Estimating the mass of CMEs from the analysis of EUV dimmings

Context. Reliable estimates of the mass of coronal mass ejections (CMEs) are required to quantify their energy and predict how they affect space weather. When a CME propagates near the observer's line of sight, these tasks involve considerable errors, which motivated us to develop alternative means for estimating the CME mass. Aims. We aim at further developing and testing a method that allows estimating the mass of CMEs that propagate approximately along the observer's line of sight. Methods. We analyzed the temporal evolution of the mass of 32 white-light CMEs propagating across heliocentric heights of 2.5-15 R, in combination with that of the mass evacuated from the associated low coronal dimming regions. The mass of the white-light CMEs was determined through existing methods, while the mass evacuated by each CME in the low corona was estimated using a recently developed technique that analyzes the dimming in extreme-UV (EUV) images. The combined white-light and EUV analyses allow the quantification of an empirical function that describes the evolution of CME mass with height. Results. The analysis of 32 events yielded reliable estimates of the masses of front-side CMEs. We quantified the success of the method by calculating the relative error with respect to the mass of CMEs determined from white-light STEREO data, where the CMEs propagate close to the plane of sky. The median for the relative error in absolute values is ≈30%; 75% of the events in our sample have an absolute relative error smaller than 51%. The sources of uncertainty include the lack of knowledge of piled-up material, subsequent additional mass supply from the dimming region, and limitations in the mass-loss estimation from EUV data. The proposed method does not rely on assumptions of CME size or distance to the observer's plane of sky and is solely based on the determination of the mass that is evacuated in the low corona. It therefore represents a valuable tool for estimating the mass of Earth-directed events.Fil: López, F. M.. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaFil: Cremades Fernandez, Maria Hebe. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Tecnológica Nacional; ArgentinaFil: Balmaceda, Laura Antonia. George Mason University; Estados Unidos. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaFil: Nuevo, Federico Alberto. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Vásquez, A. M.. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina. Universidad Nacional de Tres de Febrero; Argentin

Identificación de interacciones de partículas en sensores de imágenes de silicio.

Se desarrolló un código en C que permite obtener y analizar las imagenes raw obtenidas por sensores CMOS, para la detección de interacción de partículas con el sensor. Además de la interfaz por consola, se desarrollaron dos interfaces web que permiten visualizar la información procesada. Gracias a este software, se fabricó un prototipo de un monitor del nivel de actividad de radón. Para ello, se construyó un concentrador de iones con un material conductor, un soporte impreso en 3D, y un sensor CMOS. Los datos obtenidos fueron procesados por una raspberry pi, modelo 3B+. Se demostró el correcto funcionamiento del código y del concentrador de iones para la detección de partículas alfa, provenientes de partículas inestables previamente depositadas sobre el sensor. Se analizó la forma de los eventos de las partículas alfas detectadas, y su distribución sobre el sensor. Las mediciones se contrastaron con un medidor de radón disponible comercialmente, observándose cierta inercia en la medición dada por dicho sensor. Además, con el fin de detectar concentraciones de plomo en agua, se utilizaron sensores CCDs para la detección de los picos Lα y Lβ del plomo. Para ello se colocó una lámina de plomo sobre una mitad del sensor y una lámina de cobre sobre la otra mitad. El cobre utilizado permitió una correcta calibración de la energía de los eventos detectados. Se calculó el flujo eventos que se espera para los picos Lα y Lβ del plomo, con estos resultados se extrapoló al sensores CMOS utilizado anterior, y se adaptó un experimento su verificación. Por otro lado, se utilizaron técnicas de Machine Learning para la clasificación de imágenes en eventos y ruidos. Estas imágenes fueron simuladas tomando un ruido gaussiano para cada pixel y, en el caso de las imágenes de eventos, distribuyendo n cargas unitarias sobre el centro del sensor, siguiendo distribución gaussiana. Todas las imágenes sufrieron un proceso de pre-selección. Se implementó una red neuronal convolucional con una única capa convolucional y una capa densa y se observó la dependencia de la precisión como función de la cantidad de cargas n distribuídas en el conjunto de datos de entrenamiento

