Detection of a High-velocity Prominence Eruption Leading to a CME Associated with a Superflare on the RS CVn-type Star V1355 Orionis

Inoue, Shun; Maehara, Hiroyuki; Notsu, Yuta; Namekata, Kosuke; Honda, Satoshi; Keiichi, Namizaki,; Nogami, Daisaku; Shibata, Kazunari

doi:10.3847/1538-4357/acb7e8

Cited by 18 publications

(22 citation statements)

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“…(10 35-36 erg) on RS CVn-type stars/M-dwarfs seems to have a much larger velocity than solar flares (Houdebine et al 1990;Inoue et al 2023). It appears that there is a weak positive trend if we include solar and stellar data as…”

Section: Velocity Velocity Dispersion and Their Time Evolutionmentioning

confidence: 99%

“…Here, we estimate the area and length scale of the prominence. We basically follow the method described by Inoue et al (2023), but the assumption of optical depth and electron density is original based on the discussion in Section 5.2.4. The luminosity of the blueshift component (L Hα,blue ) at the time of maximum EW is derived as 16.6 ±1.7 × 10 28 erg s −1 for flare E1 and 0.47 ±1.6 × 10 28 erg s −1 for flare E2 as shown in Table 3, based on the results of the Gaussian spectral fit.…”

Section: Area and Length Scalementioning

confidence: 99%

“…-Here, we roughly assume the prominence ionization fraction n e /n H = 0.17 ∼ 0.47 (see Table 1 of Labrosse et al 2010). Note that this value is modified in Notsu et al (2023) because the original values used in Inoue et al (2023) was a mistake. As a result, the mass of prominence is 1.3 10 0.9 2.9 20 -+ g (i.e., 4.0 × 10 19 g-4.2 × 10 20 g) and 1.7 10 1.1…”

Section: ( ) =mentioning

confidence: 99%

“…This is thanks to the long history of ground-and space-based observations, which is a result of their frequent flares and faint stellar quiescent background (e.g., Pettersen et al 1984;Pettersen 1989;Hawley & Fisher 1992). Representatively, spectroscopic observations revealed many flare events associated with blueshifted emission line profiles, called "blue asymmetries," in optical Hydrogen Balmer lines (Houdebine et al 1990;Eason et al 1992;Gunn et al 1994;Crespo-Chacón et al 2006;Fuhrmeister et al 2008Fuhrmeister et al , 2011Vida et al 2016;Flores Soriano & Strassmeier 2017;Fuhrmeister et al 2018;Honda et al 2018;Vida et al 2019;Muheki et al 2020a;Muheki et al 2020b;Koller et al 2021;Maehara et al 2021;Inoue et al 2023), UV lines (Hawley et al 2007;Leitzinger et al 2014), and low-temperature X-ray lines (Argiroffi et al 2019) during flares on M-dwarfs, close binaries, and subgiant/giant stars. These signatures represent the direct evidence of plasma motions in line-of-sight (LOS) direction, and the detected number is very large (>100).…”

Section: Introductionmentioning

confidence: 99%

“…These signatures represent the direct evidence of plasma motions in line-of-sight (LOS) direction, and the detected number is very large (>100). Although their relatively low velocities of 100-300 km s −1 in most cases make it difficult to distinguish whether they originate from prominence eruptions/CMEs or flare-related surface phenomena, some of them are characterized as prominence eruptions leading to CMEs by faster velocities than the stellar surface escape velocities (Houdebine et al 1990;Vida et al 2016Vida et al , 2019Inoue et al 2023). Another promising method to identify stellar CMEs is based on the detection of the XUV dimming observed during solar CMEs forming as a direct result of evacuation and outward propagation of materials from the solar corona, which can last for hours (Mason et al 2016;Jin et al 2022).…”

Section: Introductionmentioning

confidence: 99%

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Multiwavelength Campaign Observations of a Young Solar-type Star, EK Draconis. I. Discovery of Prominence Eruptions Associated with Superflares

