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A fundamental property of coronal mass ejections (CMEs) is their radial expansion, which determines the increase in the CME radial size and the decrease in the CME magnetic field strength as the CME propagates. CME radial expansion can be investigated either by using remote observations or by in situ measurements based on multiple spacecraft in radial conjunction. However, there have been only few case studies combining both remote and in situ observations. It is therefore unknown if the radial expansion in the corona estimated remotely is consistent with that estimated locally in the heliosphere. To address this question, we first select 22 CME events between the years 2010 and 2013, which were well observed by coronagraphs and by two or three spacecraft in radial conjunction. We use the graduated cylindrical shell model to estimate the radial size, radial expansion speed, and a measure of the dimensionless expansion parameter of CMEs in the corona. The same parameters and two additional measures of the radial-size increase and magnetic-field-strength decrease with heliocentric distance of CMEs based on in situ measurements are also calculated. For most of the events, the CME radial size estimated by remote observations is inconsistent with the in situ estimates. We further statistically analyze the correlations of these expansion parameters estimated using remote and in situ observations, and discuss the potential reasons for the inconsistencies and their implications for the CME space weather forecasting. [ABSTRACT FROM AUTHOR]

Objective: The present study aims to investigate the effectiveness, recurrence, and adverse reaction rates of isotope phosphorus‐32 dressings combined with diprospan and mucopolysaccharide polysulphate cream in the treatment of keloids. Methods: A total of 80 patients with keloids admitted to the Dermatology Clinic of the Fourth Affiliated Hospital of Harbin Medical University between June 2019 and June 2021 were included in the present study and randomly divided into three groups: Control Group 1 (n = 27), Control Group 2 (n = 25), and the treatment group (n = 28). Patients in Control Group 1 were treated with diprospan combined with mucopolysaccharide polysulphate cream, patients in Control Group 2 were treated with an isotopic phosphorus‐32 dressing combined with mucopolysaccharide polysulphate cream, and patients in the treatment group were treated with an isotopic phosphorus‐32 dressing combined with diprospan and mucopolysaccharide polysulphate cream. The effectiveness, recurrence, and adverse reaction rates were observed in all three groups. Results: The treatment group had the most significant decrease in the itching scores. The respective effectiveness, recurrence, and adverse reaction rates were 81.4%, 43.6%, and 74.1% in Control Group 1; 56%, 38.7%, and 64% in Control Group 2; and 96.7%, 11.2%, and 41% in the treatment group. The differences were statistically significant (p < 0.05). Conclusion: An isotope phosphorus‐32 dressing combined with diprospan and mucopolysaccharide polysulphate cream keloid treatment delivers a fast onset, good effectiveness, and low recurrence and adverse effect rates. [ABSTRACT FROM AUTHOR]

The important role played by magnetic reconnection in the early acceleration of coronal mass ejections (CMEs) has been widely discussed. However, as CMEs may have expansion speeds comparable to their propagation speeds in the corona, it is not clear whether and how reconnection contributes to the true acceleration and expansion separately. To address this question, we analyze the dynamics of a moderately fast CME on 2013 February 27, associated with a continuous acceleration of its front into the high corona, even though its speed had reached ∼700 km sâˆ'1, which is faster than the solar wind. The apparent acceleration of the CME is found to be due to its expansion in the radial direction. The true acceleration of the CME, i.e., the acceleration of its center, is then estimated by taking into account the expected deceleration caused by the drag force of the solar wind acting on a fast CME. It is found that the true acceleration and the radial expansion have similar magnitudes. We find that magnetic reconnection occurs after the eruption of the CME and continues during its propagation in the high corona, which contributes to its dynamic evolution. Comparison between the apparent acceleration related to the expansion and the true acceleration that compensates the drag shows that, for this case, magnetic reconnection contributes almost equally to the expansion and to the acceleration of the CME. The consequences of these measurements for the evolution of CMEs as they transit from the corona to the heliosphere are discussed. [ABSTRACT FROM AUTHOR]

