Statistics – Computation
Scientific paper
Nov 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...381..234c&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 381, Nov. 1, 1991, p. 234-249. Research supported by NASA and ASI.
Statistics
Computation
10
Dwarf Stars, Flare Stars, M Stars, Stellar Coronas, Stellar Models, X Ray Stars, Computational Astrophysics, Digital Simulation, Hydrodynamics, Late Stars
Scientific paper
Flare-loop models are utilized to simulate the time evolution and physical characteristics of stellar X-ray flares by varying the values of flare-energy input and loop parameters. The hydrodynamic evolution is studied in terms of changes in the parameters of the mass, energy, and momentum equations within an area bounded by the chromosphere and the corona. The zone supports a magnetically confined loop for which processes are described including the expansion of heated coronal gas, chromospheric evaporation, and plasma compression at loop footpoints. The intensities, time profiles, and average coronal temperatures of X-ray flares are derived from the simulations and compared to observational evidence. Because the amount of evaporated material does not vary linearly with flare-energy input, large loops are required to produce the energy measured from stellar flares.
Cheng Chung-Chieh
Pallavicini Roberto
No associations
LandOfFree
Numerical simulations of flares on M dwarf stars. I - Hydrodynamics and coronal X-ray emission does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Numerical simulations of flares on M dwarf stars. I - Hydrodynamics and coronal X-ray emission, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Numerical simulations of flares on M dwarf stars. I - Hydrodynamics and coronal X-ray emission will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1716760