Scaling-laws of quiet-Sun coronal loops

CRISTINA H. MANDRINI; CECILIA MAC CORMACK; ALBERTO M. VÁSQUEZ; MARCELO LÓPEZ FUENTES

Ciudad de Buenos Aires

Conferencia; COLAGE XI; 2018

ALAGE

Different coronal heating models predict particular relations between the physical parameters of coronal loops, such as temperature, density, loop length and magnetic field. These relations and the expected scaling laws obtained from them have been previously compared with observations in the case of coronal loops from active regions (ARs) (see Mandrini, Demoulin and Klimchuk 2000, ApJ, 530, 999). Until recently, the lack of a direct identification of loops in the quiet-Sun corona made it very difficult to perform this kind of studies outside ARs. In a series of recent works (see the review by Vasquez 2016, AdSpR, 57, 1286), a novel coronal tomography procedure was developed that provides, integrated from EUV observations along a solar rotation, the three-dimensional distribution of the mean temperature and density in the coronal volume between 1.02 and 1.225 solar radii (Frazin et al., 2009). In addition, the magnetic field can be extrapolated using a potential model (PFSS) with a synoptic magnetogram as a boundary condition. The tomographic results are combined with potential magnetic field extrapolations to obtain the mean temperature and density of the plasma along field lines integrated from the magnetic model (see Lloveras et al. in this session). Further, using the temperatures and densities obtained with the DEMT and a model based in energy balance in individual loops we compute the expected energy input flux. In this preliminary work, we study the scaling laws between observed and inferred parameters of coronal loops reconstructed from the tomography and magnetic model combination for Carrington rotation 2081 (see Mac Cormack et al. 2017, ApJ, 843, 70).