Cited by 500Stellar, planetary, and galactic studiesSolar and Space Plasma DynamicsAstronomy and Astrophysical Research

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SUPERFLARES ON SOLAR-TYPE STARS OBSERVED WITH KEPLER . I. STATISTICAL PROPERTIES OF SUPERFLARES

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Shibayama, Takuya, Maehara, Hiroyuki, Notsu, Shota, Notsu, Yuta, Nagao, Takashi, Honda, Satoshi, Ishii, Takako T., Nogami, Daisaku, Shibata, Kazunari·2013·The Astrophysical Journal Supplement Series

DOI 10.1088/0067-0049/209/1/5

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Abstract

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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Self-citation
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NGTS clusters survey – II. White-light flares from the youngest stars in Orion
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Background
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“For KIC07133671, we could find a period of 15.19 d, which is consistent with Shibayama et al. (2013).”
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Background
Exploring the Origin of Multi‐Periodic Pulsations During a White‐Light Flare
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“Therefore, the WLF is often detected in the powerful ﬂare on the Sun (Zhao et al., 2021), or it can be observed in the superﬂare in solar-type stars (Shibayama et al., 2013; Y. Yan et al., 2021).”
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“This work was later extended by Shibayama et al. (2013) and others.”
Background
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Background
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Черенков, А. А., Шайхисламов, И. Ф., Bisikalo, D. V., Shematovich, V. I., Fossati, L., & Möstl, C. (2019) · Astronomy Reports · doi:10.1134/s1063772919020033 · Cited by 11
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Vasilyev, V., Reinhold, T., Shapiro, A. I., Krivova, N. A., USOSKIN, I. G., Montet, B. T., Solanki, S. K., & Gizon, L. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202244422 · Cited by 15
“…large photometric surveys, in particular the Kepler mission, it became clear that flares are a common phenomenon on cool stars (Walkowicz et al. 2011; Maehara et al. 2012; Shibayama et al. 2013; Davenport 2016; Van Doorsselaere et al. 2017; Yang & Liu 2019; Günther et al. 2020; Ilin et al. 2021).”
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Li, G., Wu, C., Zhou, G., Chen, Y., Li, H.-L., Chen, J., Xin, L. P., Wang, J., Haerken, H., Ma, C.-H., et al. (2022) · Research in Astronomy and Astrophysics · doi:10.1088/1674-4527/aca506 · Cited by 12
Observed Rate Variations in Superflaring G-type Stars
Crowley, J., Wheatland, M. S., & Yang, K. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/aca476 · Cited by 12
“The power-law fits for stellar superflares have been observed to have similar indices to the power-law fits for solar flares (Shibayama et al. 2013; Maehara et al. 2015; Davenport 2016; Tu et al. 2021).”
Background
Minute-cadence observations of the LAMOST fields with the TMTS – III. Statistical study of the flare stars from the first two years
Liu, Q., Lin, J., Wang, X., Gu, S., Shi, J., Zhang, L., Xi, G., Mo, J., Cai, Y., Chen, L., et al. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad365 · Cited by 10
“Following the analysis of Shibayama et al. (2013) and Lin et al. (2022b), we assume the flare emission as a blackbody, then we have the observed flare luminosity 𝐿′flare and the star luminosity 𝐿′star as 𝐿′flare = 𝐴flare ∫ 𝐵𝜆 (𝑇flare)𝑅𝜆𝑑𝜆.”
BackgroundResult
A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Rekhi, P., Ben-Ami, S., Perdelwitz, V., & Shvartzvald, Y. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/ace5ac · Cited by 10
Far-ultraviolet Flares on Accreting Protostars: Weak and Classical T Tauri Stellar Pair Analysis
Hinton, P. C., France, K. C., Batista, M. G., Serna, J., Hernández, J., Günther, H. M., Kowalski, A. F., & Schneider, P. C. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac8f26 · Cited by 10
“We find an average flare energy of 6.48× 1035 erg across all observed flares, which is higher than that reported for nearby main-sequence stars (e.g., M dwarfs, Günther et al. 2020; G-type dwarfs, Shibayama et al. 2013).”