Economic evaluation of sunitinib versus pazopanib and best supportive care for the treatment of metastatic renal cell carcinoma in Chile: cost-effectiveness analysis and a mixed treatment comparison

© 2019, © 2019 Informa UK Limited, trading as Taylor & Francis Group. Background: Sunitinib and Pazopanib are two metastatic renal cell carcinoma (MRCC) treatment alternatives, however the health system in Chile does not consider coverage for any. The cost-effectiveness versus relevant comparator was assessed to support evidence-based decision making. Methods: A four health states Markov model was built: first, second line treatments, BSC and death. Benefits were measured in QALYs, and efficacy estimates were obtained from an indirect treatment comparison. A 10-year time horizon and a 3% undifferentiated discount rate were considered. Deterministic and probabilistic sensitivity analyses were performed. Results: The costs of treating MRCC with Sunitinib were higher than Pazopanib and BSC. When comparing Sunitinib versus Pazopanib, the incremental benefit is small favoring Sunitinib (0.03 QALYs). The base case scenario shows an average ICER of PA versus BSC of US$62,327.11/QALY and of US$85,885/QALY for Sunitinib versus Pazopanib. The ICER was most sensitive to the OS relative to BSC, where evidence was associated to important bias. Conclusions: Sunitinib or Pazopanib can be considered cost-effective if a 3 GDP per-capita threshold is assumed. The decision between SU or PA is highly sensitive to the price of the drugs, rather than the outcomes. Therefore, the decision might be made based on cost-minimization exercise

Daytime Sky Quality at El Leoncito, Argentina

We characterize the daytime sky quality in terms of brightness, cloud coverage, and main weather variables at the Carlos Ulrico Cesco station of the Felix Aguilar Astronomical Observatory (OAFA), located in El Leoncito National Park, San Juan, Argentina. We have collected more than 15 years of daily observations from the auxiliary sky brightness detectors of the Mirror Coronagraph for Argentina (MICA, in operations from 1997 to 2012), including daily observing reports. We additionally present data from two meteorological stations operated at the site from 2000 to 2020. We determine the main statistical properties and seasonal variability of daytime sky brightness, clear sky time fraction (CSTF), precipitable water vapor (WV), temperature, humidity, and wind speed, which are relevant for solar, particularly coronal observations. Our results confirm that El Leoncito is an excellent place to perform daytime astronomical observations. We measure a median sky brightness of 15.8 ppm, estimated at 526.0 ± 1.0 nm and 6 solar radii from the solar disk center; a median CSTF of 0.7; and a median WV below 6 mm. These values, and those of other relevant weather variables, are comparable to the levels found among the best astronomical observing sites in the world. Due to the extended period of time analyzed and high sampling frequency, the novel data and results presented in this report contribute to the analysis and interpretation of historical sky brightness data and are of great value for the future planning of daytime astronomical instrumentation at El Leoncito.Fil: Iglesias, F. A.. Universidad de Mendoza. Facultad de Ingenieria; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas; ArgentinaFil: Francile, Carlos Natale. Universidad Nacional de San Juan. Facultad de Ciencias Exactas Físicas y Naturales. Departamento de Informática. Observatorio Astronómico Félix Aguilar; ArgentinaFil: Lazarte Gelmetti, J.. Universidad Nacional de San Juan. Facultad de Ciencias Exactas, Físicas y Naturales; ArgentinaFil: Balmaceda, L. A.. George Mason University. School Of Physics. Astronomy And Computational Sciences; Estados Unidos. National Aeronautics and Space Administration; Estados UnidosFil: Cremades Fernandez, Maria Hebe. Universidad de Mendoza; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas; ArgentinaFil: Cisterna, F.. Universidad de Mendoza. Facultad de Ingenieria; Argentin

Solar energetic electron events measured by MESSENGER and Solar Orbiter. Peak intensity and energy spectrum radial dependences: statistical analysis

