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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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Items 101–200 of 496
Two sun-like superflare stars rotating as slow as the Sun
Nogami, D., Notsu, Y., Honda, S., Maehara, H., Notsu, S., Shibayama, T., & Shibata, K. (2014) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psu012 · Cited by 45
“The analyses of the Kepler data by Maehara et al. (2012) and Shibayama et al. (2013) revealed that the relation between the occurrence frequency of the flare and the flare energy in the Sun can be roughly extended for the flare energy up to ∼ 1036 erg on superflare stars.”
BackgroundMethodInfluentialSelf-citationSimultaneous Kepler/K2 and XMM-Newton observations of superflares in the Pleiades
Guarcello, M. G., Micela, G., Sciortino, S., López‐Santiago, J., Argiroffi, C., Reale, F., Flaccomio, E., Alvarado‐Gómez, J. D., Antoniou, V., Drake, J. J., et al. (2019) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201834370 · Cited by 41
Physics of Space Weather Phenomena: A Review
Singh, A. K., Bhargawa, A., Siingh, D., & Singh, R. P. (2021) · Geosciences · doi:10.3390/geosciences11070286 · Cited by 49
Impact of space weather on climate and habitability of terrestrial-type exoplanets
Airapetian, V., Gopalswamy, N., Grenfell, J. L., Gronoff, G., Güdel, M., Herbst, K., Henning, W. G., Jackman, C. H., Jin, M., Johnstone, C. P., et al. (2020) · Yokohama National University Repository (Yokohama National University) · Cited by 41
Self-citationModeling a Carrington-scale Stellar Superflare and Coronal Mass Ejection from
Lynch, B. J., Airapetian, V. S., Devore, C. R., Kazachenko, M. D., Lüftinger, T., Kochukhov, O., Rosén, L., & Abbett, W. P. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab287e · Cited by 41
Namekata, K., Maehara, H., Honda, S., Notsu, Y., Okamoto, S., Takahashi, J., Takayama, M., Ohshima, T., Saito, T., Katoh, N., et al. (2022) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ac4df0 · Cited by 47
“…young, solar-type stars show frequent superflares (age of ∼100 Myr; Audard et al. 1999) but also that slowly rotating, old solar-type stars show superflares with low-occurrence frequencies (ages of several Gyr; Maehara et al. 2012; Shibayama et al. 2013; Notsu et al. 2019; Okamoto et al. 2021).”
BackgroundMethodSelf-citationInoue, S., Maehara, H., Notsu, Y., Namekata, K., Honda, S., Namizaki, K., Nogami, D., & Shibata, K. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acb7e8 · Cited by 45
“By setting the flux of Figure 2(a) to C flare¢ (= luminosity of flare/luminosity of star) in the Equation (5) of Shibayama et al. (2013), we estimated the flare area Aflare as follows: { } ( ) ( ) ( ) ( ) ( )A t C t R R B T d R B T d 1 i i i flare flare 1,2 2 flare ò ò p l l = ¢ å l l l l = where λ…”
BackgroundMethodSelf-citationSelf-organized Criticality in Stellar Flares
Aschwanden, M. J., & Güdel, M. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/abdec7 · Cited by 45
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/psv001 · Cited by 40
“These four superflare stars were not included in Shibayama et al. (2013), as they are not classified as solar-type stars on the basis of the Kepler Input Catalog (KIC: Brown et al. 2011).”
BackgroundMethodInfluentialSelf-citationNew Insights into Cosmic-Ray-induced Biosignature Chemistry in Earth-like Atmospheres
Scheucher, M., Grenfell, J. L., Wunderlich, F., Godolt, M., Schreier, F., & Rauer, H. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aacf03 · Cited by 42
Ikuta, K., Namekata, K., Notsu, Y., Maehara, H., Okamoto, S., Honda, S., Nogami, D., & Shibata, K. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acbd36 · Cited by 42
“According to Shibayama et al. (2013), the bolometric flare energy is formulated as ò ò ò ò s p l l l l l l = = ´ ´ ´ D ( ) ( ) ( ) ( ) ( ) ( ) ( ) E L t dt T R R B T d R B T d F F t dt 2 , , , 1 flare flare SB flare 4 star 2 eff flare where ( )L tflare and ΔF/F(t) are the bolometric luminosity…”
BackgroundSelf-citationThe host stars ofKepler's habitable exoplanets: superflares, rotation and activity
Armstrong, D. J., Pugh, C. E., Broomhall, A.-M., Brown, D. J. A., Lund, M. N., Osborn, H. P., & Pollacco, D. L. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv2419 · Cited by 37
“Estimates of the flare energies were made using the flare amplitude, duration, and luminosity, and were done in a similar manner to Shibayama et al. (2013).”
