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SUPERFLARES ON SOLAR-TYPE STARS OBSERVED WITH KEPLER . I. STATISTICAL PROPERTIES OF SUPERFLARES
Open accessAbstract
By extending our previous study by Maehara et al., we searched for superflares on G-type dwarfs (solar-type stars) using Kepler data for a longer period (500 days) than that (120 days) in our previous study. As a result, we found 1547 superflares on 279 G-type dwarfs, which is much more than the previous 365 superflares on 148 stars. Using these new data, we studied the statistical properties of the occurrence rate of superflares, and confirmed the previous results, i.e., the occurrence rate ( dN / dE ) of superflares versus flare energy ( E ) shows a power-law distribution with dN / dE ∝ E −α , where α ∼ 2. It is interesting that this distribution is roughly similar to that for solar flares. In the case of the Sun-like stars (with surface temperature 5600–6000 K and slowly rotating with a period longer than 10 days), the occurrence rate of superflares with an energy of 10 34 –10 35 erg is once in 800–5000 yr. We also studied long-term (500 days) stellar brightness variation of these superflare stars and found that in some G-type dwarfs the occurrence rate of superflares was extremely high, ∼57 superflares in 500 days (i.e., once in 10 days). In the case of Sun-like stars, the most active stars show a frequency of one superflare (with 10 34 erg) in 100 days. There is evidence that these superflare stars have extremely large starspots with a size about 10 times larger than that of the largest sunspot. We argue that the physical origin of the extremely high occurrence rate of superflares in these stars may be attributed to the existence of extremely large starspots.
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“A large number of superflares have also been detected for solar-type stars (e.g., Maehara et al. 2012, 2015; Shibayama et al. 2013; Katsova & Livshits 2015).”
From ABOUT EXOBIOLOGY: THE CASE FOR DWARF K STARS (2016) · cites this paper as Shibayama et al. 2013
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THE KEPLER CATALOG OF STELLAR FLARES
Davenport, J. R. A. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/829/1/23 · Cited by 388
“Shibayama et al. (2013) accomplish this by assum- ing blackbody radiation from both the star and flare, as well as a fixed flare temperature of 10, 000 K.”
BackgroundPerryman, M. A. C. (2011) · Cambridge University Press eBooks · doi:10.1017/9781108304160 · Cited by 380
Stellar Flares from the First TESS Data Release: Exploring a New Sample of M Dwarfs
Günther, M. N., Zhan, Z., Seager, S., Rimmer, P. B., Ranjan, S., Stassun, K. G., Oelkers, R. J., Daylan, T., Newton, E. R., Kristiansen, M. H., et al. (2020) · The Astronomical Journal · doi:10.3847/1538-3881/ab5d3a · Cited by 396
“Measuring the flare energy We calculate the flare energy from the stellar luminosity and the best fitting flare profile, following Shibayama et al. (2013).”
BackgroundMethodResultInfluentialPrebiotic chemistry and atmospheric warming of early Earth by an active young Sun
Airapetian, V., Glocer, A., Gronoff, G., Hébrard, É., & Danchi, W. C. (2016) · Nature Geoscience · doi:10.1038/ngeo2719 · Cited by 336
The economic impact of space weather: where do we stand?
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“, NASA’s Kepler spacecraft(74,75) suggests that superflares ( 10x Carrington) may occur on millennial timescales, but this is still controversial.”
BackgroundFlare-productive active regions
Toriumi, S., & Wang, H. (2019) · Living Reviews in Solar Physics · doi:10.1007/s41116-019-0019-7 · Cited by 325
Stellar Flares from the First TESS Data Release: Exploring a New Sample of M Dwarfs
Günther, M. N., Zhan, Z., Seager, S., Rimmer, P. B., Ranjan, S., Stassun, K. G., Oelkers, R. J., Daylan, T., Newton, E. R., Kristiansen, M. H., et al. (2020) · Repository of the Academy's Library (Library of the Hungarian Academy of Sciences) · Cited by 258
Johnstone, C. P., Bartel, M., & Güdel, M. (2020) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202038407 · Cited by 250
Impact of space weather on climate and habitability of terrestrial-type exoplanets
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“…solar flares are roughly on the same power-law line with an index of α = −1.8 (thin solid line) for the wide energy range between 1024 and 1035 erg. Shibayama et al. (2013) found that superflares from young (0.7 Gyr) solar-like stars with the energy of 1034 erg occur at the rate of 0.1 event…”
BackgroundInfluentialSelf-citationThe habitability of Proxima Centauri b
Ribas, I., Bolmont, É., Selsis, F., Reiners, A., Leconte, J., Raymond, S. N., Engle, S. G., Guinan, E. F., Morin, J., Turbet, M., et al. (2016) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201629576 · Cited by 252
“The current Sun, as well as average Sun-like stars observed by Kepler, and Proxima, are flaring at roughly the same rate, which is a factor of ∼10 higher than solar minimum (Shibayama et al. 2013).”