Suprathermal ions in the corona are thought to serve as seed particles for large gradual solar energetic particle (SEP) events associated with fast and wide coronal mass ejections (CMEs). A better understanding of the role of suprathermal particles as seed populations for SEP events can be made by using observations close to the Sun. We study a series of SEP events observed by the Integrated Science Investigation of the Sun (IS⊙IS) suite on board the Parker Solar Probe (PSP) from 2020 May 27 to June 2, during which PSP was at heliocentric distances between ∼0.4 and ∼0.2 au. These events were also observed by the Ahead Solar TErrestrial RElations Observatory (STEREO-A) near 1 au, but the particle intensity magnitude was much lower than that at PSP. We find that the SEPs should have spread in space as their source regions were distant from the nominal magnetic footpoints of both spacecraft and the parent CMEs were slow and narrow. We study the decay phase of the SEP events in the ∼1â€"2 MeV proton energy range at PSP and STEREO-A, and discuss their properties in terms of both continuous injections by successive solar eruptions and the distances where the measurements were made. This study indicates that seed particles can be continuously generated by eruptions associated with slow and narrow CMEs, spread over a large part of the inner heliosphere, and remain there for tens of hours, even if minimal particle intensity enhancements were measured near 1 au. [ABSTRACT FROM AUTHOR]

The scenario of twin coronal mass ejections (CMEs), i.e., a fast and wide primary CME (priCME) preceded by preceding CMEs (preCMEs), has been found to be favorable to a more efficient particle acceleration in large solar energetic particle (SEP) events. Here we study 19 events during 2007â€"2014 associated with twin-CME eruptions but without large SEP observations at the L1 point. We combine remote-sensing and in situ observations from multiple spacecraft to investigate the role of magnetic connectivity in SEP detection and the CME information in three-dimensional (3D) space. We study one-on-one correlations of the priCME 3D speed, flare intensity, suprathermal backgrounds, and height of CMEâ€"CME interaction with the SEP intensity. Among these, the priCME speed is found to correlate with the SEP peak intensity at the highest level. We use the projection correlation method to analyze the correlations between combinations of these multiple independent factors and the SEP peak intensity. We find that the only combination of two or more parameters that has a higher correlation with the SEP peak intensity than the CME speed is the CME speed combined with the propagation direction. This further supports the dominant role of the priCME in controlling the SEP enhancements and emphasizes the consideration of the latitudinal effect. Overall, the magnetic connectivity in longitude as well as latitude and the relatively lower priCME speed may explain the existence of the twin-CME SEP-poor events. The role of the barrier effect of preCME(s) is discussed for an event on 2013 October 28. [ABSTRACT FROM AUTHOR]

Background: The survival time of patients with early pancreatic cancer (PC) is still disappointing, even after surgical resection. PC has an extremely poor prognosis. Herein, we aimed to investigate the survival effect of postoperative radiotherapy (PORT) on resected stage I to II PC. Material and methods: A large eligible sample of patients was identified from 2010 to 2015 from the Surveillance, Epidemiology, and End Results (SEER) registry. Survival analysis was conducted to evaluate the efficiency of PORT. Propensity score matching (PSM) analysis was used to reduce selection bias and to make the groups comparable. Results: A total of 3219 patients with resected stage I to II PC was included after rigid screening. The median overall survival (OS) was 26 months with PORT (n = 1055) versus 21 months with non-PORT (n = 2164) before matching (p<0.001). By multivariable analysis, PORT remained a favorable prognostic predictor for OS. In PSM analysis, receiving PORT was associated with improved OS (median, 26 months vs. 23 months; at 2 years, 51.7% vs. 46.7%; at 5 years, 23.3% vs. 17.4% (P = 0.006). After further meticulous exploration, only the stage IIB subgroup benefited from PORT (p<0.001). This result was due to the positive lymph node state (N+), whose mortality risk was cut by 23.4% (p<0.001) by PORT. Conclusion: Addition of PORT to the treatment of patients with resected stage I to II PC conveys a survival benefit, particularly among those with N-positive or stage IIB disease. [ABSTRACT FROM AUTHOR]