MethodHe, H., Wang, H., Zhang, M., Mehrabi, A., Yan, Y., & Yun, D. (2018) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/aab779 · Cited by 35
“For example, in the paper by Shibayama et al. (2013), they extended the pioneer work of Maehara et al. (2012) and compiled a superflare catalog of solar-type (G-type) stars based on the observational data of Kepler.”
BackgroundMethodInfluentialThe Propitious Role of Solar Energetic Particles in the Origin of Life
Lingam, M., Dong, C., Fang, X., Jakosky, B. M., & Loeb, A. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aa9fef · Cited by 43
“As we are concerned with the young Sun, expected to have been more active ∼ 4.0 Gya (Güdel 2007), it seems reasonable to assume that it obeyed statistics similar to active G-type stars; the latter are predicted to have a superflare occurrence rate of 0.1 per day (Shibayama et al. 2013).”
BackgroundInfluentialSuperflares on AB Doradus observed with TESS
Schmitt, J. H. M. M., Ioannidis, P., Robrade, J., Czesla, S., & Schneider, P. C. (2019) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201935374 · Cited by 38
“Computing the flare rates and comparing them to the rates derived by Shibayama et al. (2013) yields good agreement (cf., Fig.”
BackgroundResultInfluentialAyres, T. R. (2015) · The Astronomical Journal · doi:10.1088/0004-6256/150/1/7 · Cited by 38
“Now, however, the Kepler Mission has provided more substantive statistics on superflares – although limited to white-light counterparts – from a wide variety of stars, normal and otherwise (e.g., Maehara et al. 2012; Shibayama et al. 2013; Candelaresi et al. 2014).”
BackgroundJackman, J. A. G., Shkolnik, E. L., Million, C., Fleming, S. W., Richey-Yowell, T., & Loyd, R. O. P. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac3135 · Cited by 37
Sun-like stars produce superflares roughly once per century
Vasilyev, V., Reinhold, T., Shapiro, A. I., USOSKIN, I. G., Krivova, N. A., Maehara, H., Notsu, Y., Brun, A. S., Solanki, S. K., & Gizon, L. (2024) · Science · doi:10.1126/science.adl5441 · Cited by 49
Self-citationUsing Extreme Value Theory for Determining the Probability of Carrington‐Like Solar Flares
Elvidge, S., & Angling, M. (2018) · Space Weather · doi:10.1002/2017sw001727 · Cited by 37
Avalanche Statistics Identify Intrinsic Stellar Processes near Criticality in KIC 8462852
Sheikh, M. A., Weaver, R. L., & Dahmen, K. A. (2016) · Physical Review Letters · doi:10.1103/physrevlett.117.261101 · Cited by 39
Was the Sun a Slow Rotator? Sodium and Potassium Constraints from the Lunar Regolith
Saxena, P., Killen, R. M., Airapetian, V., Petro, N. E., Curran, N. M., & Mandell, A. M. (2019) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ab18fb · Cited by 36
On the Size of the Flare Associated with the Solar Proton Event in 774 AD
Cliver, E. W., Hayakawa, H., Love, J. J., & Neidig, D. F. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/abad93 · Cited by 39
HL Dra: an active Algol-like binary system with a pulsating component star and a cool third body
Shi, X.-D., Qian, S. ‐., Li, L.-J., & Liao, W.-P. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab1657 · Cited by 36
Werth, A., West, C. G., & Lewandowski, H. J. (2022) · Physical Review Physics Education Research · doi:10.1103/physrevphyseducres.18.010129 · Cited by 37
Faraday rotation measure variations of repeating fast radio burst sources
Yang, Y.-P., Xu, S., & Zhang, B. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad168 · Cited by 36
Radio signatures of star–planet interactions, exoplanets and space weather
Callingham, J. R., Pope, B. J. S., Kavanagh, R. D., Bellotti, S., Daley-Yates, S., Damasso, M., Grießmeier, J. ‐., Güdel, M., Günther, M. N., Kao, M., et al. (2024) · Nature Astronomy · doi:10.1038/s41550-024-02405-6 · Cited by 45
“However, the Next Generation Very Large Array (ngVLA; 118 ) may be able to detect mass loss from the steady stellar wind of nearby M dwarfs 119 .”
Two Strong White-Light Solar Flares in AR NOAA 12673 as Potential Clues for Stellar Superflares
Romano, P., Elmhamdi, A., & Kordi, A. S. (2019) · Solar Physics · doi:10.1007/s11207-018-1388-0 · Cited by 32
“Notsu et al. (2013) showed that many superflares probably occur in large starspots (10 times larger than the largest sunspot) and that the energy of the superflares can be explained by the magnetic energy stored around such starspots (Shibayama et al., 2013).”
