Erratum: “The Flare Catalog and the Flare Activity in the Kepler Mission” (2019, ApJS, 241, 29)

Yang, Hui; Liu, Jifeng

doi:10.3847/1538-4365/abb1ab

Cited by 20 publications

(45 citation statements)

References 3 publications

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“…For the mid-to-late M-dwarf sample of Medina et al (2020), the power law index is α = 1.98 ± 0.02. Yang & Liu (2019) compiled a catalogue of flares using all available long cadence Kepler light curves from DR25, and found an average α ≈ 2 power law index for all spectral types excluding A-stars, and also a ∼ 10% incidence rate of flare stars among M-dwarfs, consistent with our result (∼ 8%). So it appears that the slope found for the TRAPPIST-1 analogues here (α = 2.11) is typical for late Mdwarfs, and consistent with TRAPPIST-1 itself (α = 2.03).…”

Section: Flare Frequency Distributionsupporting

confidence: 83%

Activity of TRAPPIST-1 analogue stars observed with TESS

Seli,

Vida,

Moór

et al. 2021

Preprint

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As more exoplanets are being discovered around ultracool dwarfs, understanding their magnetic activity -and the implications for habitability -is of prime importance. To find stellar flares and photometric signatures related to starspots, continuous monitoring is necessary, which can be achieved with spaceborn observatories like the Transiting Exoplanet Survey Satellite (TESS). We present an analysis of TRAPPIST-1 like ultracool dwarfs with TESS full-frame image photometry from the first two years of the primary mission. A volume-limited sample up to 50 pc is constructed consisting of 339 stars closer than 0. m 5 to TRAPPIST-1 on the Gaia colour-magnitude diagram. The 30-min cadence TESS light curves of 248 stars were analysed, searching for flares and rotational modulation caused by starspots. The composite flare frequency distribution of the 94 identified flares shows a power law index similar to TRAPPIST-1, and contains flares up to E TESS = 3 × 10 33 erg. Rotational periods shorter than 5 d were determined for 42 stars, sampling the regime of fast rotators. The ages of 88 stars from the sample were estimated using kinematic information. A weak correlation between rotational period and age is observed, which is consistent with magnetic braking.

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Section: Flare Frequency Distributionsupporting

confidence: 83%

Activity of TRAPPIST-1 analogue stars observed with TESS

Seli,

Vida,

Moór

et al. 2021

Preprint

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“…Comparing the flare energies of a mixed sample of flares observed on giant stars by Kepler (Yang & Liu 2019) against the flare energies of KIC 2852961 we find that KIC 2852961 flares are more powerful. Both the 35.503 mean and the 35.417 median of the log E f values in the cited sample of 6842 flares from giant stars are well below our values of 37.286 and 37.384, re-spectively.…”

Section: On the Cumulative Flare Frequency Diagrammentioning

confidence: 91%

Superflares on the late-type giant KIC 2852961

Kővári

Oláh

Günther

et al. 2020

A&A

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Context. The most powerful superflares reaching 1039 erg bolometric energy are from giant stars. The mechanism behind flaring is thought to be the magnetic reconnection, which is closely related to magnetic activity (including starspots). However, it is poorly understood how the underlying magnetic dynamo works and how the flare activity is related to the stellar properties that eventually control the dynamo action. Aims. We analyze the flaring activity of KIC 2852961, a late-type giant star, in order to understand how its flare statistics are related to those of other stars with flares and superflares, and to understand the role of the observed stellar properties in generating flares. Methods. We searched for flares in the full Kepler dataset of KIC 2852961 using an automated technique together with visual inspection. We cross-matched the flare-like events detected by the two different approaches and set a final list of 59 verified flares during the observing term. We calculated flare energies for the sample and performed a statistical analysis. Results. The stellar properties of KIC 2852961 are revised and a more consistent set of parameters are proposed. The cumulative flare energy distribution can be characterized by a broken power law; that is to say, on the log-log representation the distribution function is fitted by two linear functions with different slopes, depending on the energy range fitted. We find that the total flare energy integrated over a few rotation periods correlates with the average amplitude of the rotational modulation due to starspots. Conclusions. Flares and superflares seem to be the result of the same physical mechanism at different energy levels, also implying that late-type stars in the main sequence and flaring giant stars have the same underlying physical process for emitting flares. There might be a scaling effect behind the generation of flares and superflares in the sense that the higher the magnetic activity, the higher the overall magnetic energy released by flares and/or superflares.

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“…The brightest solar flares have a bolometric output of ∼ 10 32 ergs. Observations of Sun-like stars have shown that about ∼ 1% of stars display 'super-flares' with a bolometric output of 10 32 − 10 36 ergs (Yang & Liu 2019;Günther et al 2020). It is reasonable to expect that the accompanying radio emissions will be significantly brighter because both the radio and optical emission are ultimately powered by the same engine.…”

Section: The Ensemble Of Flaring Starsmentioning

confidence: 99%

“…The constants C 32 and α for a large population of stars of various spectral types have been well constrained by the Kepler emission, particularly for large flares in the range 10 32 − 10 36 ergs. Here I adopt the rates published by Yang & Liu (2019). Only 1.46% of the targeted G-dwarfs showed detectable flaring activity.…”

Section: The Ensemble Of Flaring Starsmentioning

confidence: 99%

“…I must at the outset qualify what 'Sun-like' means in this context. Stellar flares have been routinely detected in optical (Yang & Liu 2019;Günther et al 2020) and X-ray observations (Pye et al 2015). Such observations provide a reasonable estimate of the flare energy and duration but do not provide a concrete picture of the dynamics of the flare.…”

Section: Introductionmentioning

confidence: 99%

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Prospects for radio detection of stellar plasma beams

Vedantham

2020

Preprint

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Violent solar eruptions are often accompanied by relativistic beams of charged particles. In the solar context, they are referred to as SPEs (Solar Particle Events) and are known to generate a characteristic swept-frequency radio burst. Due to their ionizing potential, such beams influence atmospheric chemistry and habitability. Radio observations provide a crucial discriminant between stellar flares that do and do not generate particle beams. Here I use solar empirical data and semi-quantitative theoretical estimates to gauge the feasibility of detecting the associated radio bursts. My principal conclusion is that a dedicated search for swept frequency radio bursts on second-timescales in existing low-frequency (ν 10 2 MHz) datasets, while technically challenging, will likely evidence high energy particles beams in Sun-like stars.

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Erratum: “The Flare Catalog and the Flare Activity in the Kepler Mission” (2019, ApJS, 241, 29)

Cited by 20 publications

References 3 publications

Activity of TRAPPIST-1 analogue stars observed with TESS

Activity of TRAPPIST-1 analogue stars observed with TESS

Superflares on the late-type giant KIC 2852961

Prospects for radio detection of stellar plasma beams

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