Macroscopic velocity fields have been studied in a solar prominence. The spectra and monochromatic images were analysed, and the existence of a contracting motion, possibly due to a pinch effect, is discussed. A helical shape of the prominence is proposed. The paper in full will be published in Solar PhysicsAsociación Argentina de Astronomí

Grossi-Gallegos, H

Machado, M.E..

English

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ASTRONOMIA SOLARCOMUNICACIONESMacroscopic motions in prominences I, the prominence of 26th march, 1971M. E. Machado y H. Grossi GallegosObservatorio Nacional de Física Cósmica, San MiguelAbstract: Macroscopic velocity fields have been studied in a solar prominence. The spectra and monochromatic images were analy- sed, and the existence of a contracting motion, possibly due to a pinch effect, is discussed. A helical shape of the prominence is proposed. The papel in full will be published in Solar Physics.Analysis of two active prominencesM. E. MachadoObservatorio Nacional de Física Cósmica, San MiguelAbstract: We discuss the observations of two eruptive prominences, and the formation of condensations during the phenomena. The density and intensity varia tions of the condensations are analyzed spectroscopically in one of the events. Some hypotheses about the magnetic field configuration have been used in order to explain the observational data. The paper in full will be published in Solar Physics.The loop prominence of may 13, 1971 and its associated effectsM. E. Machado, H. Grossi Gallegos y A. F. SilvaObservatorio Nacional de Física Cósmica, San MiguelAbstract: A study is presented about the formation of a loop pro­minence system (LPS) on May 13, 1971. The development of the phenomenon in found the follow the model of Jefferies and Orrall, and was assooiated with small radio bursts and severa) kind SID. From the spectral analysis a temperature of 13200 K has been deduced and a density of hydrogen atoms n (H) = 1010 cnr8 estimated. The existence of inclined emissions probably pro- duced by rotatory motions is discussed. From the radio-data ana­lysis it was inferred that an impulsive and a thermal component were present, the length of the emitting plasma cloud was found to be about 56000 Km. The LPS appeared, in accordance to previous results, in a región producing proton fiares. The paper in full will be published in Solar Physics.INFORME DE TRABAJOCorrelación de las mediciones de flujo diario solar, en 73,5 cm. con otros eventos solares *R. J. MarabiniObservatorio Astronómico, La PlataAbstract: Solar radio burst on 408 MHz are not complete correla- ted, with burst on other frecuencies, it gives the possibility of di- ferent origen.GeneralidadesDe enero a octubre de 1968 se observó diariamente el Sol, mediante un radiotelescopio del Observatorio de La Plata, cuya antena tiene 6,6 m de diámetro.Eliminando, las componentes de Sol quieto y lentamen­te variable, se observaren 696 “bursts” de distintas dura­ciones e intensidades.Para estudiar como las perturbaciones de la cromos­fera y corona producen estos “bursts’, se correlacionaron en el tiempo, con los distintos eventos en H a y en radio; para ello se tomaron los datos publicados exv^Solar Gheo- phisical Data” y los “Quarterly Bulletin on Solar Activity” de la I.A.U. Se tomaron los comienzos en tiempo de cada “bursts” en 408 MHz contra los comienzos en tiempo de los otros eventos.Tipos IIILa figura 1 muestra los eventos cuyos comienzos estaban dentro de un valor absoluto menor o igual que .6 minuto, se adoptó este margen para evitar la dispersión de los datos de las publicaciones, las fechas de ocurrencia de cada uno y las frecuencias. El eje de alturas es sólo para dar la mínima altura a la cual la radiación puede escapar, la cual es mayor en las zonas activas. Las veloci­dades que se obtienen son del orden .le a .6c, para los chorres de electrones que excitan la generación por osci- lacions del plasma. Se cumple que los tipos 111 pueden aparecer con fiares en H a o no.* Trabajo realizado bajo subsidio de CONICET.Rol. N9 17 - Asoc. Arg. de Astr. 17

Macroscopic motions in prominences I, the prominence of 26th March, 1971

http://sedici.unlp.edu.ar/bitstream/handle/10915/98719/Resumen__1_p._.pdf?sequence=1

Macroscopic motions in prominences I, the prominence of 26th March, 1971

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