Context/Aims: We present a list of 61 solar energetic electron (SEE) events measured by the MESSENGER mission and the radial dependences of the electron peak intensity and the peak-intensity energy spectrum. The analysis comprises the period from 2010 to 2015, when MESSENGER heliocentric distance varied between 0.31 and 0.47 au. We also show the radial dependencies for a shorter list of 12 SEE events measured in February and March 2022 by spacecraft near 1 au and by Solar Orbiter around its first close perihelion at 0.32 au. Results: Due to the elevated background intensity level of the particle instrument on board MESSENGER, the SEE events measured by this mission are necessarily large and intense; most of them accompanied by a CME-driven shock, being widespread in heliolongitude, and displaying relativistic ($\sim$1 MeV) electron intensity enhancements. The two main conclusions derived from the analysis of the large SEE events measured by MESSENGER, which are generally supported by Solar Orbiter's data results, are: (1) There is a wide variability in the radial dependence of the electron peak intensity between $\sim$0.3 au and $\sim$1 au, but the peak intensities of the energetic electrons decrease with radial distance from the Sun in 27 out of 28 events. On average and within the uncertainties, we find a radial dependence consistent with $R^{-3}$. (2) The electron spectral index found in the energy range around 200 keV ($\delta$200) of the backward-scattered population near 0.3 au measured by MESSENGER is harder in 19 out of 20 (15 out of 18) events by a median factor of $\sim$20% ($\sim$10%) when comparing to the anti-sunward propagating beam (backward-scattered population) near 1 au.Comment: 20 pages, 13 figure

Sistema de comunicación de respaldo mediante tecnología LoRa con hardware y software abierto para aplicaciones de robótica de emergencias

Los sistemas de comunicación entre nodos sensores y los equipos de búsqueda y rescate presentan posibles vulnerabilidades ante emergencias o catástrofes, como el fallo de la infraestructura del sistema o la saturación de la red. Por ello, es necesario evaluar alternativas para garantizar la disponibilidad del sistema y los datos necesarios para la estrategia del equipo. Los requerimientos de una red de largo alcance y bajo consumo apuntan a evaluar las distintas tecnologías que engloban las redes LPWAN (Low Power, Wide Area Network). Entre ellas, destaca el protocolo LoRaWAN (Long Range, Wide Area Network) por ofrecer una flexibilidad operativa que no tienen los demás. De lado del hardware, se realizó una selección de componentes abiertos para los nodos sensores y el gateway. Para conseguir una red ad-hoc se ha usado el proyecto ChirpStack como servidor de red y de aplicación. Finalmente, se ha integrado el software de aplicación QGIS con la base de datos PostgreSQL que almacena los datos en la misma tarjeta host del gateway. El sistema fue probado en las XV Jornadas Internacionales de la Universidad de Málaga sobre Seguridad, Emergencias y Catástrofes. El código y la documentación del sistema presentado en este artículo está disponible en https://github.com/jjflozano/BackUpCommLoRa.Universidad de Málaga, Campus de Excelencia Internacional Andalucía Tech. Proyecto RTI2018-093421-B-I00, Ministerio de Ciencia, Innovación y Universidades, Programa Estatal de I+D+i 2018. Proyecto UMA18-FEDERJA-090, Programa operativo FEDER Andalucía 2014-2020, Convocatoria 2018, Junta de Andalucía

First near-relativistic solar electron events observed by EPD onboard Solar Orbiter