BackgroundA great space weather event in February 1730
Hayakawa, H., Ebihara, Y., Vaquero, J. M., Hattori, K., Carrasco, V. M. S., Gallego, M. C., Hayakawa, S., Watanabe, Y., Iwahashi, K., Tamazawa, H., et al. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201832735 · Cited by 32
Magnetic activity based on LAMOST medium-resolution spectra and the Kepler survey
Zhang, L., Long, L., Shi, J., Lu, H., Gao, Q., Han, X. L., Wang, H., & Misra, P. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa942 · Cited by 34
Sun-as-a-star Spectral Irradiance Observations of Transiting Active Regions
Toriumi, S., Airapetian, V., Hudson, H. S., Schrijver, C. J., Cheung, M. C. M., & DeRosa, M. L. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/abadf9 · Cited by 34
“…ob- Corresponding author: Shin Toriumi toriumi.shin@jaxa.jp servations reveal that similar but much more energetic superflares, with bolometric energies of 1033 to 1036 erg, can happen on slowly-rotating stars like the Sun (Maehara et al. 2012; Shibayama et al. 2013; Notsu et al. 2019).”
BackgroundStellar X-Ray Activity Across the Hertzsprung–Russell Diagram. I. Catalogs
Wang, S., Bai, Y., He, L., & Liu, J. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/abb66d · Cited by 33
Do Long-cadence Data of the Kepler Spacecraft Capture Basic Properties of Flares?
Yang, H., Liu, J., Qiao, E., Zhang, H., Gao, Q., Cui, K., & Han, H. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aabd31 · Cited by 35
“…aspects of stellar physics, such as stellar activity, the mechanism of superflares, stellar structure, the interaction of binary and so on (e.g., Shibayama et al. 2013; Balona 2013; Hawley et al. 2014; Gaulme et al. 2014; Wichmann et al. 2014; Balona 2015; Lurie et al. 2015; Davenport 2016; Gao…”
BackgroundMethodResultInfluentialNamekata, K., Ichimoto, K., Ishii, T. T., & Shibata, K. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac75cd · Cited by 33
“S R ] 3 J un 2 02 2 extreme flares (“superflares”) on our Sun (e.g., Maehara et al. 2012; Schrijver et al. 2012; Shibayama et al. 2013; Shibata et al. 2013; Schrijver et al. 2012; Notsu et al. 2019; Okamoto et al. 2021).”
BackgroundSelf-citationFractal Reconnection in Solar and Stellar Environments
Shibata, K., & Takasao, S. (2016) · Astrophysics and space science library · doi:10.1007/978-3-319-26432-5_10 · Cited by 32
“Shibayama et al. (2013)[93] extended and confirmed the work by Maehara et al. and found 1547 superflares on 279 solar type stars from 500days Kepler data.”
ResultSelf-citationGround-based detection of G star superflares with NGTS
Jackman, J. A. G., Wheatley, P. J., Pugh, C. E., Gänsicke, B. T., Gillen, E., Broomhall, A.-M., Armstrong, D. J., Burleigh, M. R., Chaushev, A., Eigmüller, P., et al. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty897 · Cited by 28
“However, we also calculate the flare duration with two additional methods - using its e-folding timescale (as performed in Shibayama et al. 2013) and its scale time (the duration where the flare is above half the maximum flux value).”
BackgroundMethodInfluentialAtmospheric Mass Loss from Hot Jupiters Irradiated by Stellar Superflares
Бисикало, Д. В., Shematovich, V. I., Черенков, А. А., Fossati, L., & Möstl, C. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aaed21 · Cited by 30
“Analyses conducted on the basis of Kepler 1-minute cadence observations (Maehara et al. 2012, 2015; Shibayama et al. 2013) revealed that flares are found ubiquitously among late-type stars.”
MethodDurán, J. S. C., & Kleint, L. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab9c1e · Cited by 35
“This method updates the temperatures and areas derived by previous studies (Kretzschmar 2011; Shibayama et al. 2013).”
