Observational Interpretation of an Active Prominence on 1999 May 1

2001 ◽  
Vol 549 (2) ◽  
pp. 1221-1230 ◽  
Author(s):  
Holly R. Gilbert ◽  
Thomas E. Holzer ◽  
B. C. Low ◽  
Joan T. Burkepile
Keyword(s):  
Active Prominence

scholarly journals Observations of the Association of Prominences and the Surrounding Corona

1998 ◽  
Vol 167 ◽  
pp. 37-40
Author(s):  
Raymond N. Smartt ◽  
Zhenda Zhang ◽  
Vladimir S. Airapetian ◽  
Ira S. Kim
Keyword(s):  
High Temperature ◽  
Emission Line ◽  
Magnetic Reconnection ◽  
Coronal Loop ◽  
Observational Evidence ◽  
Coronal Emission ◽  
Flare Loop ◽  
Active Prominence ◽  
Coronal Region

AbstractEmission-line coronal images in Fe XIV (530.3 nm) and FeX (637.5 nm) show faint enhancements at the location of quiescent prominences. Such enhancements can appear in the outer portions of a prominence, similar to the high-temperature sheath surrounding prominences as inferred from UV and EUV observations. The observational evidence supports the interpretation that this enhanced coronal emission is due to energy carried by the prominence threads and dissipated in the adjacent coronal region. Also, observed coronal loop interactions involving partial magnetic reconnection have associated Hα structures. These structures can have the appearance of an active prominence, similar to those typically observed in post flare loop systems. It appears that the association of such active prominences with the adjacent corona is fundamentally different from that of quiescent prominences. The observations indicate that these types of active prominences arise simply as a consequence of reconnection processes in the corona itself.

scholarly journals Application of Soft Computing (ANN) Techniques to study the relationship between Solar Activity Features and Total Column Ozone

2019 ◽  
Vol 14 (1) ◽  
Author(s):  
Seema Pande ◽  
Mahesh Chandra Mathpal ◽  
Bimal Pande
Keyword(s):  
Neural Network ◽  
Artificial Neural Network ◽  
Solar Activity ◽  
Solar Flares ◽  
Total Column Ozone ◽  
Active Prominence ◽  
Artificial Neural Network Ann ◽  
Column Ozone ◽  
The Relationship ◽  
Total Column

Using 30 years data (1986-2015) we have made an attempt to study the dependency of total column ozone (TCO) on solar activity features: solar flares (SF), solar active prominence (SAP) and sunspot numbers (SN) for two hill stations of Uttarakhand viz. Nainital (29.40 N.79.470E) and Mussorie (30.270 N 78.060 E) by Artificial neural network (ANN) technique. Our study supports the fact that solar activity features contribute to the production of ozone.

Active Prominences

1979 ◽  
Vol 44 ◽  
pp. 214-225 ◽  
Author(s):  
J. McKim Malville
Keyword(s):  
Magnetic Fields ◽  
High Energy ◽  
Low Energy ◽  
Necessary And Sufficient Condition ◽  
Quiescent Prominence ◽  
Internal Motions ◽  
Active Prominence ◽  
Necessary And Sufficient ◽  
Energy Side

Those prominences which are identified as active lie near the middle of a large group of objects found in the low corona bordered on the high energy side by flares and on the low energy side by quiescent prominences. Known by descriptive terms such as eruptive, surge, spray, tornado, and loop, active prominences typically have shorter lifetimes, broader line widths, larger internal motions, and stronger internal magnetic fields than quiescent prominences (Tandberg-Hanssen, 1974). When dealing with specific examples, however, it is often difficult to establish a necessary and sufficient condition for classification of such an object as an active prominence. The ambiguity at the low energy end involves “hybrid” objects which possess features of both quiescent and active prominences. For example, the active region filament may have a lifetime of several days, have large internal motions and relatively strong magnetic fields. The stable hedgerow quiescent prominence may contain small regions with large widths and large velocities. On the average, a quiescent will typically erupt every five to eight days, (Serio, et al., 1978; Bryson and Malville, 1978) and at those times a prominence is transformed from the quiescent to the active state. For these objects something other than morphology, velocity fields, or even magnetic fields is necessary to specify their condition; something less symptomatic and more fundamental is required. That necessary parameter may be, I shall suggest, the total current, J, flowing in the structure.

Oscillatory motions in an active prominence

Solar Physics ◽  
1990 ◽  
Vol 127 (1) ◽  
pp. 119-128 ◽  
Author(s):  
B. Vršnak ◽  
V. Ruždjak ◽  
R. Brajša ◽  
F. Zloch
Keyword(s):  
Active Prominence
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