Context. Solar Orbiter, launched in February 2020, started its cruise phase in June 2020, in coincidence with its first perihelion at 0.51 au from the Sun. The in situ instruments onboard, including the Energetic Particle Detector (EPD), operate continuously during the cruise phase enabling the observation of solar energetic particles. Aims. In situ measurements of the first near-relativistic solar electron events observed in July 2020 by EPD are analyzed and the solar origins and the conditions for the interplanetary transport of these particles investigated. Methods. Electron observations from keV energies to the near-relativistic range were combined with the detection of type III radio bursts and extreme ultraviolet (EUV) observations from multiple spacecraft in order to identify the solar origin of the electron events. Electron anisotropies and timing as well as the plasma and magnetic field environment were evaluated to characterize the interplanetary transport conditions. Results. All electron events were clearly associated with type III radio bursts. EUV jets were also found in association with all of them except one. A diversity of time profiles and pitch-angle distributions was observed. Different source locations and different magnetic connectivity and transport conditions were likely involved. The July 11 event was also detected by Wind, separated 107 degrees in longitude from Solar Orbiter. For the July 22 event, the Suprathermal Electron and Proton (STEP) sensor of EPD allowed for us to not only resolve multiple electron injections at low energies, but it also provided an exceptionally high pitch-angle resolution of a very anisotropic beam. This, together with radio observations of local Langmuir waves suggest a very good magnetic connection during the July 22 event. This scenario is challenged by a high-frequency occultation of the type III radio burst and a nominally non-direct connection to the source; therefore, magnetic connectivity requires further investigation

Redefining flux ropes in heliophysics

Magnetic flux ropes manifest as twisted bundles of magnetic field lines. They carry significant amounts of solar mass in the heliosphere. This paper underlines the need to advance our understanding of the fundamental physics of heliospheric flux ropes and provides the motivation to significantly improve the status quo of flux rope research through novel and requisite approaches. It briefly discusses the current understanding of flux rope formation and evolution, and summarizes the strategies that have been undertaken to understand the dynamics of heliospheric structures. The challenges and recommendations put forward to address them are expected to broaden the in-depth knowledge of our nearest star, its dynamics, and its role in its region of influence, the heliosphere.Fil: Nieves Chinchilla, Teresa. National Aeronautics and Space Administration; Estados UnidosFil: Pal, Sanchita. George Mason University. School Of Physics. Astronomy And Computational Sciences; Estados Unidos. National Aeronautics and Space Administration; Estados UnidosFil: Salman, Tarik M.. George Mason University. School Of Physics. Astronomy And Computational Sciences; Estados Unidos. National Aeronautics and Space Administration; Estados UnidosFil: Carcaboso, Fernando. Catholic University Of America; Estados Unidos. National Aeronautics and Space Administration; Estados UnidosFil: Guidoni, Silvina E.. American University. College Of Arts & Sciences. Physics Departament.; Estados Unidos. National Aeronautics and Space Administration; Estados UnidosFil: Cremades Fernandez, Maria Hebe. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad de Mendoza. Facultad de Ingenieria; ArgentinaFil: Narock, Ayris. National Aeronautics and Space Administration; Estados UnidosFil: Balmaceda, Laura Antonia. George Mason University. School Of Physics. Astronomy And Computational Sciences; Estados Unidos. National Aeronautics and Space Administration; Estados Unidos. Consejo Nacional de Investigaciones Científicas y Técnicas; ArgentinaFil: Lynch, Benjamin J.. University of California at Berkeley; Estados UnidosFil: Al Haddad, Nada. University Of New Hampshire; Estados UnidosFil: Rodríguez García, Laura. Universidad de Alcalá; EspañaFil: Narock, Thomas W.. Goucher College; Estados UnidosFil: Dos Santos, Luiz F. G.. Shell Global Solutions; Estados UnidosFil: Regnault, Florian. University Of New Hampshire; Estados UnidosFil: Kay, Christina. Catholic University Of America; Estados Unidos. National Aeronautics and Space Administration; Estados UnidosFil: Winslow, Réka M.. University Of New Hampshire; Estados UnidosFil: Palmerio, Erika. Predictive Science Inc.; Estados UnidosFil: Davies, Emma E.. University Of New Hampshire; Estados UnidosFil: Scolini, Camilla. University Of New Hampshire; Estados UnidosFil: Weiss, Andreas J.. National Aeronautics and Space Administration; Estados UnidosFil: Alzate, Nathalia. National Aeronautics and Space Administration; Estados UnidosFil: Jeunon, Mariana. Catholic University Of America; Estados Unidos. National Aeronautics and Space Administration; Estados UnidosFil: Pujadas, Roger. Universidad Politécnica de Catalunya; España. National Aeronautics and Space Administration; Estados Unido