ResultInfluential
Long-term solar variability: ISWAT S1 cluster review for COSPAR space weather roadmap
Pevtsov, A. A., Nandy, D., USOSKIN, I. G., Pevtsov, A., Corti, C., Lefèvre, L., Owens, M. J., Li, G., Krivova, N. A., Saha, C., et al. (2023) · Advances in Space Research · doi:10.1016/j.asr.2023.08.034 · Cited by 10
Flare Activity and Magnetic Feature Analysis of the Flare Stars
Goodarzi, H., Mehrabi, A., Khosroshahi, H. G., & He, H. (2019) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/ab44cd · Cited by 10
“…flare luminosity (Lflare) is calculated from temperature and area of the flares ( Tflare and Aflare, respectively) using the following equation (Shibayama et al. 2013), Lflare = σSBT 4 flareAflare , (7) where σSB is the Stefan-Boltzmann constant and we assume Tflare to be 9000K as the spectral…”
Influential
High-time-cadence Spectroscopy and Photometry of Stellar Flares on M dwarf YZ Canis Minoris with the Seimei Telescope and TESS. I. Discovery of Rapid and Short-duration Prominence Eruptions
Kajikiya, Y., Namekata, K., Notsu, Y., Maehara, H., Sato, B., & Nogami, D. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/ad91b9 · Cited by 9
Self-citation
Self-organized Criticality across 13 Orders of Magnitude in the Solar–Stellar Connection
Aschwanden, M. J., & Schrijver, C. J. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/addc58 · Cited by 9
Do Young Suns Produce Frequent, Massive CMEs? Results from Five-year Dedicated Optical Observations of EK Draconis and V889 Hercules
Namekata, K., Maehara, H., Notsu, Y., Honda, S., Ikuta, K., Nogami, D., & Shibata, K. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/adfe70 · Cited by 17
“The bolometric white-light (WL) flare energy is calculated following the methodology described in T. Shibayama et al. (2013).”
Self-citation
TESS Photometric Variability of Young Brown Dwarfs in the Taurus Star-forming Region
Kumbhakar, R., Mondal, S., Ghosh, S., & Ram, D. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/aceb65 · Cited by 9
Four New Horsemen of an Apocalypse? Solar Flares, Super-volcanoes, Pandemics, and Artificial Intelligence
Noy, I., & Uher, T. (2022) · Economics of Disasters and Climate Change · doi:10.1007/s41885-022-00105-x · Cited by 11
“Maehara et al. (2012) note that flares of such magnitude occur on sun-like stars every 800 years, similarly to Shibayama et al. (2013).”
Background
The GAPS programme at TNG
Maio, C. D., Argiroffi, C., Micela, G., Benatti, S., Lanza, A. F., Scandariato, G., Maldonado, J., Maggio, A., Affer, L., & Claudi, R. (2020) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202038011 · Cited by 9
Hydrogen recombination continua in stellar flares
Heinzel, P. (2024) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1093/mnrasl/slae046 · Cited by 8
Application of Convolutional Neural Networks to time domain astrophysics. 2D image analysis of OGLE light curves
Monsalves, N., Arancibia, M. J., Bayo, A., Sanchéz-Sáez, P., Angeloni, R., Damke, G. J., & de Perre, J. S. V. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202449995 · Cited by 10
Magnetic Activities of AD Leonis: Flares in TESS Data and Optical Spectra
Ram, D., Mondal, S., Patra, D., Ghosh, S., & Kumbhakar, R. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/adabc3 · Cited by 8
Simultaneous Optical and Radio Observations of a Large Stellar Flare on EV Lac
Lu, H., Zhang, J., Tian, H., Zhang, L., Chen, H., Zheng, J., Zhang, J., Wang, J.-G., Inoue, S., Maehara, H., et al. (2025) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/adfc5b · Cited by 9
Self-citation
Observation of a possible superflare on Proxima Centauri
Kielkopf, J. F., Hart, R., Carter, B., & Marsden, S. C. (2019) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1093/mnrasl/slz054 · Cited by 6
Earliest datable records of aurora-like phenomena in the astronomical diaries from Babylonia
Hayakawa, H., Mitsuma, Y., Ebihara, Y., Kawamura, A. D., Miyahara, H., Tamazawa, H., & Isobe, H. (2016) · Institutional Repositories DataBase (IRDB) · Cited by 8
Solar and Stellar Flares: Frequency, Active Regions, and Stellar Dynamo
Katsova, M. M., Обридко, В. Н., Sokoloff, D. D., & Livshits, I. M. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac85e3 · Cited by 8
“…powerful nonstationary stellar phenomena was introduced when the first results of the Kepler mission, which operated in 2009–2018 and detected huge flares on G-type stars, were published (Maehara et al. 2012; Shibayama et al. 2013; Maehara et al. 2015; Namekata et al. 2019; Okamoto et al. 2021a).”
