76 research outputs found

    Solar flares: waiting time characterization using a cellular automaton model

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    El modelo de avalanchas de Lu & Hamilton (LH91) ha sido, por casi 30 años, una herramienta de gran importancia para modelar la naturaleza intermitente de las erupciones solares. En este trabajo se utiliza el modelo bidimensional de Lu & Hamilton para abordar el problema del comportamiento estadístico del tiempo entre avalanchas y la posibilidad de pronosticar erupciones solares sintéticas. Se trabajó con tres definiciones diferentes de tiempo entre avalanchas: ∆T (el número de iteraciones entre el inicio y el final de una avalancha), ∆Tii (número de iteraciones entre el inicio de una avalancha y el inicio de la avalancha siguiente) y ∆TP (el número de iteraciones entre dos picos de avalanchas consecutivas. Para el caso de la definición habitual de tiempo entre, avalanchas (∆T) se encontró que puede describirse estadísticamente mediante una función exponencial mientras que, para las otras dos definiciones el comportamiento en tipo power law con valores similares a los hallados en observaciones solares.For almost 30 years the Lu & Hamilton avalanche model (LH91) has been the paramount tool to study the intermittent nature of solar flares via avalanche models. In this work we used the two-dimensional model of Lu & Hamilton to assess the statistics of the waiting time between avalanches and the possibility forecasting synthetic solar flares. We worked with three different definitions of waiting time between: ∆T, ∆Tii and ∆TP. For the case of the usual definition of the waiting time between avalanches (∆T) we found that the statistics can be described statistically through an exponential function. For the other definitions they present power-law statistics with exponents that compare well with solar observations.Fil: Morales, Laura Fernanda. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Física del Plasma. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Física del Plasma; ArgentinaFil: Kychenthal, Matias Andres. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Física del Plasma. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Física del Plasma; Argentin

    Why The Trans Programmer?

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    Through online anecdotal evidence and online communities, there is an in-group idea of trans people (specifically trans-feminine individuals) disproportionately entering computer science education &amp;amp; fields. Existing data suggests this is a plausible trend, yet no research has been done into exactly why. As computer science education (traditional schooling or self-taught methods) is integral to working in computer science fields, a simple research survey was conducted to gather data on 138 trans people’s experiences with computer science &amp;amp; computer science education. This article’s purpose is to shed insight on the motivations for trans individuals choosing computer science paths, while acting as a basis and call to action for further research.</p

    Why The Trans Programmer?

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    VITRECTOMY AFTER INTRAVITREAL BEVACIZUMAB (AVASTIN) FOR RETINAL DETACHMENT IN RETINOPATHY OF PREMATURITY

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    Alternative Waiting Time Statistics for the Lu and Hamilton Avalanche Model

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    The solar corona hosts many explosive events. Among them, flares are some of the most energetic, rapidly releasing huge amounts of energy and, in the case of the largest ones, producing coronal mass ejections that have the potential to harm life on our planet. Therefore, there is great interest in attempting to foresee the occurrence of extreme solar flares. Avalanche models for solar flares have been used since the beginning of the 1990s to model the flaring corona in a simple and computationally inexpensive way. The pioneering and now most prevalent model in the literature was proposed by Lu and Hamilton. This model has been extremely useful to reproduce most of the main characteristic features observed in solar flares (e.g., the probability density function of a flare’s energy) and, in recent years, has been used as the starting point to predict extreme flaring events. In this work, we revisit Lu and Hamilton’s model and the very definition of waiting time for both extreme and all-sized events. We find that extreme avalanche statistics are well described by a log-normal distribution, in accordance with recent observations of solar flares

    TREATMENT OF TYPE 1 RETINOPATHY OF PREMATURITY WITH INTRAVITREAL BEVACIZUMAB (AVASTIN)

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    Zone I retinopathy of prematurity

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    Management of Stage 4 ROP

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