R. P. IOP Publishing 2011 The Astrophysical journal Vol.736 No.1

<P>We usemore than 4500 microflares from the RHESSI microflare data set to estimate electron densities and volumetric filling factors of microflare loops using a cooling time analysis. We show that if the filling factor is assumed to be unity, the calculated conductive cooling times are much shorter than the observed flare decay times, which in turn are much shorter than the calculated radiative cooling times. This is likely unphysical, but the contradiction can be resolved by assuming that the radiative and conductive cooling times are comparable, which is valid when the flare loop temperature is a maximum and when external heating can be ignored. We find that resultant radiative and conductive cooling times are comparable to observed decay times, which has been used as an assumption in some previous studies. The inferred electron densities have a mean value of 10(11.6) cm(-3) and filling factors have a mean of 10(-3.7). The filling factors are lower and densities are higher than previous estimates for large flares, but are similar to those found for two microflares by Moore et al.</P>

MST1-dependent vesicle trafficking regulates neutrophil transmigration through the vascular basement membrane

Kurz, Angela R. M.,Pruenster, Monika,Rohwedder, Ina,Ramadass, Mahalakshmi,Sch&auml,fer, Kerstin,Harrison, Ute,Gouveia, Gabriel,Nussbaum, Claudia,Immler, Roland,Wiessner, Johannes R. American Society for Clinical Investigation 2016 The Journal of clinical investigation Vol.126 No.11

<P>Neutrophils need to penetrate the perivascular basement membrane for successful extravasation into inflamed tissue, but this process is incompletely understood. Recent findings have associated mammalian sterile 20-like Kinase 1 (MST1) loss of function with a human primary immunodeficiency disorder, suggesting that MST1 may be involved in immune cell migration. Here, we have shown that MST1 is a critical regulator of neutrophil extravasation during inflammation. Mst1-deficient (Mst1(-/-)) neutrophils were unable to migrate into inflamed murine cremaster muscle venules, instead persisting between the endothelium and the basement membrane. Mst1(-/-) neutrophils also failed to extravasate from gastric submucosal vessels in a murine model of Helicobacter pylori infection. Mechanistically, we observed defective translocation of VLA-3, VLA-6, and neutrophil elastase from intracellular vesicles to the surface of Mst1(-/-) neutrophils, indicating that MST1 is required for this crucial step in neutrophil transmigration. Furthermore, we found that MST1 associates with the Rab27 effector protein synaptotagmin-like protein 1 (JFC1, encoded by Sytl1 in mice), but not Munc13-4, thereby regulating the trafficking of Rab27-positive vesicles to the cellular membrane. Together, these findings highlight a role for MST1 in vesicle trafficking and extravasation in neutrophils, providing an additional mechanistic explanation for the severe immune defect observed in patients with MST1 deficiency.</P>

Optical vortex arrays from smectic liquid crystals

Son, Baeksik,Kim, Sejeong,Kim, Yun Ho,K&auml,l&auml,nt&auml,r, K.,Kim, Hwi-Min,Jeong, Hyeon-Su,Choi, Siyoung Q.,Shin, Jonghwa,Jung, Hee-Tae,Lee, Yong-Hee The Optical Society 2014 Optics express Vol.22 No.4

Farm Work–Related Injuries and Risk Factors in South Korean Agriculture

Kim, Hyocher,Rä,s&auml,nen, Kimmo,Chae, Hyeseon,Kim, Kyungsu,Kim, Kyungran,Lee, Kyungsuk Taylor Francis 2016 Journal of agromedicine Vol.21 No.4

<P>Agriculture is known to be a risk-filled industry in South Korea, as it is worldwide. The aims of this study were to identify the magnitude of farm work-related injuries and evaluate the association between injury and possible risk factors. Farmers, including farm members (N = 16,160), were surveyed. After excluding 7 subjects with missing data in questions about injury, 16,153 farmer responses were used for the analysis. Of the 16,153 farmers, 3.6% answered having at least one farm work-related injury requiring outpatient treatment or hospitalization during 2012. The proportion of injured men (4.3%) was 1.5 times higher than women (2.9%). From an age perspective, the proportion was 1.3% of those aged 49 or below, 2.7% of those aged 50-59, 4.2% of those aged 60-69, 4.2% of those aged 70-79, and 3.1% of those aged 80 or above. We used a multivariate logistic regression analysis with a stepwise model (forward) for risk factors (gender, age, farm ownership, farm type, work years in agriculture, work months during 2012, night work experience, and work experience under the influence of alcohol). The increased risk of farm work-related injuries significantly remained associated with age, farm ownership, and experience of night work. Further studies should be conducted to consistently identify injury characteristics, especially for old farmers, considering the crop cultivation in Asian countries.</P>