MethodChang, H.-Y., Lin, C.-L., Ip, W.-H., Huang, L.-C., Hou, W.-J., Yu, P., Song, Y., & Luo, A.-L. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aae2bc · Cited by 32
From solar to stellar flare characteristics
Herbst, K., Papaioannou, A., Banjac, S., & Heber, B. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201832789 · Cited by 31
“It should also be noted that based on the upper flare flux of active G-type stars (1036 erg; see Shibayama et al. 2013) and the corresponding estimated flare flux of the AD Leo event of IX = 9 W m−2 (Segura et al. 2010), which is well within the limitations, the PSDs presented in this work are in…”
BackgroundMethodResultInfluentialMulti-wavelength variability of the young solar analog ι Horologii
Sanz‐Forcada, J., Stelzer, B., Coffaro, M., Raetz, S., & Alvarado‐Gómez, J. D. (2019) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201935703 · Cited by 40
Kay, C., Airapetian, V. S., Lüftinger, T., & Kochukhov, O. (2019) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ab551f · Cited by 35
“…stellar CMEs, which could have been an important factor for planetary habitability in the early history of our solar system and/or most extrasolar systems (Maehara et al. 2012; Shibayama et al. 2013; Takahashi et al. 2016; Airapetian et al. 2016, 2019a; Notsu et al. 2019; Yamashiki et al. 2019).”
Radio emission as a stellar activity indicator
Yiu, T. W. H., Vedantham, H. K., Callingham, J. R., & Günther, M. N. (2023) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202347657 · Cited by 34
Modelling variability of solar activity cycles
Kitchatinov, L. L., Mordvinov, A. V., & Nepomnyashchikh, A. A. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201732549 · Cited by 31
“The detection of numerous flares of very high energy (superflares of >∼ 10 34 erg; Maehara et al. 2012; Shibayama et al. 2013) among solar-type targets of space telescope Kepler provoked a discussion of the possibility and hypothetical origin of exceptionally strong solar cycles (Shibata et al.…”
BackgroundStellar Superflares Observed Simultaneously with Kepler and XMM-Newton
Kuznetsov, A. A., & Kolotkov, D. Y. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/abf569 · Cited by 32
“Following Maehara et al. (2012), Shibayama et al. (2013), and Namekata et al. (2017), we adopted =T 10,000flare K as the typical effective temperature of the white-light flares, with possible variations in the range of 9000–14,000K (Kowalski 2016); this uncertainty in the flare temperature is…”
MethodCharacteristic time of stellar flares on Sun-like stars
Yan, Y., He, H., Li, C., Esamdin, A., Tan, B., Zhang, L., & Wang, H. (2021) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1093/mnrasl/slab055 · Cited by 30
Testing Self-organized Criticality across the Main Sequence Using Stellar Flares from TESS
Feinstein, A. D., Seligman, D. Z., Günther, M. N., & Adams, F. C. (2022) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ac4b5e · Cited by 29
Fast optical flares from M dwarfs detected by a one-second-cadence survey with Tomo-e Gozen
Aizawa, M., Kawana, K., Kashiyama, K., Ohsawa, R., Kawahara, H., Naokawa, F., Tajiri, T., Arima, N., Jiang, H., Hartwig, T., et al. (2022) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psac056 · Cited by 32
“…among the flare parameters and stellar properties, and constructing the template shape of the flare light curves (e.g. Maehara et al. 2012; Notsu et al. 2013; Shibayama et al. 2013; Hawley et al. 2014; Davenport et al. 2014; Davenport 2016; Günther et al. 2020; Howard & MacGregor 2021).”
BackgroundZhang, L., Su, T., Misra, P., Han, X. L., Meng, G., Pi, Q., & Yang, J. (2022) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/ac9b28 · Cited by 33
“Shibayama et al. (2013) studied the superflare associated with G-type stars, and Lin et al. (2019) did research on M-type and K-type stars.”
ResultInfluentialDynamo model for grand maxima of solar activity: can superflares occur on the Sun?
Kitchatinov, L. L., & Olemskoy, S. V. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw875 · Cited by 24
“Shibayama et al. (2013) and Shibata et al. (2013) suggest a positive answer with an esti- ⋆ E-mail: kit@iszf.irk.ru mated frequency of one in about 800 yr for solar superflares of ≥ 1034 erg (one in about 5000 yr for ≥ 1035 erg).”
BackgroundInfluentialPatsourakos, S., & Georgoulis, M. K. (2017) · Solar Physics · doi:10.1007/s11207-017-1124-1 · Cited by 25
“correspond to the wavelength-integrated radiated energy (e.g. Maehara et al., 2012; Shibayama et al., 2013).”
BackgroundMethodInfluentialA study of flares in the ultra-cool regime from SPECULOOS-South
Murray, C. A., Queloz, D. P., Gillon, M., Demory, B.-O., Triaud, A. H. M. J., de Wit, J., Burdanov, A., Chinchilla, P., Delrez, L., Dransfield, G., et al. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac1078 · Cited by 28
UNIVERSAL BEHAVIOR OF X-RAY FLARES FROM BLACK HOLE SYSTEMS
Wang, F. Y., Dai, Z. G., Yi, S. X., & Xi, S. Q. (2014) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/216/1/8 · Cited by 29
“For stellar flares from the Kepler satellite, the size distribution for the total sample of 1538 flares shows a power-law slope of αE = 2.04 ± 0.13 (Walkowicz et al. 2011; Maehara et al. 2012; Shibayama et al. 2013; Aschwanden 2014).”
