Solar signatures and eruption mechanism of the August 14, 2010 coronal mass ejection (CME)

D’Huys, Elke; Seaton, Daniel B.; Groof, A. De; Berghmans, D.; Poedts, Stefaan

doi:10.1051/swsc/2017006

Cited by 16 publications

(15 citation statements)

References 47 publications

(64 reference statements)

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“…There are occasional observations up to 2R ⊙ with regular EUV telescopes that operated in dedicated long-exposure regimes, e.g. TESIS/CORONAS-PHOTON (Kuzin et al 2011;Reva et al 2014) or SWAP/PROBA-2 (Berghmans et al 2006;Seaton et al 2013;D'Huys et al 2017), or up to 2.5R ⊙ with specialized EUV coronagraphs, e.g. SPIRIT/CORONAS-F (Zhitnik et al 2003;Slemzin et al 2008).…”

Section: Introductionmentioning

confidence: 99%

Influence of misalignments on the performance of externally occulted solar coronagraphs

Shestov

Zhukov

2018

A&A

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Context. ASPIICS is a novel externally occulted coronagraph that will be launched onboard the PROBA-3 mission of the European Space Agency. The external occulter will be placed on one satellite ∼ 150 m ahead of the second satellite that will carry an optical instrument. During 6 hours out of 19.38 hours of orbit, the satellites will fly in a precise (accuracy around a few millimetres) formation, constituting a giant externally occulted coronagraph. Large distance between the external occulter and the primary objective will allow observations of the white-light solar corona starting from extremely low heights ∼ 1.1R ⊙ . Aims. To analyze influence of shifts of the satellites and misalignments of optical elements on the ASPIICS performance in terms of diffracted light. Based on the quantitative influence of misalignments on diffracted light, we will provide a "recipe" for choosing the size of the internal occulter (IO) to achieve a trade-off between the minimal height of observations and sustainability to possible misalignments. Methods. We consider different types of misalignments and analyze their influence from optical and computational points of view. We implement a numerical model of the diffracted light and its propagation through the optical system, and compute intensities of diffracted light throughout the instrument. Our numerical model is based on the model of Rougeot et al. (2017), who considered the axi-symmetrical case. Here we extend the model to include non-symmetrical cases and possible misalignments. Results. The numerical computations fully confirm main properties of the diffracted light that we obtained from semi-analytical consideration. We obtain that relative influences of various misalignments are significantly different. We show that the internal occulter with R IO = 1.694 mm = 1.1R ⊙ is large enough to compensate possible misalignments expected to occur in PROBA-3/ASPIICS. Beside that we show that apodizing the edge of the internal occulter leads to additional suppression of the diffracted light. Conclusions. We conclude that the most important misalignment is the tilt of the telescope with respect to the line connecting the center of the external occulter and the entrance aperture. Special care should be taken to co-align the external occulter and the coronagraph, which means co-aligning the diffraction fringe from the external occulter and the internal occulter. We suggest that the best orientation strategy is to point the coronagraph to the center of the external occulter.

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Section: Introductionmentioning

confidence: 99%

Influence of misalignments on the performance of externally occulted solar coronagraphs

Shestov

Zhukov

2018

A&A

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“…Many models 49,50,51 predict that CME acceleration occurs primarily below 2 R☉. Only a handful of observations 52,53,55 have captured complete CME trajectories that track their acceleration through this region, or the associated impulsive expansion of the CME as it rises 54 . Likewise, models of reconnection in eruptions predict the formation of current sheets that drive flows and heating in the middle corona, but these have been observed only infrequently 23,56,57,58 and often the reconnection site itself lies outside the FOV of low coronal imagers 59 .…”

Section: Small-scale Rapid Outflowsmentioning

confidence: 99%

The Sun’s dynamic extended corona observed in extreme ultraviolet

et al. 2021

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The "middle corona" is a critical transition between the highly disparate physical regimes of the lower and outer solar corona. Nonetheless, it remains poorly understood due to the difficulty of observing this faint region (1.5-3 R☉). New observations from the GOES Solar Ultraviolet Imager in August and September 2018 provide the first comprehensive look at this region's characteristics and long-term evolution in extreme ultraviolet (EUV). Our analysis shows that the dominant emission mechanism here is resonant scattering rather than collisional excitation, consistent with recent model predictions. Our observations highlight that solar wind structures in the heliosphere originate from complex dynamics manifesting in the middle corona that do not occur at lower heights. These data emphasize that low-coronal phenomena can be strongly influenced by inflows from above, not only by photospheric motion, a factor largely overlooked in current models of coronal evolution. This study reveals the full kinematic profile of the initiation of several coronal mass ejections, filling a crucial observational gap that has hindered understanding of the origins of solar eruptions. These new data uniquely demonstrate how EUV observations of the middle corona provide strong new constraints on models seeking to unify the corona and heliosphere. Our EUV Observations and the Middle CoronaThe solar corona is the primary driver of almost all plasma dynamics throughout the solar system 1 . However, the precise nature of the connection between the corona and the heliosphere remains surprisingly poorly understood 2 . Recent solar and heliospheric observations taken by Parker Solar Probe, well within Mercury's orbit, revealed a highly structured environment shaped by flows and ejecta interacting with the corona's complex magnetic field 3,4,5,6 . The influence of these flows on the heliosphere and structural evolution

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“…Several studies focused on Sun-to-Earth analysis of CMEs by linking the low coronal behaviour and properties of the eruption with its observed in situ signature (D'Huys et al 2017;Temmer et al 2017). A number of studies also compared magnetic flux rope properties, such as the magnetic flux, the chirality, and its helicity sign determined from post-eruptive arcades, flare ribbons, and coronal dimmings measured close to the Sun with magnetic cloud properties at 1 AU (Qiu et al 2007;Gopalswamy et al 2017;Palmerio et al 2017;James et al 2017).…”

Section: Datamentioning

confidence: 99%

A review of the SCOSTEP’s 5-year scientific program VarSITI—Variability of the Sun and Its Terrestrial Impact

Shiokawa

Georgieva

2021

Prog Earth Planet Sci

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The Sun is a variable active-dynamo star, emitting radiation in all wavelengths and solar-wind plasma to the interplanetary space. The Earth is immersed in this radiation and solar wind, showing various responses in geospace and atmosphere. This Sun–Earth connection variates in time scales from milli-seconds to millennia and beyond. The solar activity, which has a ~11-year periodicity, is gradually declining in recent three solar cycles, suggesting a possibility of a grand minimum in near future. VarSITI—variability of the Sun and its terrestrial impact—was the 5-year program of the scientific committee on solar-terrestrial physics (SCOSTEP) in 2014–2018, focusing on this variability of the Sun and its consequences on the Earth. This paper reviews some background of SCOSTEP and its past programs, achievements of the 5-year VarSITI program, and remaining outstanding questions after VarSITI.

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Solar signatures and eruption mechanism of the August 14, 2010 coronal mass ejection (CME)

Cited by 16 publications

References 47 publications

Influence of misalignments on the performance of externally occulted solar coronagraphs

Influence of misalignments on the performance of externally occulted solar coronagraphs

The Sun’s dynamic extended corona observed in extreme ultraviolet

A review of the SCOSTEP’s 5-year scientific program VarSITI—Variability of the Sun and Its Terrestrial Impact

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