Modelling X-ray Bright Points on the Quiet Sun. Parameter fitting to a Coronal Heating solution. Matthew Chantry Mentor: Aad van Ballegooijen University.

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Modelling X-ray Bright Points on the Quiet Sun. Parameter fitting to a Coronal Heating solution. Matthew Chantry Mentor: Aad van Ballegooijen University of St Andrews

What is an X-ray Bright point? X-ray bright points are small dynamic loop structures that are observed all over the solar corona. They have a correspondence with small bipolar magnetic regions (Krieger et al. 1971, Tousey et al. 1973). Modelling X-ray Bright Points on the Quiet Sun. Matthew ChantryREU SymposiumUniversity of St Andrews

Aim To find coronal heating parameters that enable modelling of XRT intensities in multiple filters. Method Construct a potential field from a magnetogram. Solve the energy equation for each field line. Compute XRT intensities. Compare to XRT data. Modelling X-ray Bright Points on the Quiet Sun. Matthew ChantryREU SymposiumUniversity of St Andrews

Construct Potential field Line of sight Modelling X-ray Bright Points on the Quiet Sun. Matthew ChantryREU SymposiumUniversity of St Andrews

Coronal Heating rate per unit volume B photo – 1500G, field strength in the photospheric network (Stenflo 1984). B mag – the magnetic field strength at each point along the field line. f – filling factor, the heat is not applied evenly along the LOS, but is applied to a proportion of each part of the LOS. L T – the total length of the field line L p & τ – variables which describe the length and time scales of the granulations which input the energy into the system. f & L p are the unknown variables which make up our parameter space. (van Ballegooijen 1986) Modelling X-ray Bright Points on the Quiet Sun. Matthew ChantryREU SymposiumUniversity of St Andrews

Field lineLine of sight Solving the Energy Equation Temperature Density Temperature Modelling X-ray Bright Points on the Quiet Sun. Matthew ChantryREU SymposiumUniversity of St Andrews

Field lineLine of sight Computing XRT Intensities Modelling X-ray Bright Points on the Quiet Sun. Matthew ChantryREU SymposiumUniversity of St Andrews

Comparing to XRT data Ti-poly Bp 1 Model: Full line Data: Dashed line Modelling X-ray Bright Points on the Quiet Sun. Matthew ChantryREU SymposiumUniversity of St Andrews

Measuring the fit Ti-polyAl-poly/Ti-poly C-poly/Ti-polyC-poly Bp 1 Modelling X-ray Bright Points on the Quiet Sun. Matthew ChantryREU SymposiumUniversity of St Andrews

Combined fit Bp 1 Minimum Modelling X-ray Bright Points on the Quiet Sun. Matthew ChantryREU SymposiumUniversity of St Andrews

Fitting the Temperature Ti-poly Bp 1 Modelling X-ray Bright Points on the Quiet Sun. Matthew ChantryREU SymposiumUniversity of St Andrews

Fitting the Temperature Be-thin Bp 1 Modelling X-ray Bright Points on the Quiet Sun. Matthew ChantryREU SymposiumUniversity of St Andrews

Fitting the Temperature Ti-poly Bp 1 Modelling X-ray Bright Points on the Quiet Sun. Matthew ChantryREU SymposiumUniversity of St Andrews

Intensities in other filters Be-thin Al-poly/Ti-polyC-poly/Ti-poly C-poly Bp 1 Modelling X-ray Bright Points on the Quiet Sun. Matthew ChantryREU SymposiumUniversity of St Andrews

Errors Alignment of XRT images to the magnetogram. Calibration of XRT intensities. Unclear what the statistical errors are. XRT response rates. Heating model is time averaged, but bright point intensities oscillate (Kariyappa & Varghese 2008). Plasma beta > 1 for low filling factors. Using this XRT data, we cannot uniquely determine the filling factor. Need longer exposures in thicker filters? Other sources of error/uncertainty: Modelling X-ray Bright Points on the Quiet Sun. Matthew ChantryREU SymposiumUniversity of St Andrews

Conclusions For this bright point a good fit can be achieved for all 5 filters. This method has also been successfully applied to other bright points (in this and other data-sets). Fits are not always found for more complicated magnetic structures. Systematic difference found at the sides of the features. Work with density sensitive line ratios has found bright point filling factors < 0.1 (Dere 2008 & 2009). Thanks to Aad van Ballegooijen, Steve Saar, Henry (Trae) Winter III, Kelly Koreck and everyone else! Modelling X-ray Bright Points on the Quiet Sun. Matthew ChantryREU SymposiumUniversity of St Andrews