NEW VACUUM SOLAR TELESCOPE OBSERVATIONS OF A FLUX ROPE TRACKED BY A FILAMENT ACTIVATION

AbstractBased on the New Vacuum Solar Telescope observations, some new results about the solar activities are obtained. (1) In the Hα line, a flux rope tracked by filament activation is detected for the first time. There may exist some mild heating during the filament activation. (2) The direct observations illustrate the mechanism of confined flares, i.e., the flares are triggered by magnetic reconnection between the emerging loops and the pre-existing loops and prevented from being eruptive by the overlying loops. (3) The solid observational evidence of magnetic reconnection between two sets of small-scale loops is reported. The successive slow reconnection changes the conditions around the reconnection area and leads to the rapid reconnection. (4) An ensemble of oscillating bright features rooted in a light bridge is observed and given a new name, light wall. The light wall oscillations may be due to the leakage of p-modes from below the photosphere.

Download Full-text

Causal relationships between eruptive prominences and coronal mass ejections

Annales Geophysicae ◽

10.5194/angeo-26-3025-2008 ◽

2008 ◽

Vol 26 (10) ◽

pp. 3025-3031 ◽

Cited By ~ 23

Author(s):

B. Filippov ◽

S. Koutchmy

Keyword(s):

Magnetic Flux ◽

Coronal Mass Ejections ◽

Close Association ◽

Flux Rope ◽

Critical Values ◽

General Question ◽

Magnetic Flux Rope ◽

Filament Activation ◽

Field Lines ◽

The Disappeared

Abstract. A close association between eruptive prominences and CMEs, both slow and fast CMEs, was reported in many studies. Sometimes it was possible to follow the material motion starting from the prominence (filament) activation to the CME in the high corona. Remnants of the prominence were found in the bright core of the CME. However, detailed comparisons of the two phenomena reveal problems in explaining CMEs as a continuation of filament eruptions in the upper corona. For example, the heliolatitudes of the disappeared filaments and subsequent coronal ejections sometimes differ by tens of degrees. In order to clear up the problems appearing when considering this association EP-CME, we tentatively analyse the more general question of the dynamics of the generic magnetic flux rope. Prominences and filaments are the best tracers of the flux ropes in the corona long before the beginning of the eruption. A twisted flux rope is held by the tension of field lines of photospheric sources until parameters of the system reach critical values and a catastrophe happens. We suggest that the associated flux rope height above the photosphere is one of these parameters and that it is revealed by the measured height of the filament. 80 filaments were analysed and we found that eruptive prominences were near the so-called limit of stability a few days before their eruptions. We suggest that a comparison of actual heights of prominences with the calculated critical heights from magnetograms could be systematically used to predict filament eruptions and the corresponding CMEs.

Download Full-text

Introduction to the Solar Space Telescope

International Astronomical Union Colloquium ◽

10.1017/s025292110006437x ◽

2000 ◽

Vol 179 ◽

pp. 141-147

Author(s):

G. Ai ◽

S. Jin ◽

S. Wang ◽

B. Ye ◽

S. Yang

Keyword(s):

Solar Telescope ◽

Basic Aspect ◽

Space Telescope ◽

Space Solar Telescope

AbstractThe design of the space solar telescope (SST) (phase B) has been completed. The manufacturing is under development. At the end of 2000, it will be assembled. The basic aspect will be introduced in this paper.

Download Full-text

Prominences and Solar Activity

International Astronomical Union Colloquium ◽

10.1017/s0252921100065817 ◽

1979 ◽

Vol 44 ◽

pp. 357-372

Author(s):

Z. Švestka

Keyword(s):

Solar Activity ◽

Solar Cycle ◽

List Type ◽

Type Number ◽

Flare Loops ◽

Filament Activation

The following subjects were discussed:(1)Filament activation(2)Post-flare loops.(3)Surges and sprays.(4)Coronal transients.(5)Disk vs. limb observations.(6)Solar cycle variations of prominence occurrence.(7)Active prominences patrol service.Of all these items, (1) and (2) were discussed in most detail and we also pay most attention to them in this report. Items (3) and (4) did not bring anything new when compared with the earlier invited presentations given by RUST and ZIRIN and therefore, we omit them.

Download Full-text

World’s most powerful solar telescope is up and running

Nature ◽

10.1038/d41586-020-00224-z ◽

2020 ◽

Author(s):

Alexandra Witze

Keyword(s):

Solar Telescope

Download Full-text

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

JOURNAL OF ADVANCES IN PHYSICS ◽

10.24297/jap.v4i2.6965 ◽

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.

Download Full-text