HARD X-RAY OBSERVATIONS OF A JET AND ACCELERATED ELECTRONS IN THE CORONA

Glesener, Lindsay,Krucker, S&auml,m,Lin, R. P. IOP Publishing 2012 The Astrophysical journal Vol.754 No.1

<P>We report the first hard X-ray observation of a solar jet on the limb with flare footpoints occulted, so that faint emission from accelerated electrons in the corona can be studied in detail. In this event on 2003 August 21, RHESSI observed a double coronal hard X-ray source in the pre-impulsive phase at both thermal and nonthermal energies. In the impulsive phase, the first of two hard X-ray bursts consists of a single thermal/nonthermal source coinciding with the lower of the two earlier sources, and the second burst shows an additional nonthermal, elongated source, spatially and temporally coincident with the coronal jet. Analysis of the jet hard X-ray source shows that collisional losses by accelerated electrons can deposit enough energy to generate the jet. The hard X-ray time profile above 20 keV matches that of the accompanying Type III and broadband gyrosynchrotron radio emission, indicating both accelerated electrons escaping outward along the jet path and electrons trapped in the flare loop. The double coronal hard X-ray source, the open field lines indicated by Type III bursts, and the presence of a small post-flare loop are consistent with significant electron acceleration in an interchange reconnection geometry.</P>

A STATISTICAL STUDY OF SOLAR ELECTRON EVENTS OVER ONE SOLAR CYCLE

Wang, Linghua,Lin, R. P.,Krucker, S&auml,m,Mason, Glenn M. IOP Publishing 2012 The Astrophysical journal Vol.759 No.1

<P>We survey the statistical properties of 1191 solar electron events observed by the WIND 3DP instrument from <1 keV to greater than or similar to 300 keVfor a solar cycle (1995 through 2005). After taking into account times of high background, the corrected occurrence frequency of solar electron events versus peak flux exhibits a power-law distribution over three orders of magnitude with exponents between -1.0 and -1.6 for different years, comparable to the frequency distribution of solar proton events, microflares, and coronal mass ejections (CMEs), but significantly flatter than that of soft X-ray (SXR) flares. At 40 keV (2.8 keV), the integrated occurrence rate above similar to 0.29 (similar to 330) cm(-2) s(-1) sr(-1) keV(-1) near 1 AU is similar to 1000 year(-1) (similar to 600 year(-1)) at solar maximum and similar to 35 year(-1) (similar to 25 year(-1)) at solar minimum, about an order of magnitude larger than the observed occurrence rate. We find these events typically extend over similar to 45 degrees in longitude, implying the occurrence rate over the whole Sun is similar to 10(4) year(-1) near solar maximum. The observed solar electron events have a 98.75% association with type III radio bursts, suggesting all type III bursts may be associated with a solar electron event. They have a close (similar to 76%) association with the presence of low-energy (similar to 0.02-2 MeV nucleon(-1)), He-3-rich (He-3/He-4 >= 0.01) ion emissions measured by the ACE ULEIS instrument. For these electron events, only similar to 35% are associated with a reported GOES SXR flare, but similar to 60% appear to be associated with a CME, with similar to 50% of these CMEs being narrow. These electrons are often detected down to below 1 keV, indicating a source high in the corona.</P>

Agricultural injuries in Korea and errors in systems of safety

Kim, Hyocher,Lee, Kyungsuk,Rä,s&auml,nen, Kimmo Institute of Rural Health 2016 Annals of agricultural and environmental medicine Vol.23 No.3

ON THE RELATION OF ABOVE-THE-LOOP AND FOOTPOINT HARD X-RAY SOURCES IN SOLAR FLARES

Ishikawa, S.,Krucker, S&auml,m,Takahashi, T.,Lin, R. P. IOP Publishing 2011 The Astrophysical journal Vol.737 No.2

<P>We report on the most prominent example of an above-the-loop hard X-ray source in the extensive solar flare database of RHESSI. The limb flare of 2003 October 22 around 20 UT resembles the famous Masuda flare, except that only one of the footpoint sources is visible with the other one occulted. However, even for this very prominent event, the above-the-loop source is only visible during one of the four hard X-ray peaks, highlighting the rare occurrence of above-the-loop sources that are equally bright as footpoint sources. The relative timing between the above-the-loop and footpoint sources shows that the coronal source peaks about 10 s before the footpoint source and decays during the time the footpoint source is most prominent. Furthermore, the derived number of non-thermal electrons within the above-the-loop source is large enough to provide the needed number of precipitating electrons to account for the footpoint emission over the duration of the hard X-ray peak. Hence, these observations support the simple scenario where bulk energization is accelerating all electrons within the above-the-loop source and precipitating electrons are emptying out of the above-the-loop source to produce the footpoint emissions.</P>