THEMIS, BBSO, MDI and TRACE observations of a filament eruption

L. Contarino, P. Romano, Vasyl Yurchyshyn, F. Zuccarello

Research output: Contribution to journalArticle

18 Citations (Scopus)

Abstract

We describe a filament destabilization which occurred on 5 May 2001 in NOAA AR 9445, before a flare event. The analysis is based on Hα data acquired by THEMIS operating in IPM mode, Hα data and magnetograms obtained at the Big Bear Solar Observatory, MDI magnetograms and 171 Å images taken by TRACE. Observations at 171 Å show that ∼ 2.5 hours before the flare peak, the western part of the EUY filament channel seems to split into two parts. The bifurcation of the filament in the Hα line is observed to take place ∼ 1.5 hours before the flare peak, while one thread of the filament erupts ∼10 min before the peak of the flare. Our analysis of longitudinal magnetograms shows the presence of a knot of positive flux inside a region of negative polarity, which coincides with the site of filament bifurcation. We interpret this event as occurring in two steps: the first step, characterized by the appearance of a new magnetic feature and the successive reconnection in the lower atmosphere between its field lines and the field lines of the old arcade sustaining the filament, leads to a new filament channel and to the observed filament bifurcation; the second step, characterized by the eruption of part of the filament lying on the old PIL, leads to a second reconnection, occurring higher in the corona.

Original languageEnglish (US)
Pages (from-to)173-188
Number of pages16
JournalSolar Physics
Volume216
Issue number1-2
DOIs
StatePublished - Sep 1 2003

Fingerprint

bifurcation
volcanic eruptions
filaments
volcanic eruption
flares
magnetic signatures
bear
corona
observatory
atmosphere
H lines
solar observatories
lower atmosphere
sustaining
threads
destabilization
bears
coronas
analysis
polarity

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Contarino, L., Romano, P., Yurchyshyn, V., & Zuccarello, F. (2003). THEMIS, BBSO, MDI and TRACE observations of a filament eruption. Solar Physics, 216(1-2), 173-188. https://doi.org/10.1023/A:1026107727149
Contarino, L. ; Romano, P. ; Yurchyshyn, Vasyl ; Zuccarello, F. / THEMIS, BBSO, MDI and TRACE observations of a filament eruption. In: Solar Physics. 2003 ; Vol. 216, No. 1-2. pp. 173-188.
@article{fb193165101a4f7b871617e8d53be9da,
title = "THEMIS, BBSO, MDI and TRACE observations of a filament eruption",
abstract = "We describe a filament destabilization which occurred on 5 May 2001 in NOAA AR 9445, before a flare event. The analysis is based on Hα data acquired by THEMIS operating in IPM mode, Hα data and magnetograms obtained at the Big Bear Solar Observatory, MDI magnetograms and 171 {\AA} images taken by TRACE. Observations at 171 {\AA} show that ∼ 2.5 hours before the flare peak, the western part of the EUY filament channel seems to split into two parts. The bifurcation of the filament in the Hα line is observed to take place ∼ 1.5 hours before the flare peak, while one thread of the filament erupts ∼10 min before the peak of the flare. Our analysis of longitudinal magnetograms shows the presence of a knot of positive flux inside a region of negative polarity, which coincides with the site of filament bifurcation. We interpret this event as occurring in two steps: the first step, characterized by the appearance of a new magnetic feature and the successive reconnection in the lower atmosphere between its field lines and the field lines of the old arcade sustaining the filament, leads to a new filament channel and to the observed filament bifurcation; the second step, characterized by the eruption of part of the filament lying on the old PIL, leads to a second reconnection, occurring higher in the corona.",
author = "L. Contarino and P. Romano and Vasyl Yurchyshyn and F. Zuccarello",
year = "2003",
month = "9",
day = "1",
doi = "https://doi.org/10.1023/A:1026107727149",
language = "English (US)",
volume = "216",
pages = "173--188",
journal = "Solar Physics",
issn = "0038-0938",
publisher = "Springer Netherlands",
number = "1-2",

}

Contarino, L, Romano, P, Yurchyshyn, V & Zuccarello, F 2003, 'THEMIS, BBSO, MDI and TRACE observations of a filament eruption', Solar Physics, vol. 216, no. 1-2, pp. 173-188. https://doi.org/10.1023/A:1026107727149

THEMIS, BBSO, MDI and TRACE observations of a filament eruption. / Contarino, L.; Romano, P.; Yurchyshyn, Vasyl; Zuccarello, F.