Background
Coronal Heating as Determined by the Solar Flare Frequency Distribution Obtained by Aggregating Case Studies
Mason, J. P., Werth, A., West, C. G., Youngblood, A. A., Woodraska, D. L., Peck, C. L., Aradhya, A. J., Cai, Y., Chaparro, D., Erikson, J. W., et al. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/accc89 · Cited by 15
“We also know that flares of all energies (including superflares with >1034 erg) tend to occur more often for rapidly rotating stars (Maehara et al. 2012; Shibayama et al. 2013).”
Background
Spectroscopic observations of flares and superflares on AU Mic
Odert, P., Leitzinger, M., Greimel, R., Kábath, P., Lipták, J., Heinzel, P., Karjalainen, R., Wollmann, J., Guenther, E. W., Skarka, M., et al. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae2752 · Cited by 9
Statistical Signatures of Nanoflare Activity. II. A Nanoflare Explanation for Periodic Brightenings in Flare Stars Observed by NGTS
Dillon, C. J., Jess, D. B., Mathioudakis, M., Watson, C. A., Jackman, J. A. G., Wheatley, P. J., Goad, M. R., Casewell, S. L., Anderson, D. R., Burleigh, M. R., et al. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/abbfa8 · Cited by 8
Change in the activity character of the coronae of low-mass stars of various spectral types
Nizamov, B. A., Katsova, M. M., & Livshits, M. A. (2017) · Astronomy Letters · doi:10.1134/s1063773717020049 · Cited by 8
“The present investigation is initiated by the discovery onboard the Kepler spacecraft of the powerful optical radiation in the course of non-stationary processes on low-mass late-type stars (Maehara et al. 2012, Shibayama et al. 2013).”
BackgroundMethodResult
Properties of Kepler Stars with the Most Powerful Flares
Katsova, M. M., & Nizamov, B. A. (2018) · Geomagnetism and Aeronomy · doi:10.1134/s0016793218070095 · Cited by 8
“In the dedicated G dwarf investigation (Maehara et al., 2012, Shibayama et al., 2013), the discovery of powerful flares with energies in excess of 1033 erg is presented; it is based on the observations of almost 83000 stars where 365 superflares were detected in 120 days in 148 solar type stars.”
Background
Very Long-periodic Pulsations Detected Simultaneously in a White-light Flare and Sunspot Penumbra
Li, D., Wang, J., & Huang, Y. (2024) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ad6cde · Cited by 7
“This type of WLF appears to be easily seen in powerful ﬂares on the Sun (Zhao et al. 2021; Li et al. 2023b), and they are also frequently observed in superﬂares in solar-type stars (Shibayama et al. 2013; Yan et al. 2021) since they both release a large amount of energies.”
Background
Optically quiet, but FUV loud: results from comparing the far-ultraviolet predictions of flare models with TESS and HST
Jackman, J. A. G., Shkolnik, E. L., Loyd, R. O. P., & Richey-Yowell, T. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae1570 · Cited by 7
LEIA Discovery of the Longest-lasting and Most Energetic Stellar X-Ray Flare Ever Detected
Mao, X., Liu, H., Wang, S., Ling, Z., Yuan, W., Cheng, H., Pan, H., Li, D., Favata, F., Ji, T., et al. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/ada698 · Cited by 14
“…over ten to a million times the energy of the largest solar flares ( ∼ 10 32 erg; Emslie et al. 2012) and have been observed in various stars (e.g., Maehara et al. 2012; Shibayama et al. 2013; Candelaresi et al. 2014; Hawley et al. 2014; Davenport 2016; Notsu et al. 2019; Okamoto et al. 2021).”
