Coronal Heating of an Active Region Observed by XRT on May 5, 2010 A Look at Quasi-static vs Alfven Wave Heating of Coronal Loops Meet the Corona Low Densities High

Coronal Heating of an Active Region Observed by XRT on May 5, 2010 A Look at Quasi-static vs Alfven Wave Heating of Coronal Loops Meet the Corona Low Densities High www.phwiki.com

Coronal Heating of an Active Region Observed by XRT on May 5, 2010 A Look at Quasi-static vs Alfven Wave Heating of Coronal Loops Meet the Corona Low Densities High

Malaluan, Theresa, Coordinating Producer, The Weekly Update has reference to this Academic Journal, PHwiki organized this Journal Coronal Heating of an Active Region Observed by XRT on May 5, 2010 A Look at Quasi-static vs Alfven Wave Heating of Coronal Loops Am in addition to a Persichetti Aad Van Ballegooijen Meet the Corona Plasma: “The 4th State of Matter” ~ An ionized gas consisting of electrons that have been pulled free of atoms in addition to ions, in which the temperature is too high as long as neutral, un-ionized atoms to exist Low Densities High Temperatures Dominated by Magnetic Fields Electrically neutral plasma As a result of plasma motion, magnetic fields are generated in the sun X-ray Radiation B-Field Frozen-in to Plasma ~Quasi-static ~Alfven Wave Turbulence ~Micro/Nano Flares Coronal Heating it defies expectations -> hundreds of times hotter than photosphere Thermodynamics Why do we Study it A few studied Mechanisms Klimchuk, SoPh, 2006

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Magnetohydrodynamics (MHD) Equation of Motion Force Free Condition Ampere’s Law Instruments XRT (Hinode) Solar Dynamics Observatory (SDO) AIA HMI Active Region: a region in the solar atmosphere, from the photosphere to the corona, that develops when strong magnetic fields emerge from inside the sun. Magnetized realm in in addition to around sunspots. Magnetogram from HMI

May 5, 2010 Active Region 171Å AIA Image One hour movie of 171Å images Modeling Magnetic Fields ~A software package that allows you to construct models of the solar corona based on photospheric magnetograms from HMI in addition to coronal images from AIA ~Models provide in as long as mation about the coronal magnetic field that cannot already be directly observed from SDO data. Accurately model the magnetic field lines of the active region based on data from SDO. This gives us a better idea of the properties of the region in order to make more educated conclusions, in our case, about the heating. Non-Potential Field 1) Construct potential field 2)Insert flux rope in model along manually selected path 3)Apply magneto-frictional relaxation C M S Purpose M S Program Approach van Ballegooijen et al. (2010 in prep) green contours = neg Bfield adjust model so field lines match loops Can see distinct loops in 171 A image red contours = pos Bfield

Heating of Coronal Loops Quasi-Static Response to foot-point motions Alfven Waves Chromosphere Waves reflected back down due to increase in speed with height creates turbulence Alfven Wave Turbulence New View About Waves Heating Rates Quasi-Static Heating Rate per unit volume Alfven Wave Heating Rate Quasi-Static heating dependent on magnetic field, loop length, in addition to properties of foot-point motions. Alfven Wave heating is based on numerical simulations.

Heating of Coronal Loops Radiative Loses Heating Rate Thermal Conduction Compute Temperature in addition to Density with respect to position Three processes related to heating present in the corona: ~Heating rate contribution ~Thermal Conduction ~Radiative Loses Solve Coronal Heating Problem as long as Many Field Lines Alfven velocity = 1.1 km/s Foot-point motion time = 40s Computed in addition to Observed XRT Count Rates

Conclusions Alfven wave turbulence gives off a lot more heating energy than the quasi-static mechanism producing heat rates on orders of 102 greater. This made it able as long as us to get a more accurate fit of calculated intensities to actual intensities as long as reasonable values of the the foot-point motion parameters. The solar corona is so active in addition to constantly changing. When it comes to modeling active regions, each individual one must be modeled with its own individual parameters. They are not consistent as long as all active regions on surface. Continued Study Apply this analysis to various active regions New model involving Alfven wave turbulence Consider interactions between neighboring flux tubes including splitting/merging of flux tubes Special Thanks to Aad van Ballegooijen Karen Meyer

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