E-Print Archive

There are 4414 abstracts currently viewable.


Advanced Search
Main Page Add New E-Print Submitter
News Help/FAQ About Preferences
Manage Key Phrase
M-dwarf's Chromosphere, Corona and Wind Connection via the Nonlinear Alfvén Wave View all abstracts by submitter

Takahito Sakaue   Submitted: 2021-06-25 12:13

M dwarf's atmosphere is expected to be highly magnetized. The magnetic energy can be responsible for heating the stellar chromosphere and corona, and driving the stellar wind. The nonlinear propagation of Alfvén wave is the promising mechanism for both heating stellar atmosphere and driving stellar wind. Based on this Alfvén wave scenario, we carried out the one-dimensional compressive magnetohydrodynamic (MHD) simulation to reproduce the stellar atmospheres and winds of TRAPPIST-1, Proxima Centauri, YZ CMi, AD Leo, AX Mic, as well as the Sun. The nonlinear propagation of Alfvén wave from the stellar photosphere to chromosphere, corona, and interplanetary space is directly resolved in our study. The simulation result particularly shows that the slow shock generated through the nonlinear mode coupling of Alfvén wave is crucially involved in both dynamics of stellar chromosphere (stellar spicule) and stellar wind acceleration. Our parameter survey further revealed the following general trends of physical quantities of stellar atmosphere and wind. (1) The M dwarfs' coronae tend to be cooler and denser than solar corona. (2) M dwarfs' stellar winds can be characterized with relatively faster velocity and much smaller mass-loss rate compared to those of solar wind. The physical mechanisms behind these tendencies are clarified in this paper, where the stronger stratification of M dwarf's atmosphere and relatively smaller Alfvén wave energy input from the M dwarf's photosphere are remarkable.

Authors: Takahito Sakaue and Kazunari Shibata
Projects: None

Publication Status: accepted for publication in The Astrophysical Journal
Last Modified: 2021-06-26 06:05
Go to main E-Print page  Characteristic time of stellar flares on Sun-like stars  Bayesian evidence for a nonlinear damping model for coronal loop oscillations  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

Go to main E-Print pageGo to main E-Print page.
Previous AbstractPrevious Abstract.
Next AbstractNext Abstract.
Download PreprintDownload Preprint.
Submitter's HomepageSubmitters Homepage.
Edit EntryEdit Entry.
View All Abstracts By SubmitterView all abstracts by submitter.
Delete AbstractDelete abstract.

Latest Entries
Formation of Magnetic Flux Rope during Solar Eruption. I. Evolution of Toroidal Flux and Reconnection Flux
Stereoscopy of extreme UV quiet Sun brightenings observed by Solar Orbiter/EUI
Solar Flare Effects on the Earth’s Lower Ionosphere
Measurements of Photospheric and Chromospheric Magnetic Field Structures Associated with Chromospheric Heating over a Solar Plage Region
Probing Current Sheet Instabilities from Flare Ribbon Dynamics
Global Nature of Solar Coronal Shock Waves shown by Inconsistency between EUV Waves and Type II Radio Bursts
Solar surges related to UV bursts: Characterization through k-means, inversions and density diagnostics
A revised cone model and its application to non-radial prominence eruptions
Zonal harmonics of solar magnetic field for solar cycle forecast
TESS observations of flares and quasi-periodic pulsations from low mass stars and potential impact on exoplanets
Kink oscillations of coronal loops
First Frequency-Time-Resolved Imaging Spectroscopy Observations of Solar Radio Spikes
Magnetic Flux and Magnetic Non-potentiality of Active Regions in Eruptive and Confined Solar Flares
Observations of shock propagation through turbulent plasma in the solar corona
The Formation and Lifetime of Outflows in a Solar Active Region
Localised acceleration of energetic particles by a weak shock in the solar corona
Stereoscopic Measurements of Coronal Doppler Velocities
Multi-wavelength Observations of a Metric Type-II Event
A physics-based method that can predict imminent large solar flares
The Solar Memory From Hours to Decades

Related Pages
MSU Solar Physics.
Max Millennium Science Mail Archive.
Max Millennium Message of the Day Mail Archive.
Max Millennium Flare Catalog

Archive Maintainer
Alisdair Davey

© 2000-2020 Solar Physics Group - Montana State University