Particle acceleration in space: a universal mechanism?
Panasyuk, M. I., & Miroshnichenko, L. I. (2021) · Uspekhi Fizicheskih Nauk · doi:10.3367/ufnr.2021.07.039022 · Cited by 7
Blackbody Temperature of 200+ Stellar Flares Observed with the CoRoT Satellite
Rabello-Soares, M. C., de Freitas, M. C., & Ferreira, B. P. L. (2022) · The Astronomical Journal · doi:10.3847/1538-3881/ac90cb · Cited by 9
“Following Shibayama et al. (2013), we can estimate the flare luminosity (Lflare) observed by CoRoT in the White channel, in photons, as: Lflare(t) = Aflare(t) ∫ ∞ 0 Φ(λ)Bλ(Tflare)λ dλ (4) where Aflare(t) is the area of the flare as a function of time and Φ(λ) is CoRoT Response Function for…”
BackgroundMethodInfluential
Simultaneous X-ray and optical variability of M dwarfs observed with eROSITA and TESS
Joseph, W. M., Stelzer, B., Magaudda, E., & Martínez, T. V. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202449405 · Cited by 7
The White-light Superflares from Cool Stars in GWAC Triggers
Li, G.-W., 王, L. 靓. W., Yuan, H., Xin, L. P., 王, J. 竞. W., Wu, C., Li, H.-L., Haerken, H., Wang, W., Cai, H., et al. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad55e8 · Cited by 8
“…#44 (GWAC190204A), #49 (GWAC211203A), #86 (GWAC210117A), #117 (GWAC190116B) and #120 (GWAC190117A), their flare energies were calculated from their K2 light curves, so the method in Shibayama et al. (2013) was used, with stellar radii and surface temperatures from Huber et al. (2016).”
Method
Analysis of the Stellar Occultations during the Unprecedented Long-duration Flare
Bicz, K., Falewicz, R., Heinzel, P., Pietras, M., & Preś, P. (2024) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ad6c06 · Cited by 7
“Using the flaring region size from Paper I, with the assumption that the flaring region size is constant in time, we were able to estimate how the temperature of the flaring region changes using the modified method by us from Shibayama et al. (2013).”
Method
Preparing for the Early eVolution Explorer: Characterizing the Photochemical Inputs and Transit Detection Efficiencies of Young Planets Using Multiwavelength Flare Observations by TESS and Swift
Howard, W. S., MacGregor, M. A., Feinstein, A. D., Vega, L. D., Cody, A. M., Turner, N. J., Scott, V., Burt, J., & Venuti, L. (2024) · The Astronomical Journal · doi:10.3847/1538-3881/ad93ce · Cited by 7
Photometric Stellar Parameters for 195,478 Kepler Input Catalog Stars
Zhang, B., Huang, Y., Beers, T. C., Xiao, K., Liu, J., Jia, L., Han, H., Li, Z., Zheng, C., Sun, Y., et al. (2025) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/ada3ba · Cited by 7
“…advanced the field of exoplanet search and characterization, but also provided an important basis for research in many other fields, including stellar activity, astroseismology, and the study of star clusters (Gilliland et al. 2010; Shibayama et al. 2013; McQuillan et al. 2014; Borucki 2016).”
Solar extreme events
Hudson, H. S. (2015) · Journal of Physics Conference Series · doi:10.1088/1742-6596/632/1/012058 · Cited by 8
Particle acceleration in space: a universal mechanism?
