MEASURING AN ERUPTIVE PROMINENCE AT LARGE DISTANCES FROM THE SUN. I. IONIZATION AND EARLY EVOLUTION

2015 ◽  
Vol 806 (2) ◽  
pp. 175 ◽  
Author(s):  
T. A. Howard
Keyword(s):  
Early Evolution ◽  
The Sun ◽  
Eruptive Prominence

 Statistical study of CMEs, lateral overexpansion and SEP events

2021 ◽  
Author(s):  
Alexandros Adamis ◽  
Astrid Veronig ◽  
Tatiana Podladchikova ◽  
Karin Dissauer ◽  
Rositsa Miteva ◽  
...  
Keyword(s):  
Statistical Study ◽  
Solar Energetic Particle ◽  
Early Evolution ◽  
Point Of View ◽  
Time Range ◽  
The Sun ◽  
Lateral Expansion ◽  
Time Profiles ◽  
Angular Expansion

<p><strong>We present a statistical study on the early evolution of coronal mass ejections (CMEs), to better understand the effect of CME (over)- expansion and how it relates to the production of Solar Energetic Particle (SEP) events. We study the kinematic CME characteristics in terms of their radial and lateral expansion, from their early evolution in the Sun’s atmosphere as observed in EUV imagers and coronagraphs. The data covers 72 CMEs that occurred in the time range of July 2010 to September 2012, where the twin STEREO spacecraft where in quasiquadrature </strong><strong>to the Sun-Earth line. From the STEREO point-of-view, the CMEs under study were observed close to the limb. We calculated the radial and lateral height (width) versus time profiles and derived the corresponding peak and mean velocities, accelerations, and angular expansion rates, with particular emphasis on the role of potential lateral overexpansion in the early CME evolution. We find high correlations between the radial and lateral CME velocities and accelerations. CMEs that are associated tend to be located at the high-value end of the distributions of velocities, widths, and expansion rates compared to nonSEP associated events.<br></strong></p>

The early evolution of the sun

Icarus ◽  
1962 ◽  
Vol 1 (1-6) ◽  
pp. 422-441 ◽  
Author(s):  
Dilhan Ezer ◽  
G.W. Cameron
Keyword(s):  
Early Evolution ◽  
The Sun

scholarly journals The early evolution of Jupiter in the tidal field of the Sun

1982 ◽  
Vol 198 (4) ◽  
pp. 961-973 ◽  
Author(s):  
N. Schofield ◽  
M. M. Woolfson
Keyword(s):  
Early Evolution ◽  
The Sun

scholarly journals Launch of a CME-associated eruptive prominence as observed with IRIS and ancillary instruments

2019 ◽  
Vol 624 ◽  
pp. A72 ◽  
Author(s):  
P. Zhang ◽  
É. Buchlin ◽  
J.-C. Vial
Keyword(s):  
Total Mass ◽  
Observation Time ◽  
The Sun ◽  
Ionization Degree ◽  
Eruptive Prominence ◽  
Physical Conditions ◽  
Optical Flow Method ◽  
Order Of Magnitude ◽  
The Masses ◽  
Hydrogen Mass

Aims. In this paper we focus on the possible observational signatures of the processes which have been put forward for explaining eruptive prominences. We also try to understand the variations in the physical conditions of eruptive prominences and estimate the masses leaving the Sun versus the masses returning to the Sun during eruptive prominences. Methods. As far as velocities are concerned, we combined an optical flow method on the Atmospheric Imaging Assembly (AIA) 304 Å and Interface Region Imaging Spectrograph (IRIS). Mg II h&k observations in order to derive the plane-of-sky velocities in the prominence, and a Doppler technique on the IRIS Mg II h&k profiles to compute the line-of-sight velocities. As far as densities are concerned, we compared the absolute observed intensities with values derived from non-local thermodynamic equilibrium radiative transfer computations to derive the total (hydrogen) density and consequently compute the mass flows. Results. The derived electron densities range from 1.3 × 109 to 6.0 × 1010 cm−3 and the derived total hydrogen densities range from 1.5 × 109 to 2.4 × 1011 cm−3 in different regions of the prominence. The mean temperature is around 1.1 × 104 K, which is higher than in quiescent prominences. The ionization degree is in the range of 0.1–10. The total (hydrogen) mass is in the range of 1.3 × 1014–3.2 × 1014 g. The total mass drainage from the prominence to the solar surface during the whole observation time of IRIS is about one order of magnitude smaller than the total mass of the prominence.

Estimates of the Magnetic Energy Densities of two Eruptive Prominences from Their Close Association with Moving Type IV Radio Bursts

1979 ◽  
Vol 44 ◽  
pp. 315-320 ◽  
Author(s):  
R.T. Stewart ◽  
R.T. Hansen ◽  
K.V. Sheridan
Keyword(s):  
Magnetic Energy ◽  
Close Association ◽  
Private Communication ◽  
The Sun ◽  
Radio Bursts ◽  
Eruptive Prominence ◽  
X Ray ◽  
Type Iv ◽  
Long Duration ◽  
East Limb

During 1977 October 3-5 two eruptive-prominence and moving-type-IV radio events occurred above the east limb of the Sun when the active region McMath No. 14979 was ≈20° and ≈7° behind the east limb. No flares or microwave events were reported but long-duration soft X-ray events were recorded by OSO-8 and SMS-2 in the 1-8 Å range (Lemen, Wolfson and Grubbe, private communication).

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