JOP184 Bright Points from Photosphere to Corona Observations with CDS and Sac Peak (DST). Received: 2005/11/18 J.G. Doyle, M.S. Madjarska & D. Perez-Suarez Observations provided by the SoHO instruments have meant a revolution in our understanding of the Sun in several disciplines. These observations have revealed the presence of intermittent oscillatory wave-trains in the intensity response of the transition region and coronal emission of BPs. In fact, the periods of oscillation coincide with well-known oscillations in the chromospheric network, where the BPs lie, and more precisely the network bright point elements that form this network. This has lead us to suggest that a fraction of network bright points, bright chromospheric network elements associated to photospheric magnetic flux concentrations, are the cool footpoints of the loops that coronal bright points are made (Ugarte-Urra et al 2004). This immediately raises the question of how do these waves fit with the idea that magnetic reconnection is the driving force behind BPs appearance. The magnetic reconnection interpretation is not put under question yet by the results of our studies. In fact, we have found signatures of magnetic flux cancellation just before the rise of the coronal and transition region flux of the BP. However, if reconnection is important in BPs (as commonly assumed) it has to be a slow process and has to explain the observed Doppler shift of transition region lines which are at most 10 km/s red-shifted. We would like to establish more firmly the connection between the oscillations in the chromospheric network bright points (NBPs) and the coronal EUV bright points (BPs). At the moment, our results point towards that link, but no work has given a definite identification of co-spatial and co-temporal oscillations in both features. So far, both have been studied independently, which means that a study of their simultaneous evolution would improve our understanding of both phenomena and, in more general terms, the understanding of the processes in the solar atmosphere that contribute towards coronal heating. Recent works on the oscillations of the chromospheric network (McAteer et al 2004) have suggested that the waves detected could be damped in the upper chromosphere. Our results suggest that this could be the case for the shorter periods, because the longer ones have a clearly defined signature in the transition region and corona. An analysis of the BP brightness evolution at different temperatures would allow an evaluation of which frequencies are damped in the lower layers of the atmosphere and which ones propagate to the coronal counterpart of the BP. This would help us to distinguish between the different mechanisms that have been proposed for the modulation of the emission. Another key aspect that has to be studied is the relation between reconnection events and waves. It is possible that reconnection events are triggering the waves, although granular motions have been shown to be capable, too (Hasan & Kalkofen 1999). One of the missing items from these previous runs were high-cadence/high spatial resolution optical data. Ground-based Observations We propose to use the DST equipped with the UBF or Zeiss-alpha filter. Regarding detectors: One option is the visitor instrument RDI (Rapid Dual Imager) which comprises of two monochromatic 658 x 494 pixel^2 cameras. With a sampling resolution of 0.1 arcseconds per pixel, our field-of-view (FOV) will be 65 x 49 arcseconds^2. RDI can achieve a temporal sampling of up to 60 frames per second simultaneously in the 2 cameras run from the same clock. Although this is a remarkable temporal resolution we initially only intend to use a cadence of a few seconds. One of the cameras will observe in the H alpha core (i.e. chromosphere) while the second in the G-band (photosphere). The G-band images will be used to monitor photospheric changes as well as for destretching the H alpha images. The possibility of a third camera to observe in Ca II K3 (top of the chromosphere) will also be considered. Combined with CDS the proposed setup will give information from the photosphere all the way up to the TR/corona. CDS observations (with pointing up-graded after each sequence in order to feature-track) BP_W_1/v23 11 min raster BP_W_2/v2 15 min time series BP_W_2/v2 15 min time series BP_W_2/v2 15 min time series BP_W_2/v2 15 min time series BP_W_2/v2 15 min time series BP_W_2/v2 15 min time series BP_W_2/v2 15 min time series BP_W_1/v23 11 min raster BP_W_2/v2 15 min time series BP_W_2/v2 15 min time series BP_W_2/v2 15 min time series BP_W_2/v2 15 min time series BP_W_2/v2 15 min time series BP_W_2/v2 15 min time series BP_W_2/v2 15 min time series BP_W_1/v23 11 min raster Where? The coordinated aspect, makes our observations time critical. We request January 19 & 24, 2006 runtime: 14:00-18:00 UT.