Gradual and large solar energetic particle (SEP) events (flux of ions with energy >10 MeV above 10 pfu) are primarily produced in shocks driven by fast and wide coronal mass ejections (CMEs). Past research, both in theory and statistics, has found that the situation where a fast primary CME (priCME) is preceded by previous CMEs (preCMEs) is favorable to a more efficient particle acceleration. However, the physical causes of this association is still a matter of debate, including the association of the acceleration and release of SEPs with the interaction of successive CMEs. Taking advantage of the twin Solar TErrestrial RElations Observatory spacecraft, we study 41 large SEP events in solar cycle 24 by multi-viewpoint observations. Although 21 events (∼51%) have a preCME identifiable in the Large Angle and Spectrometric Coronagraph, we determine that the priCMEs overlap the preCMEs in three dimension (3D) for only 11 events (∼27%). We further investigate the acceleration (using type II radio bursts) and release (using velocity dispersion analysis) of the particles for all potential instances of CME–CME interaction in 3D. We find that, for six of 11 events, the priCME is far away from catching up with the preCME when the particles are released. However, for the limited samples, the SEP peak intensity is significantly higher in the events in which the priCME is closest to impacting the preCME, indicating the potential for the increased seed population or more enhanced turbulence levels occurring closer to the preCME. [ABSTRACT FROM AUTHOR]

Comparisons were made among the evaluation models of fatigue crack growth in various codes, standards, and guidelines, to illustrate the significance of transition point in accuracy. A new bilinear model was established with transition point and fatigue threshold fully considered, and was found more accurate than existing codes and standards for evaluation of fatigue crack growth behavior in both Paris and near-threshold regimes. • Conservativeness in existing codes and standards for fatigue crack growth assessment was compared. • Transition point in fatigue crack growth was found significant in assessment accuracy. • A new bilinear model for fatigue crack growth evaluation was developed. [ABSTRACT FROM AUTHOR]

• m -ln C relationship was correlated well with transition behavior of FCG curve. • A master curve for transition behavior of FCG curve was found. • Crack closure was considered for transition point modeling for the first time. • A new model for transition point prediction was established. The transition behavior of fatigue crack growth was investigated using data from a CrNiMoV steel welded joint. The m -ln C was linearly correlated under a given stress ratio in both Paris and near-threshold regimes, where the coordinate of transition point was found as slope and intercept of m -ln C relationship. All m -ln C curves tended to pass through one fixed point, (m 0 , lnC 0), and a master curve for transition point was determined. A new model for transition point prediction was established which had significance in accurate fatigue life assessment on the basis of the bilinear approach. [ABSTRACT FROM AUTHOR]

• Ultrapure green emissions of glass-stabilized CsPb(Br/I) 3 PeQDs are fabricated. • Quantum yields of CsPb(Br/I) 3 @glass composites are highly dependent on halogen content. • The emissive profiles and FWHMs can be well modified by varying Br-to-I ratio in glass. • The issues of instability, adverse anion-exchange and phase separation of colloidal PeQDs can be solved by glass protection. • Prototypical white LEDs are constructed and applied in backlit display, covering up 92% color gamut of Rec. 2020 standard. CsPbX 3 (X = Cl, Br, I) perovskite quantum dots (PeQDs) have potential application in backlit display. However, they generally suffer from instability and shortage of ultrapure tunable green emissions owing to halogen phase separation. This work reports the realization of elaborately tunable green emissions in glass-protected CsPb(Br/I) 3 PeQDs, which show the advantage of superior long-term stability and enable them to find promising application in ultra-high definition televisions. CsPbX 3 @glass composites are fabricated by a facile in-situ glass crystallization strategy and their emissions within the spectral range of 506–532 nm along with narrow full width at half maximum (FWHM) of ~21 nm can be well modified by simply varying Br-to-I ratio in precursor glass. Benefited from the protection of tight glass network, CsPbX 3 @glass retains 90% luminescence after immersing in water for one month, shows no any loss of luminescence after irradiation by 450 nm LED light and prevents anion-exchange and phase separation completely. As a proof-of-concept experiment, CsPbX 3 @glass-based on-chip white LED devices are constructed and applied in backlit display, covering up 123% and 92% color gamut of NTSC and Rec. 2020 standards in the CIE 1931 color space, respectively. [ABSTRACT FROM AUTHOR]