MethodInfluentialFlaring and Spot Activities on the Semi-detached Binary System KIC 06852488
Shi, X.-D., Qian, S. ‐., Li, L.-J., & Liu, N.-P. (2020) · The Astronomical Journal · doi:10.3847/1538-3881/abccd7 · Cited by 27
“The energy of the flare in the Kepler band is calculated with the following formulae (e.g., Qian et al. 2012; Shibayama et al. 2013), ò=E L t dt 6flare flare flare ( ) ( ) = ´ -- ´DL t L t 10 1 7M tflare 0 0.4 flare( ) ( ) ( ) ( )( ) = ´ - ´DL t L 10 , 8M t0 0.4 binary( ) ( )( ) where L0(t) is the…”
BackgroundMethodInfluentialEvolution of Flare Activity in GKM Stars Younger Than 300 Myr over Five Years of TESS Observations
Feinstein, A. D., Seligman, D. Z., France, K. C., Gagné, J., & Kowalski, A. F. (2024) · The Astronomical Journal · doi:10.3847/1538-3881/ad4edf · Cited by 27
“There has been extensive studies of flares in Kepler data, from the statistics of superflares on solar-type stars (e.g. Notsu et al. 2013; Shibayama et al. 2013; Maehara et al. 2015; Okamoto et al. 2021) to low-mass stars (e.g. Hawley et al. 2014; Silverberg et al. 2016).”
BackgroundSavanov, I. S., & Дмитриенко, Е. С. (2015) · Astronomy Reports · doi:10.1134/s1063772915090073 · Cited by 26
Planetary perturbers: flaring star–planet interactions in Kepler and TESS
Ilin, E., Poppenhaeger, K., Chebly, J., Ilić, N., & Alvarado‐Gómez, J. D. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad3398 · Cited by 29
K2 Ultracool Dwarfs Survey. IV. Monster Flares Observed on the Young Brown Dwarf CFHT-BD-Tau 4
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/aac8e0 · Cited by 28
“…(a brown dwarf member of Pleiades) are capable of producing strong white light superflares with energies > 1033 erg. Superflares are thus ubiquitious in Kepler G, K, M and L stars (Maehara et al. 2012; Shibayama et al. 2013; Notsu et al. 2013; Candelaresi et al. 2014; Gizis et al. 2017a,b).”
BackgroundFlares and rotation of M dwarfs with habitable zones accessible to TESS planet detections
Stelzer, B., Bogner, M., Magaudda, E., & Raetz, S. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202142088 · Cited by 25
Superflares on the late-type giant KIC 2852961
Kővári, Z., Oláh, K., Günther, M. N., Vida, K., Kriskovics, L., Seli, B., Bakos, G. Á., Hartman, J. D., Csubry, Z., & Bhatti, W. A. (2020) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202038397 · Cited by 22
“Specifically, Shibayama et al. (2013) derived α = 2.0 − 2.2 power-law indices for Kepler G-dwarf superflare stars while α=1.53 for the “normal” solar flares.”
BackgroundInfluentialNamizaki, K., Namekata, K., Maehara, H., Notsu, Y., Honda, S., Nogami, D., & Shibata, K. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acb928 · Cited by 27
“From the TESS light curve, we estimate the energy of the whitelight flare by assuming 10,000K blackbody radiation (Shibayama et al. 2013).”
BackgroundMethodSelf-citationAurora candidates from the chronicle of Qíng dynasty in several degrees of relevance
Kawamura, A. D., Hayakawa, H., Tamazawa, H., Miyahara, H., & Isobe, H. (2016) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psw074 · Cited by 24
“…recently because of the observational discoveries of “superflares” in other Sun-like (G type) stars (Schaefer et al. 2000; Maehara et al. 2012; Shibayama et al. 2013; Schrijver et al. 2012; Notsu et al. 2015a, 2015b) as well as the footprints of high cosmic-ray radiation events in wood…”
BackgroundMAGNETIC ACTIVITY ANALYSIS FOR A SAMPLE OF G-TYPE MAIN SEQUENCE KEPLER TARGETS
Mehrabi, A., He, H., & Khosroshahi, H. G. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/834/2/207 · Cited by 24
“As shown by (Maehara et al. 2012) and (Shibayama et al. 2013), the flare spikes can only be discerned from the light curves for a small part of Kepler stars, whereas the fluctuation owing to the rotational modulation is common in Kepler light curves (Notsu et al. 2013; McQuillan et al. 2014).”
