المؤلفون: Qu, Huanhuan, Zhang, Rongli, Xin, Wuyan, Jing, Huan, Wang, Gang, Gao, Lin

المصدر: Journal of Cosmetic Dermatology; May2024, Vol. 23 Issue 5, p1638-1644, 7p

مصطلحات موضوعية: MINOXIDIL, HAIR transplantation, HAIR removal, HAIR growth, BALDNESS, HAIR follicles, LASERS

مستخلص: Background: Characterized by progressive hair loss due to an excessive response to androgens, androgenetic alopecia (AGA) affects up to 50% of males and females. Minoxidil is one of approved medications for AGA but inadequate responses occur in many patients. Aims: To determine whether 1565 nm non‐ablative fractional laser (NAFL) could yield better therapeutic benefits for patients with AGA as compared with 5% minoxidil. Methods: Thirty patients with AGA were enrolled; they were randomly assigned into the laser or minoxidil treatment groups. For the laser treatment group, patients were treated by 1565 nm NAFL at 10 mJ, 250 spots/cm2 with 2 weeks intervals for 4 sessions in total. For the minoxidil treatment group, 1‐milliliter of topical 5% minoxidil solution was applied to hair loss area twice a day. Results: The primary outcomes were the changes in numerous hair growth indexes at the Week 10 as compared with the baselines. Both 1565 nm NAFL and 5% minoxidil led to significantly greater hair densities and diameters in patients at the Week 10 than the baselines (p < 0.01). As compared with 5% minoxidil, 1565 nm NAFL showed significantly greater improvements in total hair number, total hair density (hair/cm2), terminal hair number, terminal hair density (hair/cm2), number of hair follicle units, and average hair number/number of hair follicle units. Conclusions: Our data demonstrate that 1565 nm NAFL exhibits superior clinical efficacy in some aspects of hair growth to the topical minoxidil. It is a safe and effective modality in treating AGA. [ABSTRACT FROM AUTHOR]

: Copyright of Journal of Cosmetic Dermatology is the property of Wiley-Blackwell and its content may not be copied or emailed to multiple sites or posted to a listserv without the copyright holder's express written permission. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)

المؤلفون: Liu, Lu, Zheng, Chen‐Xi, Zhao, Na, Zhu, Ting, Hu, Cheng‐Biao, Zhang, Nan, Chen, Ji, Zhang, Kai‐Chao, Zhang, Sha, Liu, Jie‐Xi, Zhang, Kai, Jing, Huan, Sui, Bing‐Dong, Jin, Yan, Jin, Fang

المصدر: Advanced Healthcare Materials; 8/8/2023, Vol. 12 Issue 20, p1-19, 19p

المؤلفون: Yan, Yun, Yue, Chao, Yin, Ze‐Fan, Zhou, Xu‐Zhi, Zong, Qiu‐Gang, Li, Jing‐Huan

المصدر: Journal of Geophysical Research. Space Physics; Jul2023, Vol. 128 Issue 7, p1-14, 14p

مصطلحات موضوعية: SOLAR wind, MAGNETOSPHERE, CYCLOTRON resonance, DYNAMIC pressure, WIND pressure, RADIATION belts

