Modelling Quasi-Periodic Pulsations in Solar and Stellar Flares
James McLaughlin,Valery M. Nakariakov,Valery M. Nakariakov,Valery M. Nakariakov,M. Dominique,Petr Jelínek,Shinsuke Takasao +6 more
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TLDR
A review of the current understanding of quasi-periodic pulsations in solar and stellar flares can be found in this article, where the authors focus on the possible physical mechanisms, with an emphasis on the underlying physics that generates the resultant range of periodicities.Abstract:
Solar flare emission is detected in all EM bands and variations in flux density of solar energetic particles. Often the EM radiation generated in solar and stellar flares shows a pronounced oscillatory pattern, with characteristic periods ranging from a fraction of a second to several minutes. These oscillations are referred to as quasi-periodic pulsations (QPPs), to emphasise that they often contain apparent amplitude and period modulation. We review the current understanding of quasi-periodic pulsations in solar and stellar flares. In particular, we focus on the possible physical mechanisms, with an emphasis on the underlying physics that generates the resultant range of periodicities. These physical mechanisms include MHD oscillations, self-oscillatory mechanisms, oscillatory reconnection/reconnection reversal, wave-driven reconnection, two loop coalescence, MHD flow over-stability, the equivalent LCR-contour mechanism, and thermal-dynamical cycles. We also provide a histogram of all QPP events published in the literature at this time. The occurrence of QPPs puts additional constraints on the interpretation and understanding of the fundamental processes operating in flares, e.g. magnetic energy liberation and particle acceleration. Therefore, a full understanding of QPPs is essential in order to work towards an integrated model of solar and stellar flares.read more
Citations
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Do Kepler Superflare Stars Really Include Slowly Rotating Sun-like Stars?—Results Using APO 3.5 m Telescope Spectroscopic Observations and Gaia-DR2 Data
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TL;DR: In this article, the authors report the latest view of Kepler solar-type (G-type main-sequence) superflare stars, including recent updates with Apache Point Observatory (APO) 3.5m telescope spectroscopic observations and Gaia-DR2 data.
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Do Kepler superflare stars really include slowly-rotating Sun-like stars ? - Results using APO 3.5m telescope spectroscopic observations and Gaia-DR2 data -
Yuta Notsu,Hiroyuki Maehara,Satoshi Honda,Suzanne L. Hawley,James R. A. Davenport,Kosuke Namekata,Shota Notsu,Kai Ikuta,Daisaku Nogami,Kazunari Shibata +9 more
TL;DR: In this article, the authors report the latest view of Kepler solar-type (G-type main-sequence) superflare stars, including recent updates with Apache Point Observatory (APO) 3.5m telescope spectroscopic observations and Gaia-DR2 data.
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Quasi-Periodic Pulsations in Solar and Stellar Flares: A Review of Underpinning Physical Mechanisms and Their Predicted Observational Signatures
Ivan Zimovets,James McLaughlin,Abhishek K. Srivastava,Dmitrii Y. Kolotkov,Dmitrii Y. Kolotkov,Alexey A. Kuznetsov,Elena G. Kupriyanova,Il-Hyun Cho,Andrew Inglis,Fabio Reale,Fabio Reale,D. J. Pascoe,Hui Tian,Hui Tian,Ding Yuan,Ding Yuan,Dong Li,Q. M. Zhang +17 more
TL;DR: Several mechanisms have been developed to explain quasi-periodic pulsations (QPPs) in solar and stellar flares as discussed by the authors, which mainly assume the presence of magnetohydrodynamic (MHD) oscillations in coronal structures.
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Flaring Activity of Proxima Centauri from TESS Observations: Quasiperiodic Oscillations during Flare Decay and Inferences on the Habitability of Proxima b
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TL;DR: In this article, the authors analyzed the light curve of the M5.5 dwarf Proxima Centauri obtained by the Transiting Exoplanet Survey Satellite (TESS) in Sectors 11 and 12.
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TL;DR: RHESSI as discussed by the authors is a Principal Investigator (PI) mission, where the PI is responsible for all aspects of the mission except the launch vehicle, and is designed to investigate particle acceleration and energy release in solar flares, through imaging and spectroscopy of hard X-ray/gamma-ray continua emitted by energetic electrons, and of gamma-ray lines produced by energetic ions.
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