Estimation of a coronal mass ejection magnetic field strength using radio observations of gyrosynchrotron radiation

Coronal mass ejections (CMEs) are large eruptions of plasma and magnetic field from the low solar corona into interplanetary space. These eruptions are often associated with the acceleration of energetic electrons which produce various sources of high intensity plasma emission. In relatively rare cases, the energetic electrons may also produce gyrosynchrotron emission from within the CME itself, allowing for a diagnostic of the CME magnetic field strength. Such a magnetic field diagnostic is important for evaluating the total magnetic energy content of the CME, which is ultimately what drives the eruption. Here, we report on an unusually large source of gyrosynchrotron radiation in the form of a type IV radio burst associated with a CME occurring on 2014-September-01, observed using instrumentation from the Nançay Radio Astronomy Facility. A combination of spectral flux density measurements from the Nançay instruments and the Radio Solar Telescope Network (RSTN) from 300 MHz to 5 GHz reveals a gyrosynchrotron spectrum with a peak flux density at ∼1 GHz. Using this radio analysis, a model for gyrosynchrotron radiation, a non-thermal electron density diagnostic using the Fermi Gamma Ray Burst Monitor (GBM) and images of the eruption from the GOES Soft X-ray Imager (SXI), we were able to calculate both the magnetic field strength and the properties of the X-ray and radio emitting energetic electrons within the CME. We find the radio emission is produced by non-thermal electrons of energies >1 MeV with a spectral index of δ ∼ 3 in a CME magnetic field of 4.4 G at a height of 1.3 R�, while the X-ray emission is produced from a similar distribution of electrons but with much lower energies on the order of 10 keV. We conclude by comparing the electron distribution characteristics derived from both X-ray and radio and show how such an analysis can be used to define the plasma and bulk properties of a CME

Transition region and chromospheric signatures of impulsive heating events. II. Modeling

Results from the Solar Maximum Mission showed a close connection between the hard X-ray (HXR) and transition region (TR) emission in solar flares. Analogously, the modern combination of RHESSI and IRIS data can inform the details of heating processes in ways that were never before possible. We study a small event that was observed with RHESSI, IRIS, SDO, and Hinode, allowing us to strongly constrain the heating and hydrodynamical properties of the flare, with detailed observations presented in a previous paper. Long duration redshifts of TR lines observed in this event, as well as many other events, are fundamentally incompatible with chromospheric condensation on a single loop. We combine RHESSI and IRIS data to measure the energy partition among the many magnetic strands that comprise the flare. Using that observationally determined energy partition, we show that a proper multithreaded model can reproduce these redshifts in magnitude, duration, and line intensity, while simultaneously being well constrained by the observed density, temperature, and emission measure. We comment on the implications for both RHESSI and IRIS observations of flares in general, namely that: (1) a single loop model is inconsistent with long duration redshifts, among other observables; (2) the average time between energization of strands is less than 10 s, which implies that for a HXR burst lasting 10 minutes, there were at least 60 strands within a single IRIS pixel located on the flare ribbon; (3) the majority of these strands were explosively heated with an energy distribution well described by a power law of slope »-1.6; (4) the multi-stranded model reproduces the observed line profiles, peak temperatures, differential emission measure distributions, and densities

Modelos numéricos con malhas tetraédricas de 4 e 10 nós do fémur distal e da tíbia proximal para o estudo de próteses do joelho

Existe alguma controvérsia sobre a adequabilidade dos elementos finitos tetraédricos lineares de 4 nós e quadráticos de 10 nós para simulações de estruturas ósseas presentes em determinados problemas da biomecânica. Neste artigo analisa-se o desempenho destes dois tipos de elementos na modelação numérica do fémur distal e da tíbia proximal, necessárias para estudos sobre a prótese do joelho. Faz-se também estudo complementar experimental com uso de extensometria para comparação das extensões obtidas com as deformações numéricas. Os resultados mostram que se obtém excelente correlação numérica-experimental para malhas tetraédricas de 4 nós, com 6 graus de liberdade por nó, com um número de graus de liberdade superiores a 125000 para a tíbia e superiores a 160000 para o fémur

Efeitos da haste press-fit na artroplastia total do joelho. Influência da haste tibial no fémure e da haste tíbia