Background25 Years of Self-Organized Criticality: Solar and Astrophysics
Aschwanden, M. J., Crosby, N. B., Dimitropoulou, M., Georgoulis, M. K., Hergarten, S., McAteer, R. T. J., Milovanov, A. V., Mineshige, S., Morales, L., Nishizuka, N., et al. (2014) · Space Science Reviews · doi:10.1007/s11214-014-0054-6 · Cited by 251
“…Arzner and Güdel (2004), Arzner et al. (2007), Stelzer et al. (2007), Maehara et al. 2012; Shibayama et al. (2013); 24) Maehara et al. (2012); Shibayama et al. (2013); 25) Argyle and Gower (1972), Lundgren et al. (1995); 26) Cognard et al. (1996); 27) Gogus et al. (1999, 2000); 28) Negoro…”
BackgroundMethodInfluentialStatistical properties of superflares on solar-type stars based on 1-min cadence data
Maehara, H., Shibayama, T., Notsu, Y., Notsu, S., Honda, S., Nogami, D., & Shibata, K. (2015) · Earth Planets and Space · doi:10.1186/s40623-015-0217-z · Cited by 242
“…National Astronomical Observatory of Japan, 3037-5 Honjo, Kamogata, Asakuchi, Okayama 719-0232, Japan Full list of author information is available at the end of the article stars) have been discovered by the Kepler space telescope (Maehara et al. 2012; Shibayama et al. 2013; Wu et al. 2015).”
BackgroundMethodInfluentialSelf-citationStatistical properties of superflares on solar-type stars based on 1-min cadence data
Maehara, H., Shibayama, T., Notsu, Y., Notsu, S., Honda, S., Nogami, D., & Shibata, K. (2015) · Institutional Repositories DataBase (IRDB) · Cited by 178
Self-citationFlare stars across the H–R diagram
Balona, L. A. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu2651 · Cited by 181
“…photometric observations from space from the Kepler satellite not only provided the opportunity for the discovery of superflares on cool stars (Maehara et al., 2012; Shibayama et al., 2013), but also lead to the discovery of superflares on stars hotter than 7500 K (the A stars; Balona, 2012).”
BackgroundCliver, E. W., Schrijver, C. J., Shibata, K., & USOSKIN, I. G. (2022) · Living Reviews in Solar Physics · doi:10.1007/s41116-022-00033-8 · Cited by 216
Self-citationNotsu, Y., Maehara, H., Honda, S., Hawley, S. L., Davenport, J. R. A., Namekata, K., Notsu, S., Ikuta, K., Nogami, D., & Shibata, K. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab14e6 · Cited by 183
Self-citationStatistical Studies of Solar White-light Flares and Comparisons with Superflares on Solar-type Stars
Namekata, K., Sakaue, T., Watanabe, K., Asai, A., Maehara, H., Notsu, Y., Notsu, S., Honda, S., Ishii, T. T., Ikuta, K., et al. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa9b34 · Cited by 181
“We then calculated the energy and duration in the same way as in Shibayama et al. (2013) and Maehara et al. (2015).”
BackgroundMethodInfluentialSelf-citationThe Flaring Activity of M Dwarfs in the Kepler Field
Yang, H., Liu, J., Gao, Q. Z., Fang, X., Guo, J., Zhang, Y., Hou, Y., Wang, Y., & Cao, Z. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa8ea2 · Cited by 172
“Aflare is the area of the flare, and according to Shibayama et al. (2013), it can be estimated by the ratio of flare luminosity and stellar luminosity using A C R R B T d R B T d , 2flare flare 2 flare eff ò ò p l l = l l l l ( ) ( ) ( ) where Rl is the Kepler response function (Van Cleve &…”
BackgroundMethodInfluentialSolar Science with the Atacama Large Millimeter/Submillimeter Array—A New View of Our Sun
Wedemeyer, S., Bastian, T., Brajša, R., Hudson, H., Fleishman, G. D., Loukitcheva, M. A., Fleck, B., Kontar, E. P., Pontieu, B. D., Yagoubov, P., et al. (2015) · Space Science Reviews · doi:10.1007/s11214-015-0229-9 · Cited by 166
“Data for active G dwarfs are taken from Shibayama et al (2013) which took 46,000 hrs of observations on 4 stars observing 116 flares.”
MethodAlvarado‐Gómez, J. D., Drake, J. J., Cohen, O., Moschou, S. P., & Garraffo, C. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aacb7f · Cited by 166
“Flares in very active stars can be 103–106 times more energetic than solar flares (c.f. Osten et al. 2007; Kowalski et al. 2010; Shibayama et al. 2013; Davenport 2016).”
