Comparison of ultra-low-frequency waves at Mercury under northward and southward IMF

[1] Narrow-band ultra-low-frequency (ULF) waves at frequencies greater than the He + cyclotron frequency (f cHe+ ) were detected during MESSENGER's first two Mercury flybys. The waves were observed primarily between closest approach (CA) and the outbound magnetopause. The magnetosphere was very quiet during the first flyby (M1) and highly disturbed during the second flyby (M2); that ULF waves were observed during both flybys despite these different magnetospheric conditions is remarkable. The wave frequency structure in the boundary layer (BL) was similar between M1 and M2. Between CA and the BL, for M1 the wave frequency rose systematically from f cHe+ to the proton cyclotron frequency (f cH+ ), while during M2 two frequency bands were observed, one near the He ++ cyclotron frequency and one near f cH+ . The main difference in the waves between the two flybys, apart from their frequency structure, was their power, which was 4 to 5 times larger during M2 than during M1. Citation: Boardsen

Comparison of ultra-low-frequency waves at Mercury under northward and southward IMF

[1] Narrow-band ultra-low-frequency (ULF) waves at frequencies greater than the He + cyclotron frequency (f cHe+ ) were detected during MESSENGER's first two Mercury flybys. The waves were observed primarily between closest approach (CA) and the outbound magnetopause. The magnetosphere was very quiet during the first flyby (M1) and highly disturbed during the second flyby (M2); that ULF waves were observed during both flybys despite these different magnetospheric conditions is remarkable. The wave frequency structure in the boundary layer (BL) was similar between M1 and M2. Between CA and the BL, for M1 the wave frequency rose systematically from f cHe+ to the proton cyclotron frequency (f cH+ ), while during M2 two frequency bands were observed, one near the He ++ cyclotron frequency and one near f cH+ . The main difference in the waves between the two flybys, apart from their frequency structure, was their power, which was 4 to 5 times larger during M2 than during M1. Citation: Boardsen

Overcorrection during treatment of pectus deformities with DCC orthoses: experience in 17 cases

Treatment of pectus carinatum and pectus excavatum with dynamic chest compressor (DCC) orthoses have been reported by Haje and others. The goal of this study was to demonstrate that overcorrection during orthotic treatment of children and adolescents with pectus deformities can occur and requires medical attention. Of 3,028 children and adolescents with pectus deformities, observed between 1977 and October 2005, 1,824 were prescribed treatment with DCC orthoses and, after a few months of treatment, some overcorrection was noted in 30 patients. Of the patients who received orthoses, 738 had a minimum follow-up of 1 year and 17 of these, 2 with pectus excavatum and 15 with pectus carinatum, presented overcorrection and were studied. The dynamic remodeling method (DCC orthoses + exercises) was applied. The procedures, adopted according to each patient’s needs, were: decreasing the time of orthosis wear and/or the tightening of the screws, introducing a second orthosis, and improving the prescribed exercises and/or encouraging the patient to perform them more intensively. The therapy was successful in all patients, and the result was maintained in one case of pectus excavatum followed up until adulthood. It was concluded that overcorrection during DCC orthosis wear can occur and that careful medical follow-up is necessary if this complication is to be successfully reversed

Statistical study of ICME effects on Mercury\u27s magnetospheric boundaries and northern cusp region from MESSENGER

This paper presents a systematic investigation of the large-scale processes in Mercury\u27s magnetosphere during interplanetary coronal mass ejections (ICMEs) using observations from the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) mission. We study the motion of the bow shock and magnetopause boundaries, quantify the magnetospheric compression, and characterize the size, extent, and plasma pressure of the northern cusp region and the plasma precipitation to the surface. During ICMEs, the magnetopause was substantially compressed, as the subsolar standoff distance from the center of the planet was reduced by ∼15% compared with the value during nominal solar wind conditions, and the magnetopause reached the surface of the planet ∼30% of the time. On the other hand, the bow shock under ICME conditions was located farther from the planet than for nominal solar wind conditions. The cusp was observed to extend ∼10° farther equatorward and 2 h wider in local time. In addition, the average plasma pressure in the cusp was more than double that determined under nominal conditions. For the most extreme cases, the particle precipitation to the surface was an order of magnitude higher than on average. The solar wind ram pressure and the Alfvén Mach number are found to be the dominant factors affecting these changes in the magnetosphere, with the interplanetary magnetic field (IMF) direction and the IMF magnetic pressure playing a small but likely nonnegligible role

Utilização da tomografia computadorizada quantitativa como teste de resistência para avaliação de placas ósseas

Quantitative computed tomography was used to determine the radiodensity of bony plates. The CT scans provided information regarding radiodensity of bony plates and allowed to verify the uniformity of bone mineral density in their scope. The proposed methodology should be considered as another tool for determining the resistance of these biomaterials