مستخلص: Large‐amplitude (Bw > 1 nT) electromagnetic ion cyclotron (EMIC) waves can cause the rapid loss of >1 MeV electrons, greatly impacting radiation belt dynamics. With long‐term Van Allen Probe B observations from 2013 to 2018, we conducted a statistical survey to reveal the amplitude‐dependent EMIC wave properties and excitation mechanisms in the Earth's inner magnetosphere. Statistical results show that large‐amplitude EMIC waves prefer to occur in the afternoon‐dusk sector in the northern hemisphere and tend to be more left‐hand polarized with smaller wave normal angles. In addition, the high proton beta parallel conditions also favor the generation of larger‐amplitude EMIC waves. From the variations of EMIC wave occurrence rate as a function of SuperMAG electrojet (SME) index and solar wind dynamic pressure, we find that the small‐amplitude EMIC waves are generally triggered by high solar wind dynamic pressure, while large‐amplitude EMIC wave generation is both affected by substorm activity and solar wind dynamic pressure. The normalized magnetic field perturbations during EMIC wave appearance, which enable us to distinguish the relative roles of magnetospheric compression and substorm injection in the excitation of different‐amplitude EMIC waves, provide further evidence that as wave amplitude increases, substorm injection plays a more important role in EMIC wave excitation, and magnetospheric compression is also an indispensable trigger. Plain Language Summary: Electromagnetic ion cyclotron (EMIC) waves, one of the most commonly observed electromagnetic waves in the Earth's inner magnetosphere, can scatter relativistic electrons through cyclotron resonance and cause their loss to the atmosphere, which greatly affects radiation belt dynamics. In recent years, large‐amplitude EMIC waves have attracted much attention due to their ability to cause the rapid loss of >1 MeV electrons. This study aims to reveal the amplitude‐dependent wave properties and excitation mechanisms of EMIC waves in the Earth's inner magnetosphere. It is shown that large‐amplitude EMIC waves are more likely to be left‐hand polarized with smaller wave normal angles under high proton beta parallel β∥,p, which is the ratio of parallel thermal pressure and magnetic pressure. Through analyzing EMIC wave occurrence rate as a function of SME index and solar wind dynamic pressure, together with the normalized magnetic field perturbations during EMIC wave appearance, which can be used to quantify the effects of magnetospheric compression and substorm injection on EMIC wave excitation, we conclude that substorm injection plays a more important role in large‐amplitude EMIC wave excitation, while magnetospheric compression is an indispensable trigger for all EMIC waves. Key Points: The amplitude‐dependent properties and excitation mechanisms of electromagnetic ion cyclotron (EMIC) waves are investigated with Van Allen Probe B data from 2013 to 2018Large‐amplitude EMIC waves tend to be more left‐hand polarized with smaller wave normal angles under high proton beta parallel conditionsSubstorm injection is vital in large‐amplitude EMIC wave excitation, while magnetospheric compression is indispensable for all EMIC waves [ABSTRACT FROM AUTHOR]

: Copyright of Journal of Geophysical Research. Space Physics is the property of Wiley-Blackwell and its content may not be copied or emailed to multiple sites or posted to a listserv without the copyright holder's express written permission. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)

المؤلفون: Zhou, Xu‐Zhi, Zhang, Xuan, Li, Jing‐Huan, Zong, Qiu‐Gang

المصدر: Geophysical Research Letters; 4/28/2021, Vol. 48 Issue 8, p1-10, 10p

مصطلحات موضوعية: MAGNETOPAUSE, GEOMAGNETISM, PLASMA sheaths, SOLAR wind, PARTICLE tracks (Nuclear physics), HEAVY ions, SQUARE root, IONS

مستخلص: Recent observations and particle‐tracing models have revealed a counterintuitive difference between the behaviors of magnetospheric protons and oxygen ions when they encounter the magnetopause. The oxygen ions usually meander around the magnetopause without a full escape to the magnetosheath, whereas the protons can more easily stream across the magnetopause despite their smaller gyroradii. Here, we analytically identify the mechanisms that cause this species dependence. As magnetospheric ions drift toward the magnetopause, the grazing angle of their magnetopause encounter is constrained within a narrow range near 0°, with its maximum being proportional to the square root of the ion gyroradius. It is the grazing angle that largely determines the follow‐up ion motion. The ions with larger grazing angles would meander around the magnetopause, whereas the meandering motion for ions with smaller grazing angles could be easily disrupted to enable their escape even if the normal magnetic field is very weak. Plain Language Summary: The Earth's magnetic field is constrained by the interplanetary field within a finite region named the magnetosphere. The boundary of this region, the magnetopause, separates the magnetospheric plasma from the cooler and denser population in the shocked solar wind. Some of the magnetospheric particles, however, can still penetrate the magnetopause and escape into the interplanetary space. One may expect that heavy ions, like singly charged oxygen ions, are more likely to escape than protons due to their larger gyroradii; however, the opposite trend has been identified in spacecraft observations. This counterintuitive feature, although reproduced in a particle‐tracing model, has not yet been fully understood. Here, we analyze the particle trajectories to identify the mechanism underlying the species dependence of the ion escape. When magnetospheric ions encounter the magnetopause, their grazing angles are constrained within a narrow range near 0°, with the maximum angle depending positively on ion gyroradius. We find that the ions with larger grazing angles would meander around the magnetopause without a full escape, whereas the meandering motion for those with smaller angles could be more easily disrupted by a weak normal magnetic field to enable their field‐aligned escape. Key Points: Despite their smaller gyroradii, protons are found more likely to escape from the magnetosphere than oxygen ionsA mechanism leading to the counterintuitive species dependence is analytically identified based on a simple modelThe model also explains the bifurcated gyrophase bunching of the oxygen ions observed in the magnetosheath [ABSTRACT FROM AUTHOR]

