Statistical properties of superflares on solar-type stars based on 1-min cadence data
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- Material Type
- 記事
- Author/Editor
- Hiroyuki MaeharaTakuya ShibayamaYuta Notsu
- Publication, Distribution, etc.
- Publication Date
- 2015-04-29
- Publication Date (W3CDTF)
- 2015-04-29
- Periodical title
- EPS : Earth, Planets and Space
- No. or year of volume/issue
- 67(59)
- Volume
- 67(59)
- ISSN (Periodical Title)
- 1880-5981
- ISSN-L (Periodical Title)
- 1343-8832
- Text Language Code
- eng
- DOI
- 10.1186/s40623-015-0217-z
- Persistent ID (NDL)
- info:ndljp/pid/9483544
- Collection
- Collection (Materials For Handicapped People:1)
- Collection (particular)
- 国立国会図書館デジタルコレクション > 電子書籍・電子雑誌 > その他
- Acquisition Basis
- オンライン資料収集制度
- Date Accepted (W3CDTF)
- 2015-08-17T20:47:01+09:00
- Date Captured (W3CDTF)
- 2015-06-20
- Format (IMT)
- application/pdf
- Access Restrictions
- 国立国会図書館内限定公開
- Service for the Digitized Contents Transmission Service
- 図書館・個人送信対象外
- Availability of remote photoduplication service
- 可
- Periodical Title (URI)
- Periodical Title (Persistent ID (NDL))
- info:ndljp/pid/9227920
- Data Provider (Database)
- 国立国会図書館 : 国立国会図書館デジタルコレクション
- Summary, etc.
- We searched for superflares on solar-type stars using Kepler data with 1-min sampling in order to detect superflares with a short duration. We found 187 superflares on 23 solar-type stars whose bolometric energy ranges from the order of 10<sup>32</sup> to 10<sup>36</sup> erg. Some superflares show multiple peaks with the peak separation of the order of 100 to 1, 000 s which is comparable to the periods of quasi-periodic pulsations in solar and stellar flares. Using these new data combined with the results from the data with 30-min sampling, we found that the occurrence frequency (dN/dE) of superflares as a function of flare energy (E) shows the power-law distribution (dN/dE∞E <sup>-α</sup> ) with α∼-1.5 for 10<sup>33</sup><E<10<sup>36</sup> erg which is consistent with the previous results. The average occurrence rate of superflares with the energy of 10<sup>33</sup> erg which is equivalent to X100 solar flares is about once in 500 to 600 years. The upper limit of energy released by superflares is basically comparable to a fraction of the magnetic energy stored near starspots which is estimated from the photometry. We also found that the duration of superflares (τ) increases with the flare energy (E) as τ∞E <sup>0.39 ± 0.03</sup>. This can be explained if we assume the time scale of flares is determined by the Alfvén time.
- DOI
- 10.1186/s40623-015-0217-z10.48550/arxiv.1504.00074
- Access Restrictions
- インターネット公開
- Rights (production)
- © 2015 Maehara et al.; licensee Springer. This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly credited.
- Related Material (URI)
- Is Referenced By
- Discovery of a long-duration superflare on a young solar-type star EK Draconis with nearly similar time evolution for Ha and white-light emissionsHistorical Auroras in the 990s: Evidence of Great Magnetic StormsHigh dispersion spectroscopy of solar-type superflare stars. III. Lithium abundancesSpectroscopic observations of active solar-analog stars with high X-ray luminosity, as a proxy of superflare starsFractal Reconnection in Solar and Stellar EnvironmentsLow-latitude Aurorae during the Extreme Space Weather Events in 1859Lifetimes and Emergence/Decay Rates of Star Spots on Solar-type Stars Estimated by Kepler Data in Comparison with Those of SunspotsDo Kepler Superflare Stars Really Include Slowly Rotating Sun-like Stars?—Results Using APO 3.5 m Telescope Spectroscopic Observations and Gaia-DR2 DataProbability Distribution Functions of Solar and Stellar FlaresApache Point Observatory (APO)/SMARTS Flare Star Campaign Observations. I. Blue Wing Asymmetries in Chromospheric Lines during Mid-M-Dwarf Flares from Simultaneous Spectroscopic and Photometric Observation DataRising Near-ultraviolet Spectra in Stellar MegaflaresStatistical Studies of Solar White-light Flares and Comparisons with Superflares on Solar-type StarsOn the Size of the Flare Associated with the Solar Proton Event in 774 ADTime-resolved spectroscopy and photometry of M dwarf flare star YZ Canis Minoris with OISTER and TESS: Blue asymmetry in the Hα line during the non-white light flareStatistical Properties of Superflares on Solar-type Stars: Results Using All of the Kepler Primary Mission DataExtreme solar eventsReconstructing the XUV Spectra of Active Sun-like Stars Using Solar Scaling Relations with Magnetic FluxEffect of Time-varying X-Ray Emission from Stellar Flares on the Ionization of Protoplanetary DisksThe Characteristics of Solar X-Class Flares and CMEs: A Paradigm for Stellar Superflares and Eruptions?Starspot activity and superflares on solar-type starsMAGNETIC PROPERTIES OF SOLAR ACTIVE REGIONS THAT GOVERN LARGE SOLAR FLARES AND ERUPTIONSThe Celestial Sign in the Anglo-Saxon Chronicle in the 770s: Insights on Contemporary Solar Activity{High dispersion spectroscopy of solar-type superflare stars with Subaru/HDSRecurrent Large‐Scale Solar Proton Events Before the Onset of the Wolf Grand Solar MinimumSupernovae and Single-Year Anomalies in the Atmospheric Radiocarbon RecordA great space weather event in February 1730Modeling Hadronic Gamma-Ray Emissions from Solar Flares and Prospects for Detecting Nonthermal Signatures from ProtostarsTemporal Variation of Flare Occurrence Rates via the Spot Evolution on the Sun and Solar-type StarsImpact of Stellar Superflares on Planetary HabitabilitySouth American auroral reports during the Carrington storm
- References
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- Data Provider (Database)
- 国立情報学研究所 : CiNii Research
- Original Data Provider (Database)
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- Bibliographic ID (NDL)
- 9483544
- NAID
- 120005756325