BackgroundDoorsselaere, T. V., Kupriyanova, E. G., & Yuan, D. (2016) · Solar Physics · doi:10.1007/s11207-016-0977-z · Cited by 171
“…suggests that loop motions can be used as a diagnostic for the removal of coronal magnetic energy by flares (confirming the observational results of Simões et al., 2013), and the rapid decrease of coronal magnetic energy is a newly identified excitation mechanism for transverse loop oscillations…”
The MUSCLES Treasury Survey. V. FUV Flares on Active and Inactive M Dwarfs* † ‡
Loyd, R. O. P., France, K. C., Youngblood, A. A., Schneider, C., Brown, A., Hu, R., Segura, A., Linsky, J. L., Redfield, S., Tian, F., et al. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aae2bd · Cited by 149
Eyer, L., Rimoldini, L., Audard, M., Anderson, R. I., Nienartowicz, K., Glass, F., Marchal, O., Grenon, M., Mowlavï, N., Holl, B., et al. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201833304 · Cited by 154
Probable detection of an eruptive filament from a superflare on a solar-type star
Namekata, K., Maehara, H., Honda, S., Notsu, Y., Okamoto, S., Takahashi, J., Takayama, M., Ohshima, T., Saito, T., Katoh, N., et al. (2021) · Nature Astronomy · doi:10.1038/s41550-021-01532-8 · Cited by 158
Self-citationThe Flare Catalog and the Flare Activity in the Kepler Mission
Yang, H., & Liu, J. (2019) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/ab0d28 · Cited by 147
“The approach of the energy estimation is according to Shibayama et al. (2013) and Yang et al. (2017).”
BackgroundMethodResultInfluentialSUPERFLARE OCCURRENCE AND ENERGIES ON G-, K-, AND M-TYPE DWARFS
Candelaresi, S., Hillier, A., Maehara, H., Brandenburg, A., & Shibata, K. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/792/1/67 · Cited by 119
“Maehara et al. (2012) and Shibayama et al. (2013) determined a power-law behavior for the dependence of flare frequency on flare energy.”
BackgroundResultInfluentialSelf-citationOkamoto, S., Notsu, Y., Maehara, H., Namekata, K., Honda, S., Ikuta, K., Nogami, D., & Shibata, K. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/abc8f5 · Cited by 126
Self-citationKowalski, A. F. (2024) · Living Reviews in Solar Physics · doi:10.1007/s41116-024-00039-4 · Cited by 157
Rimoldini, L., Holl, B., Gavras, P., Audard, M., Ridder, J. D., Mowlavï, N., Nienartowicz, K., de Fombelle, G. J., Lecœur-Taı̈bi, I., Karbevska, L., et al. (2023) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202245591 · Cited by 115
ON THE DIVERSITY OF MAGNETIC INTERACTIONS IN CLOSE-IN STAR-PLANET SYSTEMS
Strugarek, A., Brun, A. S., Matt, S. P., & Réville, V. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/795/1/86 · Cited by 107
“In addition, SPIs were also proposed to be at the origin of super-flares (Rubenstein & Schaefer 2000), although the lack of correlations between super-flaring stars and hot-Jupiter hosts observed with Kepler (Shibayama et al. 2013) suggests other triggering mechanisms (see Shibata et al. 2013).”
BackgroundObservational evidence for enhanced magnetic activity of superflare stars
Karoff, C., Knudsen, M. F., Cat, P. D., Bonanno, A. M., Fogtmann-Schulz, A., Fu, J.-N., Frasca, A., Inceoglu, F., Olsen, J., Zhang, Y., et al. (2016) · Nature Communications · doi:10.1038/ncomms11058 · Cited by 102
The Evolution of Flare Activity with Stellar Age
Davenport, J. R. A., Covey, K. R., Clarke, R., Boeck, A. C., Cornet, J., & Hawley, S. L. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/aafb76 · Cited by 98
“As Shibayama et al. (2013) and Clarke et al. (2018) noted, flare activity might vary by an order of magnitude over their activity cycles (see also Veronig et al. 2002), and so our sample may preferentially include stars near their highest activity states.”
BackgroundMethodInfluentialMaehara, H., Notsu, Y., Namekata, K., Honda, S., Kowalski, A. F., Katoh, N., Ohshima, T., Iida, K., Oeda, M., Murata, K. L., et al. (2020) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psaa098 · Cited by 99
Self-citationStatistical properties of quasi-periodic pulsations in white-light flares observed with Kepler
Pugh, C. E., Armstrong, D. J., Nakariakov, V. M., & Broomhall, A.-M. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw850 · Cited by 90
“The energies of the superflares were estimated using a similar method to Shibayama et al. (2013).”
MethodStellar Flares Observed in Long-cadence Data from the Kepler Mission
Doorsselaere, T. V., Shariati, H., & Debosscher, J. (2017) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/aa8f9a · Cited by 92
“To study superflares, Maehara et al. (2012, 2015), Shibayama et al. (2013), and Candelaresi et al. (2014) selected a sample of G-type stars or later, to obtain power laws for flare amplitudes per star.”
BackgroundRisks for Life on Habitable Planets from Superflares of Their Host Stars
Lingam, M., & Loeb, A. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa8e96 · Cited by 86
“A detailed analysis of the Kepler data led to the conclusion that flares of energy ~1034 erg would occur every ∼2000 years (Shibayama et al. 2013).”