BackgroundEstrela, R., & Válio, A. (2018) · Astrobiology · doi:10.1089/ast.2017.1724 · Cited by 25
“It is also expected that younger stars frequently produce superflares (Shibayama et al. , 2013).”
Namekata, K., Sakaue, T., Watanabe, K., Asai, A., & Shibata, K. (2016) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psw111 · Cited by 24
“In the past decade, many stellar and protostellar flares have been observed (e.g., Hawley & Pettersen 1991; Koyama et al. 1996; Tsuboi et al. 1998; Kowalski et al. 2010), and recently, many superflares on solar-type stars have also been detected (Maehara et al. 2012; Shibayama et al. 2013).”
BackgroundSelf-citationSolar Flare Forecasting: Present Methods and Challenges
Leka, K. D., & Barnes, G. (2018) · Elsevier eBooks · doi:10.1016/b978-0-12-812700-1.00003-0 · Cited by 29
Correcting Stellar Flare Frequency Distributions Detected by TESS and Kepler
Gao, D.-Y., Liu, H.-G., Yang, M. D., & Zhou, J. (2022) · The Astronomical Journal · doi:10.3847/1538-3881/ac937e · Cited by 23
“After correction for gyrochronology and detection incompleteness, they obtained α = −1.5 ± 0.1 and −1.8 ± 0.1 for fast rotating solar-type stars (Prot<5 days) with Teff = 5100 − 5600K and 5600−6000K, respectively, using the flare events with 1033.75 erg < Ebol <1035.75 erg. Maehara et al. (2015) and Shibayama et al. (…”
BackgroundMethodInfluentialPaudel, R. R., Barclay, T., Youngblood, A. A., Quintana, E. V., Schlieder, J. E., Vega, L. D., Gilbert, E. A., Osten, R. A., Peacock, S., Tristan, I. I., et al. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad487d · Cited by 23
“Instead, we adopted the approach of Shibayama et al. (2013) which assumes a blackbody (BB) for the spectral energy distribution of each flare and estimates its energy using: where, In Equation 3, A flare is the area of flare emitting region, L flare is the bolometric luminosity of the flare and…”
MethodA Bayesian method for detecting stellar flares
Pitkin, M., Williams, D. R., Fletcher, L., & Grant, S. D. T. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu1889 · Cited by 24
“Previous searches for flares in this data set include Walkowicz et al. (2011), Balona (2012), Maehara et al. (2012) and Shibayama et al. (2013), which have tended to focus on easily recognized large flares.”
BackgroundMethodMatthews, L. D. (2018) · Publications of the Astronomical Society of the Pacific · doi:10.1088/1538-3873/aae856 · Cited by 23
“And importantly, not only do many late-type stars have significantly higher activity levels than the Sun (e.g., Shibayama et al. 2013; Karmakar et al. 2017), but as J. Villadsen reminded us, they may stay active for far longer timescales (up to several Gyr).”
BackgroundDetection Methods and Relevance of Exoplanetary Magnetic Fields
Grießmeier, J. ‐. (2014) · Astrophysics and space science library · doi:10.1007/978-3-319-09749-7_11 · Cited by 26
Spotting stellar activity cycles in Gaia astrometry
Morris, B. M., Agol, E., Davenport, J. R. A., & Hawley, S. L. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty568 · Cited by 25
“Kepler observed 29 large flare eventson this star, with energies ranging from 7 × 1034 to 2 × 1035 ergs (Shibayama et al. 2013).”
BackgroundInoue, S., Enoto, T., Namekata, K., Notsu, Y., Honda, S., Maehara, H., Zhang, J., Lu, H., Uchida, H., Tsuru, T. G., et al. (2024) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psae001 · Cited by 22
Self-citationEarliest 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) · Earth Planets and Space · doi:10.1186/s40623-016-0571-5 · Cited by 25
“interest from the viewpoint of extreme space weather (e.g., Tsurutani et al. 2003; Schrijver et al. 2012) particularly after the discoveries of “superflares” in solar-type stars (Maehara et al. 2012; Shibayama et al. 2013; Maehara at al. 2015) as well as the sharp increase of cosmogenic radioisotopes in tree rings aro…”
BackgroundM-dwarf Eclipsing Binaries with Flare Activity
Huang, L.-C., Ip, W.-H., Lin, C.-L., Zhang, X.-L., Song, Y., & Luo, A.-L. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab774a · Cited by 23
Near-ultraviolet continuum modeling of the 1985 April 12 great flare of AD Leo
Kowalski, A. F. (2022) · Frontiers in Astronomy and Space Sciences · doi:10.3389/fspas.2022.1034458 · Cited by 21
Lin, C.-L., Ip, W.-H., Hsiao, Y., Chang, T.-H., Song, Y., & Luo, A.-L. (2023) · The Astronomical Journal · doi:10.3847/1538-3881/ace322 · Cited by 23
“This is in stark contrast to solar-type stars, which produce flares of this magnitude only once every 35–40 years (Shibayama et al. 2013).”