Namekata,

Airapetian,

Petit

et al. 2024

ApJ

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Young solar-type stars frequently produce superflares, serving as a unique window into the young Sun-Earth environments. Large solar flares are closely linked to coronal mass ejections (CMEs) associated with filament/prominence eruptions, but observational evidence for stellar superflares remains scarce. Here, we present a 12-day, multiwavelength campaign observation of young solar-type star EK Draconis (G1.5V, 50–120 Myr age) utilizing the Transiting Exoplanet Survey Satellite, the Neutron star Interior Composition ExploreR, and the Seimei telescope. The star has previously exhibited blueshifted Hα absorptions as evidence for a filament eruption associated with a superflare. Our simultaneous optical and X-ray observations identified three superflares of 1.5 × 1033–1.2 × 1034 erg. We report the first discovery of two prominence eruptions on a solar-type star, observed as blueshifted Hα emissions at speeds of 690 and 430 km s−1 and masses of 1.1 × 1019 and 3.2 × 1017 g, respectively. The faster, massive event shows a candidate of post-flare X-ray dimming with the amplitude of up to ∼10%. Several observational aspects consistently point to the occurrence of a fast CME associated with this event. The comparative analysis of the estimated length scales of flare loops, prominences, possible dimming region, and starspots provides the overall picture of the eruptive phenomena. Furthermore, the energy partition of the observed superflares in the optical and X-ray bands is consistent with flares from the Sun, M-dwarfs, and close binaries, yielding the unified empirical relations. These discoveries provide profound implications of the impact of these eruptive events on early Venus, Earth, and Mars and young exoplanets.

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Section: Velocity Velocity Dispersion and Their Time Evolutionmentioning

confidence: 99%

Section: Area and Length Scalementioning

confidence: 99%

Section: ( ) =mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Multiwavelength Campaign Observations of a Young Solar-type Star, EK Draconis. I. Discovery of Prominence Eruptions Associated with Superflares

Namekata,

Airapetian,

Petit

et al. 2024

ApJ

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Flare-related plasma motions in the outer atmosphere of the RS CVn-type star II Peg

Cao,

2024

A&A

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Analogous to solar flares, stellar flares are dramatic explosions in the atmosphere, which may be accompanied by prominence eruptions, coronal mass ejections (CMEs), and other forms of plasma motion. Based on time-resolved spectroscopic observations of the RS CVn-type star II Peg, we aim to search for the potential plasma motions associated with flares. In these observations, we detected part of the gradual decay phase of an optical flare, for which we find a lower limit on the energy of the H$ alpha $ line of $6.03 $ erg. Converting this H$ alpha $ energy, we find a bolometric white-light energy of $3.10 $ erg. Moreover, a secondary peak is also observed. After removing a quiescence reference, the H$ alpha $ residual shows an asymmetric behavior, including both a blueshifted and a redshifted emission component. The former component has a bulk velocity of about -180 km s$^ $ and extends its velocity to more than -350 km s$^ $. This phenomenon is likely caused by a prominence eruption event or a chromospheric evaporation process. The latter emission component has a bulk velocity of 130 to 70 km s$^ $ and extends its velocity to nearly 400 km s$^ $. We attribute the redshifted emission component to one or a combination of several possible scenarios: flare-driven coronal rain, chromospheric condensation, backward-directed prominence eruption close to the stellar limb, or falling material in a prominence eruption. The minimum masses of the moving plasmas resulting in the blueshifted and redshifted emission components are estimated to be $0.56 $ g and $1.74 $ g, respectively.

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Heating and cooling in stellar coronae: coronal rain on a young Sun

Daley-Yates,

Jardine,

Johnston

2023

Monthly Notices of the Royal Astronomical Society

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Recent observations of rapidly rotating cool dwarfs have revealed H α line asymmetries indicative of clumps of cool, dense plasma in the stars’ coronae. These clumps may be either long-lived (persisting for more than one stellar rotation) or dynamic. The fastest dynamic features show velocities greater than the escape speed, suggesting that they may be centrifugally ejected from the star, contributing to the stellar angular momentum loss. Many, however, show lower velocities, similar to coronal rain observed on the Sun. We present 2.5D magnetohydrodynamic simulations of the formation and dynamics of these condensations in a rapidly rotating (Prot = 1 d) young Sun. Formation is triggered by excess surface heating. This pushes the system out of thermal equilibrium and triggers a thermal instability. The resulting condensations fall back towards the surface. They exhibit quasi-periodic behaviour, with periods longer than typical periods for solar coronal rain. We find line-of-sight velocities for these clumps in the range of 50 km s−1 (blueshifted) to 250 km s−1 (redshifted). These are typical of those inferred from stellar H α line asymmetries, but the inferred clump masses of 3.6 × 1014 g are significantly smaller. We find that a maximum of ${\simeq}3~{{ \rm per\ cent}}$ of the coronal mass is cool clumps. We conclude that coronal rain may be common in solar-like stars, but may appear on much larger scales in rapid rotators.

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Detection of a High-velocity Prominence Eruption Leading to a CME Associated with a Superflare on the RS CVn-type Star V1355 Orionis

Cited by 18 publications

References 48 publications

Multiwavelength Campaign Observations of a Young Solar-type Star, EK Draconis. I. Discovery of Prominence Eruptions Associated with Superflares

Multiwavelength Campaign Observations of a Young Solar-type Star, EK Draconis. I. Discovery of Prominence Eruptions Associated with Superflares

Flare-related plasma motions in the outer atmosphere of the RS CVn-type star II Peg

Heating and cooling in stellar coronae: coronal rain on a young Sun

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