Filament eruption from active region 13283 leading to fast halo-CME and intense geomagnetic storm on 23 April 2023. (arXiv:2312.08790v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Vemareddy_P/0/1/0/all/0/1">P. Vemareddy</a>
Using multi-instrument and multi-wavelength observations, we studied a CME
eruption that led to intense geomagnetic storm on 23 April 2023. The eruption
occurred on April 21 in solar active region 13283 near the disk-center. The AR
was in its decay stage, with fragmented polarities and a pre-existing long
filament channel, a few days before the eruption. The study of magnetic field
evolution suggests that the flux-rope (filament) has been built up by
monotonous helicity accumulation over several days, and further converging and
canceling fluxes lead to helicity injection change, resulting in the unstable
nature of the magnetic flux-rope (MFR) and its further eruption. Importantly,
the CME morphology revealed that the MFR apex underwent a rotation of upto
56degree~in clockwise-direction owing to its positive helicity. The CME
decelerates in the LASCO-FOV and has a plane-of-sky velocity of 1226 km/s at
20,R$_odot$. In the Heliospheric Imager FOV, the CME lateral expansion is
tracked more than the earthward motion. This implies that the arrival time
estimation is difficult to assess. The in-situ arrival of ICME shock was at
07:30 UT on April 23, and a geomagnetic storm commenced at 08:30,UT. The flux
rope fitting to the in-situ magnetic field observations reveals that the MC
flux rope orientation is consistent with its near Sun orientation, which has a
strong negative Bz-component. The analysis of this study indicates that the
near-Sun rotation of the filament during its eruption to the CME is the key to
the negative Bz-component and consequently the intense geomagnetic storm.
Using multi-instrument and multi-wavelength observations, we studied a CME
eruption that led to intense geomagnetic storm on 23 April 2023. The eruption
occurred on April 21 in solar active region 13283 near the disk-center. The AR
was in its decay stage, with fragmented polarities and a pre-existing long
filament channel, a few days before the eruption. The study of magnetic field
evolution suggests that the flux-rope (filament) has been built up by
monotonous helicity accumulation over several days, and further converging and
canceling fluxes lead to helicity injection change, resulting in the unstable
nature of the magnetic flux-rope (MFR) and its further eruption. Importantly,
the CME morphology revealed that the MFR apex underwent a rotation of upto
56degree~in clockwise-direction owing to its positive helicity. The CME
decelerates in the LASCO-FOV and has a plane-of-sky velocity of 1226 km/s at
20,R$_odot$. In the Heliospheric Imager FOV, the CME lateral expansion is
tracked more than the earthward motion. This implies that the arrival time
estimation is difficult to assess. The in-situ arrival of ICME shock was at
07:30 UT on April 23, and a geomagnetic storm commenced at 08:30,UT. The flux
rope fitting to the in-situ magnetic field observations reveals that the MC
flux rope orientation is consistent with its near Sun orientation, which has a
strong negative Bz-component. The analysis of this study indicates that the
near-Sun rotation of the filament during its eruption to the CME is the key to
the negative Bz-component and consequently the intense geomagnetic storm.
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