Biography:

In the past M.E. Machado has collaborated on articles with C.H. Mandrini and B. Schmieder. One of their most recent publications is Observed signatures of magnetic energy conversion in solar flares and microflares. Which was published in journal Advances in Space Research.

More information about M.E. Machado research including statistics on their citations can be found on their Copernicus Academic profile page.

M.E. Machado's Articles: (4)

Observed signatures of magnetic energy conversion in solar flares and microflares

AbstractWe follow up on our earlier studies of the characteristics of energy release in solar flares, extending it to weak flare-like transient brightenings which are called “microflares”. We find that all events share similar properties in spite of their large differences in X-ray brightness, including the fact that their trigger seems to be due to the interaction of impacted bipolar regions which leads to the release of their internally stored energy. The overall topology of the energy release region is preserved over a period in which an active region produced numerous events, except at the site of a two ribbon flare, which probably led to a permanent disruption of the magnetic configuration. Our results suggest that transient microflares can be responsible for a large fraction of the coronal heating in active regions, and we propose a picture in which reconnection may act as a catalyst for the release of stored magnetic energy.

Relationship between magnetic field evolution and flaring sites in AR 6659 on June 1991

AbstractDuring the international campaign of June 1991, the active region AR 6659 produced 6 very large long duration flares at the same location during its passage across the solar disk. Vector magnetograms were obtained at Marshall (Huntsville) and Huairou Station (Beijing) with a time difference of 10 to 12 hours, thus giving a good survey of the magnetic field evolution with time. The flare of June 6/01:08 UT (X12 plus/4B) was observed in Shahe Station (Beijing) in white light, in Hα and in radio centimetric wavelengths. The evolution of the flare of June 9/01:43 UT (X10/3B) has been followed in Hα at the Yunnan Observatory (Kunming). An other one was well observed on June 15 at 08:20 UT in Wroclaw and in Debrecen. Some subflares were observed at Sac Peak on June 4, 5, 7 at Meudon on June 10, 14 and Debrecen on June 12 and 13.In this short communication we concentrate on the relationship between magnetic field shear and flare sites.

The fine scale temporal structure of hard X-ray bursts

AbstractWe report on the preliminary analysis of fast temporal fluctuations observed in hard X-ray bursts, as recorded by the Burst and Transient Source Experiment (BATSE) on the Compton Gamma Ray Observatory.

Backscatter LIDAR signal simulation applied to spacecraft LIDAR instrument design

AbstractIn the framework of the scientific cooperation between the CEILAP laboratory (Argentina) and IPSL Institut Pierre Simon Laplace (France), devoted to the development of LIDAR techniques for Atmospheric sciences, a new area of scientific research, involving LIDARs, is starting in Argentine space technology. This new research area is under consideration at CEILAP in a joint effort with CONAE, the Argentine space agency, responsible for the development of future space missions. The LIDAR technique is necessary to improve our knowledge of meteorological, dynamic, and radiative processes in the South American region, for the whole troposphere and the lower stratosphere. To study this future mission, a simple model for the prediction of backscatter LIDAR signal from a spacecraft platform has been used to determine dimensions and detection characteristics of the space borne LIDAR instrument. The backscatter signal was retrieved from a modeled atmosphere considering its molecular density profile and taking into account different aerosols and clouds conditions. Signal-to-noise consideration, within the interval of possible dimension of the instrument parameters, allows us to constrain the telescope receiving area and to derive maximum range achievable, integration time and the final spatial and temporal resolutions of backscatter profiles.

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