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المؤلفون: Li, Jing‐Huan¹ (AUTHOR) jinghuan.li@pku.edu.cn, Zhou, Xu‐Zhi¹ (AUTHOR) xzzhou@pku.edu.cn, Yang, Fan¹ (AUTHOR), Artemyev, Anton V.^2,3 (AUTHOR), Zong, Qiu‐Gang¹ (AUTHOR)

المصدر: Geophysical Research Letters. 3/28/2021, Vol. 48 Issue 6, p1-11. 11p.

مصطلحات موضوعية: *SPACE plasmas, *PARTICLE motion, *PLASMA pressure, *PLASMA density, *PLASMA instabilities

الشركة/الكيان: UNITED States. National Aeronautics & Space Administration

مستخلص: Magnetic cavities are sudden depressions of magnetic field strength widely observed in the space plasma environments, which are often accompanied by plasma density and pressure enhancement. To describe these cavities, self‐consistent kinetic models have been proposed as equilibrium solutions to the Vlasov‐Maxwell equations. However, observations from the Magnetospheric Multi‐Scale (MMS) constellation have shown the existence of helical magnetic cavities characterized by the presence of azimuthal magnetic field, which could not be reconstructed by the aforementioned models. Here, we take into account another invariant of motion, the canonical axial momentum, to construct the particle distributions and accordingly modify the equilibrium model. The reconstructed magnetic cavity shows excellent agreement with the MMS1 observations not only in the electromagnetic field and plasma moment profiles but also in electron pitch‐angle distributions. With the same set of parameters, the model also predicts signatures of the neighboring MMS3 spacecraft, matching its observations satisfactorily. Plain Language Summary: Magnetic cavities, also referred to as magnetic holes, are ubiquitous in the space plasma environment characterized by depressed magnetic field strength and enhanced plasma pressure. These structures are usually believed to result from plasma instabilities, although recent observations and simulations have suggested their quasi‐stationary nature. Kinetic models of magnetic cavities have been also proposed, which show excellent agreement with spacecraft observations to indicate the formation of quasi‐equilibrium cavities during the turbulent evolution of space plasmas. These models, however, apply only to magnetic cavities with straight field lines, and therefore cannot describe the helical magnetic cavities recently discovered by NASA's Magnetospheric Multi‐Scale (MMS) constellation. In this paper, we propose a revised model by incorporating the canonical axial momentum as an additional invariant of particle motion into the particle distributions, to resolve the self‐consistent profiles of the electromagnetic field and particle distributions within the magnetic cavity. This revision accommodates the field‐aligned current to support the helical field lines, which shows remarkable agreement with the observations from the MMS constellation. Key Points: Spacecraft observations of magnetic cavities are sometimes accompanied by azimuthal magnetic field indicating the helical structureKinetic, equilibrium model of helical magnetic cavities is developed based on four invariants of particle motionThe model reproduces the MMS observations of helical magnetic cavities in both electromagnetic field and particle distributions [ABSTRACT FROM AUTHOR]

المؤلفون: Li, Jing‐Huan¹ (AUTHOR), Zhou, Xu‐Zhi¹ (AUTHOR) xzzhou@pku.edu.cn, Zong, Qiu‐Gang¹ (AUTHOR), Yang, Fan¹ (AUTHOR), Fu, Suiyan¹ (AUTHOR), Yao, Shutao² (AUTHOR), Liu, Ji³ (AUTHOR), Shi, Quanqi² (AUTHOR)

المصدر: Geophysical Research Letters. 1/28/2021, Vol. 48 Issue 2, p1-11. 11p.