Este artigo descreve um estudo que teve como principal objectivo determinar as alterações biomecânicas induzidas pela utilização de hastes press-fit no osso contrário do joelho devido à revisão da artroplastia do mesmo. Considerou-se a prótese do joelho (modelo P.F.C. Sigma Modular Knee System) constituída pela componente femoral e componente tibial sem hastes. Outros dois sistemas foram comparados com este, nomeadamente um com componente femoral sem haste e componente tibial com haste press-fit e um outro com componente tibial sem haste e componente femoral com haste press-fit. Analisou-se a influência da utilização das hastes no osso contrário, em comparação com a prótese sem qualquer haste. Analisaram-se as alterações referentes à repartição de carga transferida na interface osso esponjoso-cimento, às deformações principais de compressão no osso esponjoso, aos micromovimentos entre os componentes e o osso cortical e à estabilidade da interface osso-cimento. Os resultados evidenciaram que a utilização da haste tibial não altera de forma significativa o comportamento biomecânico da ligação do componente femoral ao fémur. O mesmo se verificou quando se utilizou uma haste femoral, onde as alterações de estabilidade induzidas na tíbia com componente tibial foram bastante significativas, podendo por em causa a longevidade da fixação do componente tibial

Strain field analysis of cancellous bone under compression by image correlation

Experimental mechanical analysis of cancellous bone has been performed to capture the global strain field of specimens under compression. One major objective is to assess the test procedure and obtain the cancellous bone mechanical properties. Now a day, several techniques are available for the experimental measurement of the field displacement. Among them, the Cross-Correlation is one of most simple’s techniques and can be applied to several studies cases. Based on the correlation of random speckle pattern between two images, the spatial displacement fields can be accessed. A simple digital camera or video recorder can be used without special light to capture the surface intensity pattern in each instant. If several images are taken during a test loading, the displacement field can be fallowed and subsequently the strain can be obtain by the spatial differentiation. Because of random surface pattern, the image can be divided in small areas, each of them pattern independent. By cross-correlating each of one between the two images, the relative displacement is obtained

Spontaneous parity violation and minimal Higgs models

In this paper we present a model for the spontaneous breaking of parity with two Higgs doublets and two neutral Higgs singlets which are even and odd under D-parity. The condition $v_R >>v_L$ can be satisfied without introducing bidoublets and it is induced by the breaking of D-parity through the vacuum expectation value of the odd Higgs singlet. Examples of left-right symmetric and mirror fermions models in grand unified theories are presented.Comment: Revised version. Accepted in Eur. Phys. Journal

Single neutral heavy lepton production at electron-muon colliders

New heavy Majorana and Dirac neutrinos production at future electron-muon colliders are investigated. The production of a single heavy neutrino is shown to be more relevant than pair production when comparing cross sections and neutrino mass ranges. The process $e^\pm \mu^\mp \longrightarrow {\nu} \ell^{\pm} W^{\mp}$ is studied including on-shell and off-shell heavy neutrino effects. Distributions are calculated including hadronization effects and experimental cuts that suppress background, in order to have a clear signal for heavy neutral leptons.Comment: 4 pages, 14 jpg figures, Published Phys.Lett B494 (2000) 273-27

Characterization of oil shale residue and rejects from irati formation by electron paramagnetic resonance

In this study, sedimentary organic matter of oil shale rejects, calschist, shale fine and the so called retorted shale from Irati formation was characterized. EPR was used to analyse the samples regarding loss of signal in g = 2.003 associated to the organic free radical with the calcined samples and washing with hydrogen peroxide. The radical signal was detected in all samples, however, for the calschist and shale fine samples another signal was identified at g = 2.000 which disappeared when the sample was heated at 400 ºC. Hydrogen peroxide washing was also performed and it was noted that after washing the signal appeared around g = 2.000 for all samples, including retorted shale, which might be due to the quartz E1 defect

Reproducing type II white-light solar flare observations with electron and proton beam simulations

We investigate the cause of the suppressed Balmer series and the origin of the white-light continuum emission in the X1.0 class solar flare on 2014 June 11. We use radiative hydrodynamic simulations to model the response of the flaring atmosphere to both electron and proton beams, which are energetically constrained using Ramaty High Energy Solar Spectroscopic Imager and Fermi observations. A comparison of synthetic spectra with the observations allows us to narrow the range of beam fluxes and low energy cutoff that may be applicable to this event. We conclude that the electron and proton beams that can reproduce the observed spectral features are those that have relatively low fluxes and high values for the low energy cutoff. While electron beams shift the upper chromosphere and transition region to greater geometrical heights, proton beams with a similar flux leave these areas of the atmosphere relatively undisturbed. It is easier for proton beams to penetrate to the deeper layers and not deposit their energy in the upper chromosphere where the Balmer lines are formed. The relatively weak particle beams that are applicable to this flare do not cause a significant shift of the τ = 1 surface and the observed excess WL emission is optically thin