BackgroundMethodInfluentialQUASI-PERIODIC PULSATIONS IN SOLAR AND STELLAR FLARES. REVIEW
Kupriyanova, E. G., Kolotkov, D. Y., Nakariakov, V. M., & Kaufman, A. (2020) · Solar-Terrestrial Physics · doi:10.12737/stp-61202001 · Cited by 100
“A comparison of the statistical results for solar and stellar flares allows us to estimate the mean occurrence rate of solar flares with an energy of about 1034–1035 erg (i.e. 100–1000 times more powerful than the Carrington flare) as one event in 800–5000 years [Shibayama et al., 2013].”
Starspot activity and superflares on solar-type stars
Maehara, H., Notsu, Y., Notsu, S., Namekata, K., Honda, S., Ishii, T. T., Nogami, D., & Shibata, K. (2017) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psx013 · Cited by 91
Self-citationSuperflares on Solar-type Stars from the First Year Observation of TESS
Tu, Z.-L., Yang, M., Zhang, Z. J., & Wang, F. Y. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab6606 · Cited by 99
“However, a lot of statistical works based on Kepler data did not detected hot Jupiters around flare stars (Maehara et al. 2012; Shibayama et al. 2013; Maehara et al. 2015).”
BackgroundMethodResultInfluentialPerryman, M. A. C. (2018) · Cambridge University Press eBooks · doi:10.1017/9781108304160.017 · Cited by 89
Wu, C.-J., Ip, W., & Huang, L.-C. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/798/2/92 · Cited by 79
K2 Ultracool Dwarfs Survey. III. White Light Flares Are Ubiquitous in M6-L0 Dwarfs
Paudel, R. R., Gizis, J. E., Mullan, D. J., Schmidt, S. J., Burgasser, A. J., Williams, P. K. G., & Berger, E. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aab8fe · Cited by 86
“…superflares on so many cool targets (the flares discussed here, plus the flares discussed in Schmidt et al. (2016) and Gizis et al. (2017b)) suggests that this is a universal phenomenon which is commonly observed on solar-type stars (Maehara et al. 2012; Shibayama et al. 2013; Notsu et al. 2013).”
BackgroundFlares in open clusters with K2
Ilin, E., Schmidt, S. J., Poppenhaeger, K., Davenport, J. R. A., Kristiansen, M. H., & Omohundro, M. (2020) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202039198 · Cited by 90
Aschwanden, M. J. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/782/1/54 · Cited by 74
Namekata, K., Maehara, H., Notsu, Y., Toriumi, S., Hayakawa, H., Ikuta, K., Notsu, S., Honda, S., Nogami, D., & Shibata, K. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/aaf471 · Cited by 80
Self-citationChang, S.-W., Byun, Y., & Hartman, J. D. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/814/1/35 · Cited by 76
“In a larger sample of stars of similar spectral types, this statistical approach is useful to understand their flaring nature (e.g., Kowalski et al. 2009; Hilton 2011; Walkowicz et al. 2011; Osten et al. 2012; Davenport et al. 2012; Shibayama et al. 2013).”
BackgroundMethodABOUT EXOBIOLOGY: THE CASE FOR DWARF K STARS
Cuntz, M., & Guinan, E. F. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/827/1/79 · Cited by 77
“A large number of superflares have also been detected for solar-type stars (e.g., Maehara et al. 2012, 2015; Shibayama et al. 2013; Katsova & Livshits 2015).”
BackgroundTRAPPIST-1: Global results of theSpitzerExploration Science Program Red Worlds
Ducrot, E., Gillon, M., Delrez, L., Agol, E., Rimmer, P., Turbet, M., Günther, M. N., Demory, B.-O., Triaud, A. H. M. J., Bolmont, É., et al. (2020) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201937392 · Cited by 87
Tu, Z.-L., Yang, M., Wang, H.-F., & Wang, F. Y. (2021) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/abda3c · Cited by 72
“…(Aschwanden et al. 2000), solar microflares (Crosby et al. 1993), solar flares (Shimizu 1995), and superflares on solar-type stars from Kepler (Shibayama et al. 2013; Maehara et al. 2015) and TESS (Tu et al. 2020; this work) basically distribute around µ -dN dE E 1.8 (black dashed–dotted…”
BackgroundMethodResultInfluentialNamekata, K., Airapetian, V., Petit, P. M., Maehara, H., Ikuta, K., Inoue, S., Notsu, Y., Paudel, R. R., Arzoumanian, Z., Avramova-Boncheva, A., et al. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad0b7c · Cited by 76
“The calculation of bolometric WL fl are energy follows the conventional technique proposed by Shibayama et al. 2013.”