ResultThe Correlation between Isotropic Energy and Duration of Gamma-Ray Bursts
Tu, Z. L., & Wang, F. Y. (2018) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/aaf4b8 · Cited by 21
Detection of a giant white-light flare on an L2.5 dwarf with the Next Generation Transit Survey
Jackman, J. A. G., Wheatley, P. J., Bayliss, D., Burleigh, M. R., Casewell, S. L., Eigmüller, P., Goad, M. R., Pollacco, D., Raynard, L., Watson, C. A., et al. (2019) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1093/mnrasl/slz039 · Cited by 21
“These parameters are often used in flare analysis (e.g. Shibayama et al. 2013; Davenport et al. 2014) and provide separate measures of the duration.”
MethodVarela, J., Brun, A. S., Strugarek, A., Réville, V., Zarka, P., & Pantellini, F. G. E. (2021) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202141181 · Cited by 22
The Origin of Superflares on G-Type Dwarf Stars of Various Ages
Katsova, M. M., & Livshits, M. A. (2015) · Solar Physics · doi:10.1007/s11207-015-0752-6 · Cited by 21
“We will use the total energies of optical flare emission presented by Shibayama et al. (2013).”
BackgroundMethodResultInfluentialStarspot Mapping with Adaptive Parallel Tempering. I. Implementation of Computational Code
Ikuta, K., Maehara, H., Notsu, Y., Namekata, K., Kato, T., Notsu, S., Okamoto, S., Honda, S., Nogami, D., & Shibata, K. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/abae5f · Cited by 21
Self-citationStarspot Modeling and Flare Analysis on Selected Main-sequence M-type Stars
Bicz, K., Falewicz, R., Pietras, M., Siarkowski, M., & Preś, P. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac7ab3 · Cited by 20
“The highest number of flares has energy of approximately 1032 erg, for the method based on Shibayama et al. (2013), and about 1031.75 erg, for the method based on Kovári et al. (2007).”
BackgroundMethodInfluentialZhang, W., Zhang, J., He, H., Song, Z., Luo, A.-L., & Zhang, H. (2022) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/ac9406 · Cited by 22
Tamazawa, H., Kawamura, A. D., Hayakawa, H., Tsukamoto, A., Isobe, H., & Ebihara, Y. (2017) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psw132 · Cited by 21
“The total energy of the superflares found in the Kepter data by Maehara et al. (2012) and Shibayama et al. (2013) ranges between 1033–1035 ergs, which is 10–1000 times larger than that of the Oct 28, 2003 X17 flare, as reported in Schrijver et al. (2012).”
BackgroundFrequencies of Flare Occurrence: Interaction between Convection and Coronal Loops
Mullan, D. J., & Paudel, R. R. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aaa960 · Cited by 20
“Shibayama et al. (2013) supplement their Kepler superflare analysis with spectra obtained by previous researchers for smaller solar flares: nanoflares, microflares, and “solar flares,” with energies of 1024–1026 erg, 1027–1029 erg, and 1027–1032 erg respectively.”
MethodInfluentialK2 Ultracool Dwarfs Survey. IV. Monster Flares Observed on the Young Brown Dwarf CFHT-BD-Tau 4
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/m2yylj-u2jg · Cited by 20
Close-in planet induces flares on its host star
Ilin, E., Vedantham, H. K., Poppenhaeger, K., Bloot, S., Callingham, J. R., Brandeker, A., & Chakraborty, H. (2025) · Nature · doi:10.1038/s41586-025-09236-z · Cited by 19
Global analysis of the TRAPPIST Ultra-Cool Dwarf Transit Survey
Lienhard, F., Queloz, D. P., Gillon, M., Burdanov, A., Delrez, L., Ducrot, E., Handley, W. J., Jehin, E., Murray, C. A., Triaud, A. H. M. J., et al. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa2054 · Cited by 19
“Shibayama et al. (2013) estimated the uncertainty in the flare energy to ± 60 per cent.”
BackgroundMethodInfluentialStellar flares from blended and neighbouring stars in Kepler short cadence observations
Jackman, J. A. G., Shkolnik, E. L., & Loyd, R. O. P. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab166 · Cited by 19
Su, T., Zhang, L., Long, L., Han, X. L., Misra, P., Meng, G., Pi, Q., Yang, Z., & Yang, J. (2022) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/ac7151 · Cited by 20
“The data set of Shibayama et al. (2013a) shows that the powerlaw index of G-type stars is 2.2.”
