Llamaradas Estelares: Modeling the Morphology of White-light Flares

Mendoza, Guadalupe Tovar; Davenport, James R. A.; Agol, Eric; Jackman, James A. G.; Hawley, Suzanne L.

doi:10.3847/1538-3881/ac6fe6

Cited by 21 publications

(2 citation statements)

References 72 publications

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“…The typical time scale of flare events is a few minutes to a few hours, but in some cases, even day-long events have been reported [40,41]. The light curve shape of a typical, single peaked flare is well described by a short rise, and a more gradual, exponential decay phase [42,43]. However, many flares show more complex light curves, especially when observed with higher cadence [44], including multiple peaks, bumps, or quasi-periodic oscillations.…”

Section: Flare Detection In Space-borne Photometrymentioning

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: Flare Detection In Space-borne Photometrymentioning

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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“…The response at optical wavelengths has historically been the best-observed phenomenon in stellar flares, thanks to many decades of ground-based monitoring in the UBVR bandpasses (Lacy et al 1976;Pettersen et al 1984;Hilton 2011) and recent long-baseline, high-precision ancillary white-light data provided by Kepler, K2, and the Transiting Exoplanet Survey Satellite (TESS; Hawley et al 2014;Davenport 2016;Notsu et al 2019;Howard 2022;Mendoza et al 2022). Large observational campaigns spanning the X-ray, UV, optical, and radio have unfortunately been few and far between (Osten et al 2005(Osten et al , 2006.…”

Section: Introductionmentioning

confidence: 99%

A 7 Day Multiwavelength Flare Campaign on AU Mic. I. High-time-resolution Light Curves and the Thermal Empirical Neupert Effect

Tristan

Notsu

Kowalski

et al. 2023

ApJ

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We present light curves and flares from a 7 day, multiwavelength observational campaign of AU Mic, a young and active dM1e star with exoplanets and a debris disk. We report on 73 unique flares between the X-ray to optical data. We use high-time-resolution near-UV (NUV) photometry and soft X-ray (SXR) data from the X-ray Multi-Mirror Mission to study the empirical Neupert effect, which correlates the gradual and impulsive phase flaring emissions. We find that 65% (30 of 46) flares do not follow the Neupert effect, which is 3 times more excursions than seen in solar flares, and propose a four-part Neupert effect classification (Neupert, quasi-Neupert, non-Neupert types I and II) to explain the multiwavelength responses. While the SXR emission generally lags behind the NUV as expected from the chromospheric evaporation flare models, the Neupert effect is more prevalent in larger, more impulsive flares. Preliminary flaring rate analysis with X-ray and U-band data suggests that previously estimated energy ratios hold for a collection of flares observed over the same time period, but not necessarily for an individual, multiwavelength flare. These results imply that one model cannot explain all stellar flares and care should be taken when extrapolating between wavelength regimes. Future work will expand wavelength coverage using radio data to constrain the nonthermal empirical and theoretical Neupert effects to better refine models and bridge the gap between stellar and solar flare physics.

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Searching for similarities in the accretion flow of Seyfert 1 galaxies and cataclysmic variables based on the flare profiles of IRAS 13224–3809, 1H 0707–495, Mrk 766, and MV Lyr

Dobrotka,

Negoro,

Bezák

2024

A&A

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We studied the fast variability of three selected active galactic nuclei (AGNs), IRAS\,13224-3809, 1H\,0707-495, and Mrk\,766, and the cataclysmic variable MV\,Lyr, which were observed by the and spacecrafts, respectively. Our goal is to search for the common origin of the variability and to test the so-called sandwich model, in which a geometrically thick corona surrounds a geometrically thin disc. We studied the substructures of the averaged flare profiles. The flare profile method identifies individual flares in the light curve, and averages them. The direct fitting of the profile substructures identified individual characteristic frequencies that are seen in standard power density spectra (PDS) as a break frequency or quasi-periodic oscillation. The credibility of the flare profile substructures is demonstrated by comparison with the autocorrelation function. We found that the flare profiles of AGNs are similar to those of a cataclysmic variable in the low state. We explain this as a consequence of a truncated inner disc in a sandwich model. The same scenario is also able to explain the characteristic break frequencies in X-ray PDS, which are not seen in the optical. We also searched for substructures in the flare profile of IRAS\,13224-3809. In addition to a permanently present main flare, we found that a transient side-lobe appears before the main flare and is only seen in a high-flux period. The complex flare profile of this AGN suggests that an additional source of X-rays appears during the high-flux period. We propose a scenario in which an accretion flow fluctuation enters the sandwich corona and propagates further to some very central part of the accretion disc.

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Llamaradas Estelares: Modeling the Morphology of White-light Flares

Cited by 21 publications

References 72 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 7 Day Multiwavelength Flare Campaign on AU Mic. I. High-time-resolution Light Curves and the Thermal Empirical Neupert Effect

Searching for similarities in the accretion flow of Seyfert 1 galaxies and cataclysmic variables based on the flare profiles of IRAS 13224–3809, 1H 0707–495, Mrk 766, and MV Lyr

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