BackgroundMethodSelf-citationVida, K., Oláh, K., Kővári, Z., van Driel-Gesztelyi, L., Moór, A., & Pál, A. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab41f5 · Cited by 68
The Near-ultraviolet Continuum Radiation in the Impulsive Phase of HF/GF-type dMe Flares. I. Data
Kowalski, A. F., Wisniewski, J. P., Hawley, S. L., Osten, R. A., Brown, A., Fariña, C., Valenti, J. A., Brown, S., Xilouris, E. M., Schmidt, S. J., et al. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/aaf058 · Cited by 71
“In Kepler 30-minute cadence data (e.g. Walkowicz et al. 2011; Shibayama et al. 2013; Davenport 2016; Yang et al. 2017; Van Doorsselaere et al. 2017), the flare would be a single point at the level indicated in the plot.”
BackgroundParticles and Photons as Drivers for Particle Release from the Surfaces of the Moon and Mercury
Wurz, P., Fatemi, S., Galli, A., Halekas, J. S., Harada, Y., Jäggi, N., Jasinski, J. M., Lammer, H., Lindsay, S. T., Nishino, M. N., et al. (2022) · Space Science Reviews · doi:10.1007/s11214-022-00875-6 · Cited by 73
Large 14 C excursion in 5480 BC indicates an abnormal sun in the mid-Holocene
Miyake, F., Jull, A. J. T., Panyushkina, I. P., Wacker, L., Salzer, M., Baisan, C. H., Lange, T., Cruz, R., Masuda, K., & Nakamura, T. (2017) · Proceedings of the National Academy of Sciences · doi:10.1073/pnas.1613144114 · Cited by 67
“In the observation of solar-type stars by the Kepler telescope, stars where several superflares occurred over several years were detected (28).”
BackgroundTHRESHOLDED POWER LAW SIZE DISTRIBUTIONS OF INSTABILITIES IN ASTROPHYSICS
Aschwanden, M. J. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/814/1/19 · Cited by 68
“…1 data (Walkowicz et al. 2011), 365 superflares from slowly rotating solar-type stars (Maehara et al. 2012), 1547 superflares on 279 G-type dwarfs (Shibayama et al. 2013), 209 flares from K-M flare stars and A-F stars (Balona 2015), and 4944 superflares on 77 G-type stars (Wu, Ip, and Huang 2015).”
BackgroundInfluentialFlares in open clusters with K2
Ilin, E., Schmidt, S. J., Davenport, J. R. A., & Strassmeier, K. G. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201834400 · Cited by 70
K2 Ultracool Dwarfs Survey. III. White Light Flares Are Ubiquitous in M6-L0 Dwarfs
Paudel, R. R., Gizis, J. E., Mullan, D. J., Schmidt, S. J., Burgasser, A. J., Williams, P. K. G., & Berger, E. (2018) · Maryland Shared Open Access Repository (USMAI Consortium) · doi:10.13016/m2o6ru-kmdn · Cited by 65
Notsu, Y., Honda, S., Maehara, H., Notsu, S., Shibayama, T., Nogami, D., & Shibata, K. (2015) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psv002 · Cited by 66
“Shibayama et al. (2013) confirmed that the occurrence rate (dN/dE) of the superflare versus the flare energy (E) has a power-law distribution of dN/dE ∝ E−α, where α ∼ 2, and this distribution is roughly similar to that for the solar flare.”
BackgroundMethodInfluentialSelf-citationTime-resolved spectroscopic observations of an M-dwarf flare star EV Lacertae during a flare
Honda, S., Notsu, Y., Namekata, K., Notsu, S., Maehara, H., Ikuta, K., Nogami, D., & Shibata, K. (2018) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psy055 · Cited by 64
“Recent photometric data from the Kepler spacecraft found many superflare events on G, K, M-type stars (cf. Maehara et al. 2012, Shibayama et al. 2013, Notsu et al. 2013, Candelaresi et al. 2014, Hawley et al. 2014, Davenport 2016, Yang et al. 2017).”