BackgroundInfluentialObservations and simulations of stellar coronal mass ejections
Tian, H., Xu, Y., Chen, H., Zhang, J., Lu, H., Chen, Y., Yang, Z., & Wu, Y. (2022) · Scientia Sinica Technologica · doi:10.1360/sst-2022-0212 · Cited by 17
Activity and cold spots on the surface of G-type superflare stars
Savanov, I. S. (2015) · Astrophysical Bulletin · doi:10.1134/s1990341315030062 · Cited by 18
Can Superflares Occur on the Sun? A View from Dynamo Theory
Katsova, M. M., Kitchatinov, L. L., Livshits, M. A., Moss, D. L., Sokoloff, D. D., & USOSKIN, I. G. (2018) · Astronomy Reports · doi:10.1134/s106377291801002x · Cited by 19
The Fractality and Size Distributions of Astrophysical Self-Organized Criticality Systems
Aschwanden, M. J. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac6bf2 · Cited by 18
“These stellar flares have been observed mostly in solar-like G-type stars (Notsu et al. 2013; Maehara et al. 2012; Shibayama et al. 2013), and in cool dwarf (dMe) stars (Robinson et al. 1999; Audard et al. 2000; Kashyap et al. 2002; Güdel et al. 2003; Arzner et al. 2007; Stelzer et al.…”
BackgroundStellar Flares, Superflares, and Coronal Mass Ejections—Entering the Big Data Era
Vida, K., Kővári, Z., Leitzinger, M., Odert, P., Oláh, K., Seli, B., Kriskovics, L., Greimel, R., & Görgei, A. (2024) · Universe · doi:10.3390/universe10080313 · Cited by 23
“We know that solar flares follow a power-law distribution [see 53, and ) [48], green points denote the Kepler flare catalogue of Yang and Liu [49], red points show G-type stars showing superflares [50], and pink points mark flaring giant stars [51].”
BackgroundHigh dispersion spectroscopy of solar-type superflare stars. III. Lithium abundances
Honda, S., Notsu, Y., Maehara, H., Notsu, S., Shibayama, T., Nogami, D., & Shibata, K. (2015) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psv054 · Cited by 21
“It is because the detection of relatively small superflares is somewhat affected by stellar brightness variations (Shibayama et al. 2013).”
BackgroundMethodInfluentialSelf-citationA low-mass eclipsing binary within the fully convective zone from the Next Generation Transit Survey
Casewell, S. L., Raynard, L., Watson, C. A., Gillen, E., de Mooij, E., Bayliss, D., Bouchy, F., Thompson, A., Jackman, J. A. G., Burleigh, M. R., et al. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty2183 · Cited by 18
“To calculate the energy of this flare we use the method from Shibayama et al. (2013), which assumes the flare to be a blackbody-like emitter of 9000 ± 500K. Previous works have identified such emission from M dwarf flares (e.g. Mochnacki & Zirin 1980; Hawley & Fisher 1992) and this method has…”
MethodA sudden change and recovery in the magnetic environment around a repeating fast radio burst.
Li, Y., Zhang, S.-B., Yang, Y.-P., Tsai, C.-W., Yang, X., Law, C., Anna-Thomas, R., Chen, X.-L., Lee, K. J., Tang, Z.-F., et al. (2025) · Science · doi:10.1126/science.adq3225 · Cited by 26
Flare Hunting in Hot Subdwarf and White Dwarf Stars from Cycles 1–5 of TESS Photometry
Xing, K., Zong, W., Silvotti, R., Fu, J.-N., Charpinet, S., Cang, T., Hermes, J. J., Ma, X.-Y., Wang, H., Wang, X., et al. (2024) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/ad2ddd · Cited by 17
“Typically, the total energy emitted by a stellar flare (i.e., the bolometric flare energy) can be estimated if the effective temperature and radius of the star are known (see, e.g., Shibayama et al. 2013; G¨unther et al. 2020).”
BackgroundStellar flares are far-ultraviolet luminous
Berger, V. L., Hinkle, J. T., Tucker, M. A., Shappee, B. J., van Saders, J. L., Huber, D., Reep, J. W., Sun, X., & Yang, K. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae1648 · Cited by 24
“While large-scale observational studies of stellar flares have primarily been conducted in the optical wave-lengths (e.g., Walkowicz et al. 2011; Shibayama et al. 2013; Hawley et al. 2014; Davenport 2016; Schmidt et al. 2019; Rodr´ıguez Mart´ınez et al. 2020; G¨unther et al. 2020; Feinstein et al.…”
Background
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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