The hard X-ray limb of the Sun H. S. Hudson. Basic factors Gravity makes the limb round to about 10 ppm Gravity also makes it smooth: the maximum small-

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Presentation transcript:

The hard X-ray limb of the Sun H. S. Hudson

Basic factors Gravity makes the limb round to about 10 ppm Gravity also makes it smooth: the maximum small- scale roughness (the Wilson depression) is of order 0.1% Above the photosphere the rough structure rapidly increases in amplitude because of dynamics created by convection and oscillations in the interior

How do we sense the limb? The radius of the Sun is defined at  5000 = 1 (ie, unit opacity at 5000 Å at disk center At the limb, the altitude of  5000 = 1 increases, depending upon the details of the opacity around 5000 Å For Thomson opacity, ie that applicable to hard X- rays for which h << m e c 2 but above the photoeffect range, the limb is at 649 km above the radius.

Kontar-Jeffrey opacities

Can RHESSI measure the structure of the limb usefully? Traditional models (the “semi-empirical” approach of VAL-C) are 1D and have no direct height scale Modern knowledge of the structure of the chromosphere depends on complex models that treat radiative transfer and dynamics simultaneously X-ray opacity is relatively simple (very simple in the Thomson-scattering energy range)

Modern models From Wedemeyer-Bohm in the Cartoon Archive. The lower version is a more realistic scaling.

What could RHESSI learn? The actual height distribution of mass in the quiet solar atmosphere is known only anecdotally at present. This is because of the dynamics and the uncertainties of radiative transfer, I think The height jump at the Fe K edge would determine the iron abundance in a straightforward way

Based on models, what can we expect? Fontenla et al. (2009) model 1001 Ad hoc linear connection Corona with ad hoc base height and density

The Thomson opacity integrated along the tangent to the X-ray limb (649 km) Kernel ~ 2 Mm

Kontar-Jeffrey opacities

Limb heights

What could RHESSI learn? Three photon energies: kev, keV, and ~15 keV (Thomson range) The height differences of the limb are discouragingly small: arc sec to determine the Fe abundance; 0.16 arc sec to determine if there is any Fe at all RHESSI limb observations will be very informative for various reasons, even if the Fe abundance is a bit of a stretch

Practical matters Flare source from behind the limb - need to know location (STEREO) - ideal spectrum is featureless time-stationary continuum We (Hurford) know how to use visibility phases for measuring limb structure We (Glesener, Krucker) have found a candidate source for practice We (Battaglia) have found that footpoint sources occur (in the TTM) above the limb; hence we may have useable continuum background sources

Practice flare SOL T13:03 C2.2 AR ow=grth+qlpcr+qli02+grwa&date= &time=

Practice flare Longitude ? Source height > 10 4 km?