In: Solar Physics, Vol. 216, No. 1-2, 01.09.2003, p. 173-188.

Research output: Contribution to journalArticle

TY - JOUR

T1 - THEMIS, BBSO, MDI and TRACE observations of a filament eruption

AU - Contarino, L.

AU - Romano, P.

AU - Yurchyshyn, Vasyl

AU - Zuccarello, F.

PY - 2003/9/1

Y1 - 2003/9/1

N2 - We describe a filament destabilization which occurred on 5 May 2001 in NOAA AR 9445, before a flare event. The analysis is based on Hα data acquired by THEMIS operating in IPM mode, Hα data and magnetograms obtained at the Big Bear Solar Observatory, MDI magnetograms and 171 Å images taken by TRACE. Observations at 171 Å show that ∼ 2.5 hours before the flare peak, the western part of the EUY filament channel seems to split into two parts. The bifurcation of the filament in the Hα line is observed to take place ∼ 1.5 hours before the flare peak, while one thread of the filament erupts ∼10 min before the peak of the flare. Our analysis of longitudinal magnetograms shows the presence of a knot of positive flux inside a region of negative polarity, which coincides with the site of filament bifurcation. We interpret this event as occurring in two steps: the first step, characterized by the appearance of a new magnetic feature and the successive reconnection in the lower atmosphere between its field lines and the field lines of the old arcade sustaining the filament, leads to a new filament channel and to the observed filament bifurcation; the second step, characterized by the eruption of part of the filament lying on the old PIL, leads to a second reconnection, occurring higher in the corona.

AB - We describe a filament destabilization which occurred on 5 May 2001 in NOAA AR 9445, before a flare event. The analysis is based on Hα data acquired by THEMIS operating in IPM mode, Hα data and magnetograms obtained at the Big Bear Solar Observatory, MDI magnetograms and 171 Å images taken by TRACE. Observations at 171 Å show that ∼ 2.5 hours before the flare peak, the western part of the EUY filament channel seems to split into two parts. The bifurcation of the filament in the Hα line is observed to take place ∼ 1.5 hours before the flare peak, while one thread of the filament erupts ∼10 min before the peak of the flare. Our analysis of longitudinal magnetograms shows the presence of a knot of positive flux inside a region of negative polarity, which coincides with the site of filament bifurcation. We interpret this event as occurring in two steps: the first step, characterized by the appearance of a new magnetic feature and the successive reconnection in the lower atmosphere between its field lines and the field lines of the old arcade sustaining the filament, leads to a new filament channel and to the observed filament bifurcation; the second step, characterized by the eruption of part of the filament lying on the old PIL, leads to a second reconnection, occurring higher in the corona.

UR - http://www.scopus.com/inward/record.url?scp=0347753415&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=0347753415&partnerID=8YFLogxK

U2 - https://doi.org/10.1023/A:1026107727149

DO - https://doi.org/10.1023/A:1026107727149

M3 - Article

VL - 216

SP - 173

EP - 188

JO - Solar Physics

JF - Solar Physics

SN - 0038-0938

IS - 1-2

ER -

Contarino L, Romano P, Yurchyshyn V, Zuccarello F. THEMIS, BBSO, MDI and TRACE observations of a filament eruption. Solar Physics. 2003 Sep 1;216(1-2):173-188. https://doi.org/10.1023/A:1026107727149