eprintid: 10136
rev_number: 55
eprint_status: archive
userid: 599
dir: disk0/00/01/01/36
datestamp: 2008-09-10 13:43:30
lastmod: 2021-10-19 22:08:12
status_changed: 2008-09-10 13:43:30
type: article
metadata_visibility: show
item_issues_count: 0
creators_name: Goff, CP
creators_name: van Driel-Gesztelyi, L
creators_name: Harra, LK
creators_name: Matthews, SA
creators_name: Mandrini, CH
title: A slow coronal mass ejection with rising X-ray source
subjects: 11200
divisions: UCL
divisions: B04
divisions: C06
divisions: F63
keywords: Sun : X-ray : gamma rays, Sun : flares, Sun : magnetic fields, Sun : coronal mass ejections (CMEs), Sun : corona, Sun : atmosphere, KINK INSTABILITY, MAGNETIC LOOP, SOLAR-FLARE, RHESSI, SPECTROMETER, TELESCOPE, IMAGER
abstract: An eruptive event, which occurred on 16th April 2002, is discussed. Using images from the Transition Region and Coronal Explorer ( TRACE) at 195 angstrom, we observe a lifting flux rope which gives rise to a slow coronal mass ejection ( CME). There are supporting velocity observations from the Coronal Diagnostic Spectrometer ( CDS) on the Solar and Heliospheric Observatory ( SOHO), which illustrate the helical nature of the structure. Additionally a rising coronal hard X- ray source, which is observed with the Reuven Ramaty High Energy Solar Spectroscopic Imager ( RHESSI), is shown to follow the flux rope with a speed of similar to 60 km s(-1). It is also sampled by the CDS slit, although it has no signature in the Fe XIX band. Following the passage of this source, there is evidence from the CDS for down- flowing ( cooling) material along newly reconnected loops through Doppler velocity observations, combined with magnetic field modeling. Later, a slow CME is observed with the Large Angle and Spectroscopic Coronagraph ( LASCO). We combine a height- time profile of the flux rope at lower altitudes with the slow CME. The rising flux rope speeds up by a factor of 1.7 at the start of the impulsive energy release and goes through further acceleration before reaching 1.5 solar radii. These observations support classical CME scenarios in which the eruption of a filament precedes flaring activity. Cusped flare loops are observed following the erupting flux rope and their altitude increases with time. In addition we find RHESSI sources both below and above the probable location of the reconnection region.
date: 2005-05
publisher: E D P SCIENCES
vfaculties: VMPS
rae2008: 19
oa_status: green
primo: open
primo_central: open_green
article_type_text: Article
verified: verified_batch
elements_source: Web of Science
elements_id: 64701
doi: 10.1051/0004-6361:20042321
lyricists_name: Harra, Louise
lyricists_name: Matthews, Sarah
lyricists_name: Van Driel-Gesztelyi, Lidia
lyricists_id: LKHAR43
lyricists_id: SAMAT57
lyricists_id: LVAND77
full_text_status: public
publication: ASTRON ASTROPHYS
volume: 434
number: 2
pagerange: 761 - 771
refereed: TRUE
issn: 0004-6361
citation:        Goff, CP;    van Driel-Gesztelyi, L;    Harra, LK;    Matthews, SA;    Mandrini, CH;      (2005)    A slow coronal mass ejection with rising X-ray source.                   ASTRON ASTROPHYS , 434  (2)   761 - 771.    10.1051/0004-6361:20042321 <https://doi.org/10.1051/0004-6361%3A20042321>.       Green open access   
 
document_url: https://discovery.ucl.ac.uk/id/eprint/10136/1/10136.pdf