مصطلحات موضوعية: *LIOUVILLE'S theorem, *ELECTRON distribution, *MUSICAL pitch, *SPACE plasmas, *MAGNETIC structure, *PHASE space, *PLASMA pressure

مستخلص: Magnetic cavities, also known as magnetic holes, are ubiquitous in space plasmas characterized by depressed magnetic strength and enhanced plasma pressure. Most of the observed cavities are associated with anisotropic particle distributions with higher fluxes in the direction perpendicular to the magnetic field. Recent observations of kinetic‐scale magnetic cavities have identified another type of electron distributions in the pitch angle spectrum, the so‐called donut‐shaped distributions, although their formation mechanism remains unclear. Here, we present a simplistic model of cavity shrinkage and deepening, in which electrons are traced backward in time to the initial, equilibrium‐state cavity. The resulting electron distributions, determined from Liouville's theorem, agree with the observations in the presence of donut‐shaped pitch angle structures. The model also enables a quantitative evaluation on the roles of betatron cooling, radial transport, and pitch angle variations in the formation of donut‐shaped electron distributions within evolving magnetic cavities. Plain Language Summary: Satellite observations of the space plasma environments have identified many localized structures with reduced magnetic field amplitude in an otherwise unperturbed background. These structures, referred to as magnetic cavities or holes, are usually observed in association with anisotropic particle distributions, with higher fluxes in the direction perpendicular to the magnetic field. It is these anisotropic distributions that provide the strongest support to the prevalent understanding that magnetic cavities are generated via mirror or electron‐mirror instabilities. However, recent observations have identified a different type of electron distributions in kinetic‐scale magnetic cavities, the so‐called donut‐shaped distributions after their characteristic appearances in the electron pitch angle spectrum. In this paper, we examine the hypothesis that donut‐shaped electron distributions originate from the simultaneous deepening and shrinkage of magnetic cavities, a process identified in recent observations. To do so, we carry out a particle‐tracing simulation to analyze the electron behavior within the evolving magnetic cavity, which includes the adiabatic betatron cooling, radial transport, and pitch angle variations. The variations of the electron phase space densities are then computed based on Liouville's theorem, which results in donut‐shaped distributions consistent with observations from NASA's Magnetospheric Multiscale mission. Key Points: Magnetic cavity electrons sometimes display donut‐shaped pitch angle distributions, which differ from their usual, 90°‐concentrated formNumerical simulations show that donut‐shaped electron distributions originate from the shrinkage and deepening of magnetic cavitiesThe donut‐shaped distributions are formed by the combined effects of betatron cooling, radial transport, and pitch angle variations [ABSTRACT FROM AUTHOR]

المؤلفون: Su, Xiaoxia, Jing, Huan, Yu, Wenting, Lei, Fengzhen, Wang, Rui, Hu, Cheng, Li, Mujia, Lin, Tingting, Zhou, Hong, Wang, Fei, Liao, Li

المصدر: Journal of Biomedical Materials Research, Part A; Sep2020, Vol. 108 Issue 9, p1955-1967, 13p

مستخلص: Replicative senescence during in vitro augmentation, which is mostly induced by the loss of physiological microenvironment, hinders the application of mesenchymal stem cells (MSCs) in the clinic. Here, we investigated whether MSCs senescence could be prevented by bio‐scaffold mimicking the natural tissue matrix. Human umbilical cord mesenchymal stem cells (hUCMSCs) exhibited a senescent phenotype during a long‐term passage in the conventional culture dish. To fabricate the bone matrix, a naturally based matrix composed of nano‐hydroxyapatite/chitosan/poly lactide‐co‐glycolide (nHA/CS/PLGA) was produced. Long‐term passage resulted in an obvious increase in the expression of senescence markers and a reduction in the expression of master genes involved in tissue regeneration. Functional assay confirmed that nHA/CS/PLGA scaffold preserved the proliferation and differentiation of hUCMSCs even after being passaged 27 times. Moreover, in vivo ectopic bone formation assay revealed that the bone formation of hUCMSCs cultured on the nano‐scaffolds for the long term was as robust as the cells in the early passage. In summary, our results demonstrate that nHA/CS/PLGA scaffold effectively preserves the stemness and youth of hUCMSCs in the long‐term passage. Taken advantage of its compatibility and bioactivity, nHA/CS/PLGA scaffold is of great potential in large‐scale expansion of MSCs for stem cell therapy and tissue engineering. [ABSTRACT FROM AUTHOR]

: Copyright of Journal of Biomedical Materials Research, Part A is the property of Wiley-Blackwell and its content may not be copied or emailed to multiple sites or posted to a listserv without the copyright holder's express written permission. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)

المؤلفون: Tang, Simin, Jing, Huan, Huang, Zhenxing, Huang, Teng, Lin, Sen, Liao, Meijuan, Zhou, Jun

المصدر: Journal of Cellular Biochemistry; Feb2020, Vol. 121 Issue 2, p1635-1648, 14p

