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Investigation of coronal properties of X-ray bright G-dwarf stars based on the solar surface magnetic field - corona relation View all abstracts by submitter

Shinsuke Takasao   Submitted: 2020-08-12 02:29

We investigated the coronal properties of G-dwarf stars including the Sun over a wide range of X-ray luminosity L_X (3x1026 to 2x1030 erg s-1). We analyzed the archival data of ten X-ray bright (L_X >1028 erg s-1) G-dwarf stars to derive their emission measure (EM) and the coronal temperature (T) during the periods when no prominent stellar flares were observed. We attempted to explain the relation on the basis of our understanding of the present Sun: a steady corona model based on the so-called RTV scaling laws and the observed power-law distribution function of surface magnetic features. We derived a theoretical scaling law of the EM-T relation for a star with multiple active regions, and applied it to the observations combined with data in literature. We found that with the solar parameters, our scaling law seems to be consistent with the data of slowly-rotating stars. However, more X-ray bright stars are located well above the scaling law based on the solar parameter. The scaling law may explain the observations if those stars show a power-law distribution function of active regions with the same power-law index but a 10-100 times larger coefficient. This suggests that X-ray bright stars show more active regions for a given size than the Sun. Since our samples include rapidly-rotating stars, we infer that the offset of the X-ray bright stars from the present-Sun-based scaling law is due to the enhancement of the surface magnetic field generation by their rapid rotation.

Authors: Shinsuke Takasao, Ikuyuki Mitsuishi, Takuma Shimura, Atsushi Yoshida, Masanobu Kunitomo, Yuki A. Tanaka, Daisuke Ishihara
Projects: None

Publication Status: accepted for publication in ApJ
Last Modified: 2020-08-12 11:26
Go to main E-Print page  Network Jets as the Driver of Counter-streaming Flows in a Solar Filament/Filament Channel  Energy Transfer by Nonlinear Alfv'en Waves in the Solar Chromosphere, and Its Effect on Spicule Dynamics, Coronal Heating, and Solar Wind Acceleration  Edit Entry  Download Preprint  Delete Entry 

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