BackgroundSelf-citationRetrospective analysis of GLEs and estimates of radiation risks
Miroshnichenko, L. I. (2018) · Journal of Space Weather and Space Climate · doi:10.1051/swsc/2018042 · Cited by 66
“Exhaustive statistics of the Kepler mission on superflares at other Sun-like stars with solar rotation rates (Maehara et al., 2012; Shibayama et al., 2013; Nogami et al., 2014; Wichmann et al., 2014, and many others) have greatly reinvigorated the discussion of whether or not such events could in…”
BackgroundSolar superstorm of AD 774 recorded subannually by Arctic tree rings
Uusitalo, J., Arppe, L., Hackman, T., Helama, S., Kovaltsov, G. A., Mielikäinen, K., Mäkinen, H. H., Nöjd, P., Palonen, V., USOSKIN, I. G., et al. (2018) · Nature Communications · doi:10.1038/s41467-018-05883-1 · Cited by 66
Superflares and variability in solar-type stars with TESS in the Southern hemisphere
Doyle, L., Ramsay, G., & Doyle, J. G. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa923 · Cited by 68
TRAPPIST-1: Global results of the Spitzer Exploration Science Program Red Worlds★
Ducrot, E., Gillon, M., Delrez, L., Agol, E., Rimmer, P. B., Turbet, M., Günther, M. N., Demory, B.-O., Triaud, A. H. M. J., Bolmont, É., et al. (2020) · Apollo (University of Cambridge) · doi:10.17863/cam.55531 · Cited by 59
Colloquium: Physical constraints for the evolution of life on exoplanets
Lingam, M., & Loeb, A. (2019) · Reviews of Modern Physics · doi:10.1103/revmodphys.91.021002 · Cited by 64
Gavras, P., Rimoldini, L., Nienartowicz, K., de Fombelle, G. J., Holl, B., Ábrahám, P., Audard, M., Carnerero, M. I., Clementini, G., Ridder, J. D., et al. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202244367 · Cited by 58
A Comparative Study of the Magnetic Activities of Low-mass Stars from M-type to G-type
Lin, C.-L., Ip, W.-H., Hou, W.-J., Huang, L.-C., & Chang, H.-Y. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab041c · Cited by 60
X-Ray Superflares from Pre-main-sequence Stars: Flare Energetics and Frequency
Getman, K. V., & Feigelson, E. D. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/ac00be · Cited by 66
Reconnection Fluxes in Eruptive and Confined Flares and Implications for Superflares on the Sun
Tschernitz, J., Veronig, A. M., Thalmann, J. K., Hinterreiter, J., & Pötzi, W. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aaa199 · Cited by 59
“…such extrapolation that is well grounded by observed solar quantities also allows us to place the strongest flares expected from the present day’s Sun in context to “superflares” on solar-like stars that have been recently discovered in Kepler data (Maehara et al. 2012; Shibayama et al. 2013).”
BackgroundStatistical Analysis of Stellar Flares from the First Three Years of TESS Observations
Pietras, M., Falewicz, R., Siarkowski, M., Bicz, K., & Preś, P. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac8352 · Cited by 56
“For this reason, they have lower values than for the first method, which is based on Shibayama et al. (2013).”
BackgroundMethodResultInfluentialProperties of flare events based on light curves from the TESS survey
Yang, Z., Zhang, L., Meng, G., Han, X. L., Misra, P., Yang, J., & Pi, Q. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202142710 · Cited by 62
NGTS-7Ab: an ultrashort-period brown dwarf transiting a tidally locked and active M dwarf
Jackman, J. A. G., Wheatley, P. J., Bayliss, D., Gill, S., Hodgkin, S. T., Burleigh, M. R., Braker, I. P., Günther, M. N., Louden, T., Turner, O., et al. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz2496 · Cited by 55
Oscillations in stellar superflares
Balona, L. A., Broomhall, A.-M., Kosovichev, A. G., Nakariakov, V. M., Pugh, C. E., & Doorsselaere, T. V. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv661 · Cited by 50
“More recently, Shibayama et al. (2013) found superflares on 279 G dwarfs.”
BackgroundStellar flares detected with the Next Generation Transit Survey
Jackman, J. A. G., Wheatley, P. J., Acton, J. S., Anderson, D. R., Bayliss, D., Briegal, J. T., Burleigh, M. R., Casewell, S. L., Gänsicke, B. T., Gill, S., et al. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab979 · Cited by 56
From Starspots to Stellar Coronal Mass Ejections—Revisiting Empirical Stellar Relations
Herbst, K., Papaioannou, A., Airapetian, V. S., & Atri, D. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/abcc04 · Cited by 59
Llamaradas Estelares: Modeling the Morphology of White-light Flares
Mendoza, G. T., Davenport, J. R. A., Agol, E., Jackman, J. A. G., & Hawley, S. L. (2022) · The Astronomical Journal · doi:10.3847/1538-3881/ac6fe6 · Cited by 53
Vida, K., Oláh, K., Kővári, Z., van Driel-Gesztelyi, L., Moór, A., & Pál, A. (2019) · Repository of the Academy's Library (Library of the Hungarian Academy of Sciences) · Cited by 53
Pedersen, M. G., Antoci, V., Korhonen, H., White, T. R., Jessen-Hansen, J., Lehtinen, J. J., Nikbakhsh, S., & Viuho, J. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw3226 · Cited by 52
“In order to obtain an upper boundary for the flare energy and amplitude in this magnitude range, we carried out a flare detection and parameter determination for one of the G–type superflare stars (KIC 9603367) listed in Shibayama et al. (2013).”
MethodImpact of Stellar Superflares on Planetary Habitability
Yamashiki, Y. A., Maehara, H., Airapetian, V., Notsu, Y., Sato, T., Notsu, S., Kuroki, R., Murashima, K., Sato, H., Namekata, K., et al. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab2a71 · Cited by 63
Self-citationRotation-activity relations and flares of M dwarfs with K2 long- and short-cadence data
Raetz, S., Stelzer, B., Damasso, M., & Scholz, A. (2020) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201937350 · Cited by 54
Flare-productive active regions
Toriumi, S., Wang, H., & 鳥海, 森. (2019) · JAXA Repository (JAXA) · Cited by 49
The Dehydration of Water Worlds via Atmospheric Losses
Dong, C., Huang, Z., Lingam, M., Tóth, G., Gombosi, T., & Bhattacharjee, A. (2017) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/aa8a60 · Cited by 51
“It is well-known that space weather events, such as coronal mass ejections (CMEs), occur frequently on young Sun-like stars (Shibayama et al. 2013).”
