STUDY OF THE POYNTING FLUX IN ACTIVE REGION 10930 USING DATA-DRIVEN MAGNETOHYDRODYNAMIC SIMULATION

Journal Article · Wed Aug 10 00:00:00 EDT 2011 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/737/1/39· OSTI ID:21579962

Fan, Y L; Wang, H N; He, H; Zhu, X S ^[1]

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1. Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012 (China)

Powerful solar flares are closely related to the evolution of magnetic field configuration on the photosphere. We choose the Poynting flux as a parameter in the study of magnetic field changes. We use time-dependent multidimensional MHD simulations around a flare occurrence to generate the results, with the temporal variation of the bottom boundary conditions being deduced from the projected normal characteristic method. By this method, the photospheric magnetogram could be incorporated self-consistently as the bottom condition of data-driven simulations. The model is first applied to a simulation datum produced by an emerging magnetic flux rope as a test case. Then, the model is used to study NOAA AR 10930, which has an X3.4 flare, the data of which has been obtained by the Hinode/Solar Optical Telescope on 2006 December 13. We compute the magnitude of Poynting flux (S{sub total}), radial Poynting flux (S{sub z} ), a proxy for ideal radial Poynting flux (S{sub proxy}), Poynting flux due to plasma surface motion (S{sub sur}), and Poynting flux due to plasma emergence (S{sub emg}) and analyze their extensive properties in four selected areas: the whole sunspot, the positive sunspot, the negative sunspot, and the strong-field polarity inversion line (SPIL) area. It is found that (1) the S{sub total}, S{sub z} , and S{sub proxy} parameters show similar behaviors in the whole sunspot area and in the negative sunspot area. The evolutions of these three parameters in the positive area and the SPIL area are more volatile because of the effect of sunspot rotation and flux emergence. (2) The evolution of S{sub sur} is largely influenced by the process of sunspot rotation, especially in the positive sunspot. The evolution of S{sub emg} is greatly affected by flux emergence, especially in the SPIL area.

• OSTI ID: 21579962
• Journal Information: Astrophysical Journal, Vol. 737, Issue 1; Other Information: DOI: 10.1088/0004-637X/737/1/39; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
FLUX DENSITY
MAGNETIC FIELD CONFIGURATIONS
MAGNETIC FLUX
MAGNETOHYDRODYNAMICS
PHOTOSPHERE
SIMULATION
SOLAR FLARES
SOLAR SYSTEM EVOLUTION
TIME DEPENDENCE
ATMOSPHERES
EVOLUTION
FLUID MECHANICS
HYDRODYNAMICS
MECHANICS
SOLAR ACTIVITY
SOLAR ATMOSPHERE
STELLAR ACTIVITY
STELLAR ATMOSPHERES
STELLAR FLARES