The sources of material comprising a mass ejection coronal transient

Solar Physics ◽  
1975 ◽  
Vol 45 (2) ◽  
pp. 363-376 ◽  
Author(s):  
E. Hildner ◽  
J. T. Gosling ◽  
R. T. Hansen ◽  
J. D. Bohlin
Keyword(s):  
Coronal Transient ◽  
Mass Ejection

scholarly journals The Disruption of EUV Coronal Loops Following a Mass Ejection Transient

1980 ◽  
Vol 91 ◽  
pp. 241-244
Author(s):  
E. J. Schmahl
Keyword(s):  
White Light ◽  
Coronal Loops ◽  
X Rays ◽  
Transient Event ◽  
Mass Outflow ◽  
Coronal Transient ◽  
Loop Prominence ◽  
Mass Ejection

A classic filament disruption/coronal transient event ocurred on 10 January 1974. After the prominence liftoff, “gradual” x-rays were recorded by Solrad 9. A white light coronal ejection, interpreted as a loop seen edge-on, followed. During the mass outflow, Hα loops formed at the original site of the prominence. The loops appeared also in EUV spectroheliograms, and rose rapidly before vanishing abruptly. During the disintegration of the loops the apices showed great enhancements and vertical spike structures. The overall behavior of this loop prominence system is compatible with reconnection models.

scholarly journals The Cross Sectional Magnetic Profile of a Coronal Transient

1980 ◽  
Vol 91 ◽  
pp. 475-481
Author(s):  
M. K. Bird ◽  
H. Volland ◽  
B. L. Seidel ◽  
C. T. Stelzried
Keyword(s):  
Magnetic Field ◽  
Substantial Improvement ◽  
Cross Sectional ◽  
Linearly Polarized ◽  
Coronal Event ◽  
Coronal Transient ◽  
Magnetic Profile ◽  
Mass Ejection ◽  
The Magnetic Field

The role of the magnetic field in a coronal mass ejection event has not been unequivocally defined, and may in fact be quite variable in view of the large variety of shapes and sizes of coronal transients. Measurements of the magnetic field associated with these events have thus far been inferred from simultaneously observed radio bursts, which provide no information on the direction of the field and are limited in spatial resolution. Substantial improvement in these two areas could be achieved by continuous monitoring of the Faraday rotation of a linearly polarized spacecraft signal during solar occultation. A coronal event traversing the line-of-sight would yield a characteristic profile in cross section, which would be of value for discriminating between the various models of coronal transients.

Type II Solar Radio Bursts over Solar Cycle 21

1994 ◽  
Vol 144 ◽  
pp. 283-284
Author(s):  
G. Maris ◽  
E. Tifrea
Keyword(s):  
Solar Radio ◽  
Interplanetary Space ◽  
Impulsive Phase ◽  
Radio Bursts ◽  
Type Ii ◽  
Solar Radio Bursts ◽  
Strong Energy ◽  
Mass Ejection ◽  
Geophysical Effect ◽  
Radio Event

The type II solar radio bursts produced by a shock wave passing through the solar corona are one of the most frequently studied solar activity phenomena. The scientific interest in this type of phenomenon is due to the fact that the presence of this radio event in a solar flare is an almost certain indicator of a future geophysical effect. The origin of the shock waves which produce these bursts is not at all simple; besides the shocks which are generated as a result of a strong energy release during the impulsive phase of a flare, there are also the shocks generated by a coronal mass ejection or the shocks which appear in the interplanetary space due to the supplementary acceleration of the solar particles.

Observations for the Role of Flux rope Eruption in a Geoeffective Solar Flare

2014 ◽  
Vol 4 (2) ◽  
pp. 555-564
Author(s):  
A.M Aslam
Keyword(s):  
Solar Flare ◽  
Flux Rope ◽  
Magnetic Configuration ◽  
Solar Dynamics Observatory ◽  
Multi Wavelength ◽  
Solar Dynamics ◽  
Halo Coronal Mass Ejection ◽  
Mass Ejection ◽  
The Waves

On September 24, 2011 a solar flare of M 7.1 class was released from the Sun. The flare was observed by most of the space and ground based observatories in various wavebands. We have carried out a study of this flare to understand its causes on Sun and impact on earth. The flare was released from NOAA active region AR 11302 at 12:33 UT. Although the region had already produced many M class flares and one X- class flare before this flare, the magnetic configuration was not relaxed and still continued to evolve as seen from HMI observations. From the Solar Dynamics Observatory (SDO) multi-wavelength (131 Ã…, 171 Ã…, 304 Ã… and 1600Ã…) observations we identified that a rapidly rising flux rope triggered the flare although HMI observations revealed that magnetic configuration did not undergo a much pronounced change. The flare was associated with a halo Coronal Mass Ejection (CME) as recorded by LASCO/SOHO Observations. The flare associated CME was effective in causing an intense geomagnetic storm with minimum Dst index -103 nT. A radio burst of type II was also recorded by the WAVES/WIND. In the present study attempt is made to study the nature of coupling between solar transients and geospace.

The Solar Mass Ejection Imager (SMEI) Mission

2004 ◽  
Author(s):  
Bernard V. Jackson ◽  
Andrew Buffington ◽  
P. P. Hick
Keyword(s):  
Solar Mass ◽  
Solar Mass Ejection Imager ◽  
Mass Ejection

scholarly journals The Observational Evidence for Accretion

1997 ◽  
Vol 182 ◽  
pp. 391-405 ◽  
Author(s):  
Lee Hartmann
Keyword(s):  
Large Range ◽  
Observational Evidence ◽  
Young Stars ◽  
Young Stellar Objects ◽  
Stellar Objects ◽  
T Tauri ◽  
Accretion Rates ◽  
Low Mass ◽  
Stellar Magnetospheres ◽  
Mass Ejection

Outflows from low-mass young stellar objects are thought to draw upon the energy released by accretion onto T Tauri stars. I briefly summarize the evidence for this accretion and outline present estimates of mass accretion rates. Young stars show a very large range of accretion rates, and this has important implications for both mass ejection and for the structure of stellar magnetospheres which may truncate T Tauri disks.

EVIDENCE FOR INTERNAL TETHER-CUTTING IN A FLARE/CORONAL MASS EJECTION OBSERVED BYMESSENGER,RHESSI, ANDSTEREO

2010 ◽  
Vol 721 (2) ◽  
pp. 1579-1584 ◽  
Author(s):  
Claire L. Raftery ◽  
Peter T. Gallagher ◽  
R. T. James McAteer ◽  
Chia-Hsien Lin ◽  
Gareth Delahunt
Keyword(s):  
Coronal Mass Ejection ◽  
Mass Ejection

Flux Rope Model of the 2003 October 28–30 Coronal Mass Ejection and Interplanetary Coronal Mass Ejection

2006 ◽  
Vol 642 (1) ◽  
pp. 541-553 ◽  
Author(s):  
J. Krall ◽  
V. B. Yurchyshyn ◽  
S. Slinker ◽  
R. M. Skoug ◽  
J. Chen
Keyword(s):  
Coronal Mass Ejection ◽  
Flux Rope ◽  
Interplanetary Coronal Mass Ejection ◽  
Mass Ejection
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