Panasyuk, M. I., & Miroshnichenko, L. I. (2021) · Physics-Uspekhi · doi:10.3367/ufne.2021.07.039022 · Cited by 7
AstroSat observations of long-duration X-ray superflares on active M-dwarf binary EQ Peg
Karmakar, S., Naik, S., Pandey, J. C., & Savanov, I. S. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab3099 · Cited by 12
Quasi-periodic pulsations in solar and stellar flares. Review
Kupriyanova, E. G., Kolotkov, D. Y., Nakariakov, V. M., & Kaufman, A. (2020) · Solnechno-Zemnaya Fizika · doi:10.12737/szf-61202001 · Cited by 7
Study of the energetic X-ray superflares from the active fast rotator AB doradus
Didel, S., Pandey, J. C., Srivastava, A. K., & Singh, G. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad3245 · Cited by 10
Variability of Superflare Frequency of Sun Like Stars
Акопян, А. А. (2015) · Astrophysics · doi:10.1007/s10511-015-9366-9 · Cited by 7
Activity of the sun in the age of 1–2 Gyr
Katsova, M. M., & Livshits, M. A. (2014) · Geomagnetism and Aeronomy · doi:10.1134/s0016793214080088 · Cited by 7
“9 in Shibayama et al. (2013) we obtain the fre quency of such events 3 × 10–26 erg–1 star–1 year–1.”
Flare Properties of A-type Stars in Kepler Data
Bai, J., & Esamdin, A. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/abc479 · Cited by 7
Soft X-ray heating as a mechanism of optical continuum generation in solar-type star superflares
Nizamov, B. A. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz2478 · Cited by 7
“They found that 40% of the stars reported by Shibayama et al. (2013) are subgiants.”
Background
Flaring activities of fast rotating stars have a solar-like latitudinal distribution
Yang, H., Cheng, X., Liu, J., Liu, S., Zhao, Z., Zhou, G., Hou, Y., Gao, C., & Niu, Z. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202453120 · Cited by 6
Sun-as-a-star Analysis of the Solar Eruption Source Region Using H α Spectroscopic Observations of CHASE
Liu, X., Hou, Y., Li, Y., Qiu, Y., Li, T., Cai, Y., Rao, S., Zhang, J., & Li, C. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/ae0743 · Cited by 7
“Statistical analyses have shown that the majority of stellar flares observed on solar-type stars are superflares, with energies exceeding 10 33 erg (Maehara et al. 2012, Shibayama et al. 2013, Zhao et al. 2024).”
The M4.5V flare star AF Psc as seen in K2 engineering data
Ramsay, G., & Doyle, J. G. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu1063 · Cited by 5
“For instance, Balona (2012) reported observations of flares from stars with early A and F spectral types, while Maehara et al. (2012) and Shibayama et al. (2013) report ‘super-flares’ from Solar type stars.”
Background
Convolutional Neural Networks for Searching Superflares from Pixel-level Data of the Transiting Exoplanet Survey Satellite
Tu, Z.-L., Wu, Q., Wang, W., Zhang, G. Q., Liu, Z.-K., & Wang, F. Y. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac7f2c · Cited by 6
“We select solar-type stars according to the following criteria: (1) stellar effective temperature (Teff), 5100 K Teff< 6000 K, and (2) surface gravity ( glog ), >glog 4.0 (e.g., Shibayama et al. 2013; Maehara et al. 2015; Tu et al. 2020, 2021).”
MethodInfluential
Analysis of Solar-like X-class Flare on Wolf 359 Observed Simultaneously with TESS and XMM-Newton
Pietras, M., Falewicz, R., Siarkowski, M., Kępa, A., Bicz, K., & Preś, P. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/ace69a · Cited by 6
Unveiling the spectacular over 24-hour flare of star CD-36 3202
Bicz, K., Falewicz, R., & Pietras, M. (2023) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202347901 · Cited by 6

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
ORCID: Notsu, Shota
Notsu, Yuta
Nogami, Daisaku
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
DOI: 10.1088/0067-0049/209/1/5
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: iopscience.iop.org/info/page/text-and-data-mining (tdm)
iopscience.iop.org/page/copyright (vor)
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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SUPERFLARES ON SOLAR-TYPE STARS OBSERVED WITH KEPLER . I. STATISTICAL PROPERTIES OF SUPERFLARES

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