BackgroundFinding flares in Kepler data using machine-learning tools
Vida, K., & Roettenbacher, R. M. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201833194 · Cited by 49
“These events can be found in almost all types of main-sequence stars, including hot and cool stars (Švanda & Karlický 2016; Shibayama et al. 2013); but flares are most numerous in low-mass, late-type M dwarfs (Walkowicz et al. 2011; Vida et al. 2016).”
BackgroundMagnetic Activities of M-type Stars Based on LAMOST DR5 and Kepler and K2 Missions
Lu, H., Zhang, L., Shi, J., Han, X. L., Fan, D., Long, L., & Pi, Q. (2019) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/ab2f8f · Cited by 48
Short-duration Stellar Flares in GALEX Data
Brasseur, C. E., Osten, R. A., & Fleming, S. W. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab3df8 · Cited by 49
Tuning the Exospace Weather Radio for Stellar Coronal Mass Ejections
Alvarado-Gómez, J. D., Drake, J. J., Fraschetti, F., Garraffo, C., Cohen, O., Vocks, C., Poppenhäger, K., Moschou, S. P., Yadav, R. K., & Manchester, W. B., IV (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab88a3 · Cited by 48
“…see Yashiro & Gopalswamy 2009, Compagnino et al. 2017), combined with the enhanced stellar flare rates and energies (e.g., Kashyap et al. 2002, Caramazza et al. 2007, Shibayama et al. 2013, Loyd et al. 2018), are expected to yield enough type II burst events in active stars to secure detections.”
Background10 Years of Stellar Activity for GJ 1243
Davenport, J. R. A., Mendoza, G. T., & Hawley, S. L. (2020) · The Astronomical Journal · doi:10.3847/1538-3881/ab9536 · Cited by 48
“Flare frequency distribution (FFD) diagrams have been used to compare the occurrence rate of flares on stars as a function of flare energy (e.g. Lacy et al. 1976; Shibayama et al. 2013).”
MethodSun-as-a-star Analyses of Various Solar Active Events Using Hα Spectral Images Taken by SMART/SDDI
Otsu, T., Asai, A., Ichimoto, K., Ishii, T. T., & Namekata, K. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac9730 · Cited by 50
“In recent years, superflares—which are stellar flares emitting more than 1033 erg—have been observed even in stars similar to the Sun (Maehara et al. 2012; Shibayama et al. 2013; Tu et al. 2020; Okamoto et al. 2021).”
BackgroundSelf-citationCan Flare Loops Contribute to the White-light Emission of Stellar Superflares?
Heinzel, P., & Shibata, K. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aabe78 · Cited by 47
“The former case is usually used in the literature as approximation (Shibayama et al. (2013)), in this study we assume that Ibg = Ispot.”
BackgroundMethodSelf-citationJackman, J., Wheatley, P., Pugh, C., Kolotkov, D., Broomhall, A., Kennedy, G., Murphy, S., Raddi, R., Burleigh, M., Casewell, S., et al. (2018) · Monthly notices of the Royal Astronomical Society · doi:10.1093/mnras/sty3036 · Cited by 31
“This energy is greater than all M dwarf flares observed with Kepler by Yang et al. (2017) and it is comparable to that emitted by the highest energy G star superflares (e.g. Shibayama et al. 2013; Wu, Ip & Huang 2015).”
