Simple Model for Temporal Variations of Hα Spectrum by an Eruptive Filament from a Superflare on a Solar-type Star

Ikuta, Kai; Shibata, Kazunari

doi:10.3847/1538-4357/ad1ce6

Cited by 5 publications

(1 citation statement)

References 62 publications

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“…This can not be explained with scattering only, as the emissivity of the prominence/filament needs to be taken into account in the formalism. Ikuta and Shibata [186] applied a 1D hydrodynamical simulation of the plasma flow to the possible filament eruption seen in Hα from Namekata et al [187]. The authors find that the variations (absorption) seen in the stellar Hα profile can be explained in terms of a failed filament eruption.…”

Section: Stellar Cmesmentioning

confidence: 99%

Stellar Flares, Superflares and Coronal Mass Ejections – Entering the Big Data Era

Vida,

Kővári,

Leitzinger

et al. 2024

Preprint

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Flares, sometimes accompanied by coronal mass ejections (CMEs), are the result of sudden changes in the magnetic field of stars with high energy release through magnetic reconnection, which can be observed across a wide range of the electromagnetic spectrum from radio waves to the optical range to X-rays. In our review, we attempt to collect some fundamental new results, which can largely be linked to the Big data era that has arrived due to the expansion of space photometric observations of the last two decades. We list the different types of stars showing flare activity, their observation strategies, and discuss how their main stellar properties relate to the characteristics of the flares (or even CMEs) they emit. Our goal is to focus, without claiming to be complete, on those results that may in one way or another challenge the "standard" flare model based on the solar paradigm.

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Section: Stellar Cmesmentioning

confidence: 99%

Stellar Flares, Superflares and Coronal Mass Ejections – Entering the Big Data Era

Vida,

Kővári,

Leitzinger

et al. 2024

Preprint

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A fast-filament eruption observed in the Hα spectral line

Cabezas,

Ichimoto,

Asai

et al. 2024

A&A

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Solar filament eruptions usually appear to occur in association with the sudden explosive release of magnetic energy accumulated in long-lived arched magnetic structures. The released energy occasionally drives fast-filament eruptions that can the be source regions of coronal mass ejections. A quantitative analysis of high-speed filament eruptions is thus essential to help elucidate the formation and early acceleration of coronal mass ejections. The goal of this paper is to investigate the dynamic processes of a fast-filament eruption by using unprecedented high-resolution full-disk Halpha imaging spectroscopy observations. The whole process of the eruption was captured in a wide spectral window of the Halpha line ($ AA ), which allowed for the detection of highly Doppler-shifted plasma. By applying the ``cloud model'' and obtaining two-dimensional optical thickness spectra, we derived the Doppler velocity; the true eruption profiles (height, velocity, and acceleration); and the trajectory of the filament eruption in 3D space. The Doppler velocity maps show that the filament was predominantly blueshifted. During the main and final process of the eruption, strongly blueshifted materials manifest, traveling with velocities exceeding $250 km $. The spectral analysis further revealed that the erupting filament is made of multiple components, some of which were Doppler-shifted approximately to $-300 km $. We found that the filament eruption attains a maximum true velocity and acceleration of about $600 km $ and $2.5 km $, respectively, and its propagation direction deviates from the radial direction. On the other hand, downflows manifested as redshifted plasma close to the footpoints of the erupting filament move with velocities of $45-125 km $. We interpret these redshifted signatures as draining material and therefore as mass loss of the filament, which has implications for the dynamic and the acceleration process of the eruption. Furthermore, we have estimated the total mass of the Halpha filament, resulting in sim $5.4 g

show abstract

Stellar Flares, Superflares, and Coronal Mass Ejections—Entering the Big Data Era

Vida,

Kővári,

Leitzinger

et al. 2024

Universe

View full text Add to dashboard Cite

Flares, sometimes accompanied by coronal mass ejections (CMEs), are the result of sudden changes in the magnetic field of stars with high energy release through magnetic reconnection, which can be observed across a wide range of the electromagnetic spectrum from radio waves to the optical range to X-rays. In our observational review, we attempt to collect some fundamental new results, which can largely be linked to the Big Data era that has arrived due to the expansion of space photometric observations over the last two decades. We list the different types of stars showing flare activity and their observation strategies and discuss how their main stellar properties relate to the characteristics of the flares (or even CMEs) they emit. Our goal is to focus, without claiming to be complete, on those results that may, in one way or another, challenge the “standard” flare model based on the solar paradigm.

show abstract

Simple Model for Temporal Variations of Hα Spectrum by an Eruptive Filament from a Superflare on a Solar-type Star

Cited by 5 publications

References 62 publications

Stellar Flares, Superflares and Coronal Mass Ejections – Entering the Big Data Era

Stellar Flares, Superflares and Coronal Mass Ejections – Entering the Big Data Era

A fast-filament eruption observed in the Hα spectral line

Stellar Flares, Superflares, and Coronal Mass Ejections—Entering the Big Data Era

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