المؤلفون: Lin, Chuan, Yang, Jun, Fuller, Peter J., Jing, Huan, Song, Ying, He, Wenwen, Du, Zhipeng, Luo, Ting, Cheng, Qingfeng, Yang, Shumin, Wang, Hongman, Li, Qifu, Hu, Jinbo, Mei, Mei, Luo, Suxin, Liao, Kangla, Zhang, Yao, He, Yunfeng, He, Yihong, Xiao, Ming

المصدر: Clinical Endocrinology; Feb2020, Vol. 92 Issue 2, p131-137, 7p, 1 Diagram, 3 Charts, 1 Graph

مصطلحات موضوعية: DIAGNOSIS methods, HYPERALDOSTERONISM

مستخلص: Context: The saline infusion test (SIT) is a common confirmatory test for primary aldosteronism (PA). According to the guideline, a postinfusion plasma aldosterone concentration (PAC) of 5‐10 ng/dL is considered indeterminate, and recommendations for diagnostic strategies are currently limited in this situation. Objective: To explore whether an addition of the captopril challenge test (CCT) could improve the diagnostic accuracy in patients with indeterminate SIT. Methods: A total of 280 hypertensive patients with high risk of PA completed this study. Subjects were defined as SIT indeterminate based on their PAC post‐SIT. These patients then underwent the CCT where PACs post‐CCT >11 ng/dL were considered positive. Using fludrocortisone suppression test (FST) as the reference standard, diagnostic parameters including area under the receiver‐operator characteristic curves (AUC), sensitivity and specificity were calculated. Results: There were 65 subjects (23.2%) diagnosed as PA indeterminate after SIT. With the addition of CCT, true‐positive numbers increased from 134 to 147, and false‐negative numbers decreased from 27 to 14. Compared to SIT alone, a combination of SIT and CCT showed a higher AUC (0.91 [0.87,0.94] vs 0.87 [0.83,0.91], P =.041) and an increased sensitivity for the diagnosis of PA (0.91 [0.86,0.95] vs 0.83 [0.76,0.89], P =.028), while the specificity remained similar. In the subgroup with indeterminate SIT results, using PAC post‐CCT resulted in a 36% higher AUC than using PAC post‐SIT alone for the diagnosis of PA. Conclusion: For patients under investigation for possible PA who have indeterminate SIT results, an addition of CCT improves the diagnostic accuracy. [ABSTRACT FROM AUTHOR]

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المؤلفون: Shen, Yi‐Fan¹ (AUTHOR), Huang, Jing‐Huan¹ (AUTHOR), Li, Xiao‐Lin¹ (AUTHOR), Gao, Hong¹ (AUTHOR) honggao630@163.com

المصدر: ANZ Journal of Surgery. Oct2019, Vol. 89 Issue 10, pE422-E427. 6p. 2 Color Photographs, 1 Diagram, 2 Charts.

مصطلحات موضوعية: *SOFTWARE measurement, *COMPUTER software, *COMPUTED tomography, *HUMAN abnormalities, *MEASUREMENT

مستخلص: Background: A novel measurement technique has been designed to assess femoral rotation deformation. The purpose of this study was to evaluate smartphone‐aided measurement, including measurement software, intra‐observer differences and the occurrence frequency of the unacceptable outliers. Methods: Five positions (intact bone, external and internal rotations of 20° and 40° of the distal blocks after dividing the femoral shafts using a saw) were used in each of the five artificial femora. Guide wires were separately inserted into the proximal and distal ends of the model femora with a navigation system and the intersection angles between the guide wires were measured with a smartphone. The values obtained by two measurement software packages (Smart Tools and Super Swiss Army Knife) were compared with that measured on the overlapped computed tomography images. Results: There were no significant differences between the intersection angles measured by smartphone and that measured on the overlapped images (P = 0.24). The mean absolute difference between pairs of measurements of the two software packages for all guide wire angles was 2.33 ± 2.34°, without statistically significant difference (P = 0.33). There was a significant correlation (r = 0.99) between the first and second (1 week apart) measurements with the same measurement tool. The values of offset capability index of the Smart Tools and the Super Swiss Army Knife measurement tools were 1.62 and 1.13, respectively. Conclusion: Smartphone‐aided measurement technique could reliably assess femoral rotation deformation with more accurate angle measurement for software with zero calibration function. [ABSTRACT FROM AUTHOR]