MethodResultGaia Data Release 2. Variable stars in the colour-absolute magnitude diagram
Eyer, L., Rimoldini, L., Audard, M., Anderson, R. I., Nienartowicz, K., Glass, F., Marchal, O., Grenon, M., Mowlavï, N., Holl, B., et al. (2019) · LA Referencia (Red Federada de Repositorios Institucionales de Publicaciones Científicas) · doi:10.17863/cam.38302 · Cited by 46
Extreme Solar Events: Setting up a Paradigm
USOSKIN, I. G., Miyake, F., Baroni, M., Brehm, N., Dalla, S., Hayakawa, H., Hudson, H. S., Jull, A. J. T., Knipp, D. J., Koldobskiy, S., et al. (2023) · Space Science Reviews · doi:10.1007/s11214-023-01018-1 · Cited by 63
Self-citationWHITE-LIGHT FLARES ON CLOSE BINARIES OBSERVED WITH KEPLER
Gao, Q., Xin, Y., Liu, J., Zhang, X.-B., & Gao, S. (2016) · The Astrophysical Journal Supplement Series · doi:10.3847/0067-0049/224/2/37 · Cited by 47
“…three main criteria: (1) binaries with neighboring stars within 12 arcsec are excluded to avoid false events from the flux of the neighboring stars (Shibayama et al. 2013); (2) the orbital period is longer than 0.4 days, since the light curves with periods of less than 0.4 days are…”
BackgroundMethodResultInfluentialA census of coronal mass ejections on solar-like stars
Leitzinger, M., Odert, P., Greimel, R., Vida, K., Kriskovics, L., Guenther, E. W., Korhonen, H., Koller, F., Hanslmeier, A., Kővári, Z., et al. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa504 · Cited by 46
Detection of Flare-induced Plasma Flows in the Corona of EV Lac with X-Ray Spectroscopy
Chen, H., Tian, H., Li, H., Wang, J.-G., 陆洪鹏, H. L., 徐昱, Y. X., Hou, Z., & 吴昱川, Y. W. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac739b · Cited by 45
“…observations (e.g., Neupert 1968; Dennis & Zarro 1993; Hawley et al. 1995; Güdel et al. 1996) and recent parameter analyses (Notsu et al. 2013; Shibayama et al. 2013; Maehara et al. 2017; Namekata et al. 2017; Yan et al. 2021), stellar flares are generally assumed to be caused by the same…”
BackgroundSiegert, T. (2023) · Astrophysics and Space Science · doi:10.1007/s10509-023-04184-4 · Cited by 45
“From Kepler and TESS measurements (e.g., Shibayama et al. 2013), it is known that also other stars flare in a similar fashion as the Sun, with a flare-frequency-energy-distribution of dN dEdt ≈ 10−29 ( E 1030 erg )−1.8 erg−1 yr−1.”
BackgroundInfluentialACTIVITY ANALYSES FOR SOLAR-TYPE STARS OBSERVED WITH KEPLER . I. PROXIES OF MAGNETIC ACTIVITY
He, H., Wang, H., & Yun, D. (2015) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/221/1/18 · Cited by 44
“We selected the star samples based on the Kepler superflare starlist given by Shibayama et al. (2013); the stars in this list (279 G-type stars in total) had been identified with superflare spikes (flare energy greater than 1033 erg) in their light curves (Notsu et al. 2013b; Shibayama et al. 2013;…”
BackgroundMethodInfluentialModelling stellar proton event-induced particle radiation dose on close-in exoplanets
Atri, D. (2016) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1093/mnrasl/slw199 · Cited by 45
“In general large superflares are more frequent by a factor of 20 on M and 6 on K-type stars compared to G-type stars(Shibayama et al. 2013).”
BackgroundNandy, D., Martens, P. C. H., Обридко, В. Н., Dash, S., & Georgieva, K. (2021) · Progress in Earth and Planetary Science · doi:10.1186/s40645-021-00430-x · Cited by 60
“13), including many solar-like stars, showed that faster rotating stars are statistically more likely to produce stellar superflares with energies as high as 1036 erg with a higher frequency (Maehara et al. 2012; Shibayama et al. 2013; Notsu et al. 2013).”
BackgroundKeplersuper-flare stars: what are they?
Wichmann, R., Fuhrmeister, B., Wolter, U., & Nagel, E. (2014) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201423717 · Cited by 43
“We note that Shibayama et al. 2013 prefer the shorter period and list 7.7 days for this star.”
BackgroundInfluentialNotsu, Y., Kowalski, A. F., Maehara, H., Namekata, K., Hamaguchi, K., Enoto, T., Tristan, I. I., Hawley, S. L., Davenport, J. R. A., Honda, S., et al. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad062f · Cited by 49
Self-citation
Metadata
- Authors
- Shibayama, T., Maehara, H., Notsu, S., Notsu, Y., Nagao, T., Honda, S., Ishii, T. T., Nogami, D., & Shibata, K.
- Affiliations
- Kyoto University (JP)
- University of Hyogo (JP)
- Corresponding author
- Shibayama, Takuya
- Venue
- The Astrophysical Journal Supplement Series
- Publisher
- American Astronomical Society
- Published
- 2013-10-17
- Volume
- 209
- Issue
- 1
- Pages
- 5
- ISSN
- 0067-0049 (ISSN-L)
- 1538-4365
- OpenAlex
- W2052980643
- Cited by
- 500
- References
- 43
- Citations by year
- 2026: 26 · 2025: 50 · 2024: 51 · 2023: 45 · 2022: 47 · 2021: 35 · 2020: 37 · 2019: 40 · 2018: 71 · 2017: 20 · 2016: 29 · 2015: 29 · 2014: 19
- FWCI
- 13.86
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Licence
- Locations
- The Astrophysical Journal Supplement Series (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- arXiv (Cornell University)
- Funders
- Japan Society for the Promotion of Science (25287039)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Solar and Space Plasma Dynamics
- Physical Sciences › Physics and Astronomy › Instrumentation › Astronomy and Astrophysical Research
- Keywords
- superflares, solar-type stars, flare occurrence rate, flare energy distribution, power-law distribution, stellar brightness variations, stellar activity, stellar spots, stellar magnetic activity
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