Solar-type activity in main-sequence stars

By R. Gershberg. 2005

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Do Kepler Superflare Stars Really Include Slowly Rotating Sun-like Stars?—Results Using APO 3.5 m Telescope Spectroscopic Observations and Gaia-DR2 Data (2019, methodology): “These lines have been widely used for investigating stellar chromospheric activities (e.g., Wilson 1978; Linsky et al. 1979a; Noyes et al. 1984; Duncan et al. 1991; Baliunas et al. 1995; Hall 2008) and are good indicators of stellar average magnetic fields (e.g., Schrijver et al. 1989; Notsu et al.…”
Can Superflares Occur on Our Sun (2012, background): “which is much larger than the total kinetic energy of differential rotation if B = 10(5) G is assumed, as in the current dynamo theory (Ferriz-Mas & Steiner 2007). Hence, the necessary magnetic flux cannot be created by simple stretching of the magnetic field lines by shear motion in differential ro”
SUPERFLARES ON SOLAR-TYPE STARS OBSERVED WITH KEPLER. I. STATISTICAL PROPERTIES OF SUPERFLARES (2013, background): “, Shibata and Yokoyama 2002; Gershberg 2005; Benz and Guedel 2010; Shibata and Magara 2011). During these flare events, various observable effects occur over a wide range in wavelength. On the Sun, our ability to spatially resolve the surface allows flares to be observed in rich detail with high cad”