On 28 October 2021, solar eruptions caused intense and long‐lasting solar energetic particle (SEP) flux enhancements observed by spacecraft located over a wide longitudinal range in the heliosphere. SEPs arriving at Earth caused the 73rd ground level enhancement (GLE) event recorded by ground‐based neutron monitors. In particular, this is also the first GLE event seen on the surface of three planetary bodies, Earth, Moon, and Mars, by particle and radiation detectors as shown in this study. We derive the event‐integrated proton spectrum from measurements by near‐Earth spacecraft and predict the lunar and martian surface radiation levels using particle transport models. Event doses at the lunar and martian surfaces of previous GLE events are also modeled and compared with the current event. This statistical and comparative study advances our understanding of potential radiation risks induced by extreme SEP events for future human explorations of the Moon and Mars. Plain Language Summary: Human beings are considering going back to the Moon and eventually to Mars within the next decades. However, we are still facing one major hurdle "space radiation" which is a significant and unavoidable risk for crews' health, especially for long‐term stays at future lunar or martian stations. In particular, sporadic solar energetic particles (SEPs) generated via extreme solar eruptions may enhance the lunar or martian surface radiation levels to potentially hazardous values. Recent lunar and martian surface and orbital radiation detectors have advanced our understanding of the radiation environment of both planetary bodies. On 28 October 2021 a SEP event occurred and had energies high enough to trigger ground‐level‐enhancement (GLE) events on the surface of Earth, the Moon, and Mars. Combining both measurements and modeling approaches, we study this first GLE event seen on three planetary surfaces and demonstrate its potential SEP radiation risk to humans on the Moon and Mars together with the results of previous GLE events. Key Points: This is the first ground level enhancement event simultaneously measured on Earth, Moon, and MarsWe analyze the radiation measurements at 3 locations and compare with our model predictions based on detected solar energetic particle (SEP) fluxWe show that extreme SEP events can induce much higher (∼100 times) radiation doses on the Moon than on Mars [ABSTRACT FROM AUTHOR]

The radial expansion of coronal mass ejections (CMEs) is known to occur from remote observations, from the variation of their properties with radial distance, and from local in situ plasma measurements showing a decreasing speed profile throughout the magnetic ejecta (ME). However, little is known on how local measurements compare to global measurements of expansion. Here, we present results from the analysis of 42 CMEs measured in the inner heliosphere by two spacecraft in radial conjunction. The magnetic-field decrease with distance provides a measure of their global expansion. Near 1 au, the decrease in their bulk speed provides a measure of their local expansion. We find that these two measures have little relation with each other. We also investigate the relation between characteristics of CME expansion and CME properties. We find that the expansion depends on the initial magnetic-field strength inside the ME, but not significantly on the magnetic field inside the ME measured near 1 au. This is indirect evidence that CME expansion in the innermost heliosphere is driven by the high magnetic pressure inside the ME, while by the time the MEs reach 1 au, they are expanding due to the decrease in the solar-wind dynamic pressure with distance. We also determine the evolution of the ME tangential and normal magnetic-field components with distance, revealing significant deviations as compared to the expectations from force-free field configurations as well as some evidence that the front half of MEs expand at a faster rate than the back half. [ABSTRACT FROM AUTHOR]

Abstract: Rare earth (RE)—3d transition metal (TM) films were codeposited in low temperature urea–acetamide–NaBr–KBr–RECl3–TMCl2 baths by potentiostatic electrolysis. Cyclic voltammetry is used to investigate the electrochemical behavior of RE(III) and TM(II) in baths on a Pt electrode. The reduction of TM(II) is an irreversible process. RE(III) cannot be reduced alone, but it can be inductively codeposited with TM(II). Some kinetic parameters are measured, e.g., the transfer coefficient α and the diffusion coefficient D 0 for TM(II). It is reasonably suggested that the RE-induced codeposition ability and efficiency is dominated by the electronegativity difference between RE and TM atoms. Moreover, it is found that the surface morphologies, the magnetic anisotropy and preferring orientation of the as-deposited RE–TM films depend strongly on the composition and potential. At last, it is observed that, there exists a clear anisotropy with easy magnetization along the plane of the RE–TM films. The magnetic anisotropy in amorphous RE–TM films should be due to the competing contributions from several factors, such as spin–orbit coupling, stress, etc. [Copyright &y& Elsevier]