2007-08-23T23:42:15.000Z http://sot.lmsal.com Mr. Sam Freeland Lockheed Martin Solar and Astrophysics Laboratory (LMSAL) http://www.lmsal.com Lockheed Martin Advanced Tech Center, 3251 Hanover Rd, O/ADBS, B/252, Palo Alto, CA 94304 null null HINODE XRT OKAMOTO, Takenori, J. ISHIBASHI, Kazunori 0 5 0.704 -0.028 2113.66 528.415 2007-08-21T05:47:49.000Z 2007-08-21T18:22:54.000Z 0.704 -0.028 EIS+ SOT+XRT Physical mechanisms driving solar microflares and supergranular network dynamics - relevance for coronal heating, Active Region and; Network Wave Propagation: Active Region Movie STOP_Observation Tim File-OBS_DEC: CCD Monitor During Bakeout - G-Band and X-ray + 4 strips Al/mesh; Daily Note: none; Request to XRT HOP Number 0020: XRT: high cadence of the images is required using just one selected filter using no binning and loss-less compression of data. and;#8226;Microflare mode: 256x256px,thin Be filter, exposure max. 1s with AEC cadence 10s and;#8226;Network mode: 384x384px, thin-Al/Mesh, exposure max. 15s with AEC, cadence 15s For the each particular day target will selected well in advance leading to the corresponding XRT observing mode. ; Other Instruments: DOT SoHO/CDS/MDI/EIT JOP 189: 3-17 Aug 2007 7:00 - 13:30 UT TRACE RHESSI ; Scientific Objectives: This proposal merges together attempts to observe two kinds of solarstructures and;#8211; solar micro flares and super granular network and;#8211; which are planned tobe investigated toaddress common openquestions on the irrelevance for the heating and dynamics of the solar corona.Daily Note: none; Request to XRT HOP Number 0034: XRT observations are requested to provide 'Dynamics' observations. High cadence 512x512, no binning, observations are requested in the Ti_poly filter with 20s exposure and ~30s cadence, or alternatively 368x368 images if required to obtain high cadence.; Other Instruments: SST TRACE; Scientific Objectives: Intensity and velocity oscillations have been observed in the chromosphere above sunspots for over thirty years (Beckers and; Tallant 1969; Beckers and; Schultz 1972; Gurman et al. 1982; Lites et al. 1982). These oscillations have since been observed in the transition region, using space-based instruments observing in the extreme ultra-violet (EUV) (see, Fludra 2001; O'Shea et al. 2002; Rendtel et al. 2003; Brynildsen et al. 2004, and references within). Additionally, space-based EUV bandpass imagers have observed periodic intensity propagations along diffuse, fan-like, coronal loop structures (Berghmans and; Clette 99; Nightingale et al 1999, De Moortel 2002a). De Moortel (2002b) observe a relationship between 3-minute propagations found within sunspot coronal loops, and 5-minute propagations found within plage coronal loops. In Marsh et al.(2003) we present an observation of a 5-minute propagating wave within a plage coronal loop; the intensity oscillation of the wave was also observed simultaneously at transition region temperatures, suggesting wave propagation through the transition region into the corona along the active region loops. Depontieu et al. (2005) also discuss the possibility of channeling the 5-min photospheric oscillations into the corona along the magnetic field. The bright solar network, defined by the boundaries of supergranular flows, is dominated by magnetohydrodynamic (MHD) processes and contains oscillations with periods above of the acoustic cut-off (Goodman 2000). Regions of enhanced emission have the strongest magnetic fields and constitute the most intense radiative losses. The microstructure of these fields and their interactions with the convection zone supply energy to the overlying layers. The granular buffeting of flux tubes in the photosphere can create transverse waves which may mode couple to longitudinal waves and can be observed through variations in the plasma emission and radial velocity. In Marsh and; Walsh (2006) we present new, spatially resolved, monochromatic imaging data of a sunspot region at transition region temperatures, combined with simultaneous bandpass imaging of the emerging coronal loops. The 3-minute umbral oscillations are observed in the transition region, and are then observed to propagate along the sunspot coronal loop system. These propagating waves are interpreted as the transmission of global p-modes that undergo absorption, slow mode conversion, and are wave-guided into the corona by the strong magnetic field. A complete, simultaneous, view of the atmosphere from the photosphere, chromosphere, transition region and corona is required.Daily Note: none; Request to XRT HOP Number 0020: XRT: high cadence of the images is required using just one selected filter using no binning and loss-less compression of data. and;#8226;Microflare mode: 256x256px,thin Be filter, exposure max. 1s with AEC cadence 10s and;#8226;Network mode: 384x384px, thin-Al/Mesh, exposure max. 15s with AEC, cadence 15s For the each particular day target will selected well in advance leading to the corresponding XRT observing mode. ; Other Instruments: DOT SoHO/CDS/MDI/EIT JOP 189: 3-17 Aug 2007 7:00 - 13:30 UT TRACE RHESSI ; Scientific Objectives: This proposal merges together attempts to observe two kinds of solarstructures and;#8211; solar micro flares and super granular network and;#8211; which are planned tobe investigated toaddress common openquestions on the irrelevance for the heating and dynamics of the solar corona.Daily Note: none; Request to XRT HOP Number 0034: XRT observations are requested to provide 'Dynamics' observations. High cadence 512x512, no binning, observations are requested in the Ti_poly filter with 20s exposure and ~30s cadence, or alternatively 368x368 images if required to obtain high cadence.; Other Instruments: SST TRACE; Scientific Objectives: Intensity and velocity oscillations have been observed in the chromosphere above sunspots for over thirty years (Beckers and; Tallant 1969; Beckers and; Schultz 1972; Gurman et al. 1982; Lites et al. 1982). These oscillations have since been observed in the transition region, using space-based instruments observing in the extreme ultra-violet (EUV) (see, Fludra 2001; O'Shea et al. 2002; Rendtel et al. 2003; Brynildsen et al. 2004, and references within). Additionally, space-based EUV bandpass imagers have observed periodic intensity propagations along diffuse, fan-like, coronal loop structures (Berghmans and; Clette 99; Nightingale et al 1999, De Moortel 2002a). De Moortel (2002b) observe a relationship between 3-minute propagations found within sunspot coronal loops, and 5-minute propagations found within plage coronal loops. In Marsh et al.(2003) we present an observation of a 5-minute propagating wave within a plage coronal loop; the intensity oscillation of the wave was also observed simultaneously at transition region temperatures, suggesting wave propagation through the transition region into the corona along the active region loops. Depontieu et al. (2005) also discuss the possibility of channeling the 5-min photospheric oscillations into the corona along the magnetic field. The bright solar network, defined by the boundaries of supergranular flows, is dominated by magnetohydrodynamic (MHD) processes and contains oscillations with periods above of the acoustic cut-off (Goodman 2000). Regions of enhanced emission have the strongest magnetic fields and constitute the most intense radiative losses. The microstructure of these fields and their interactions with the convection zone supply energy to the overlying layers. The granular buffeting of flux tubes in the photosphere can create transverse waves which may mode couple to longitudinal waves and can be observed through variations in the plasma emission and radial velocity. In Marsh and; Walsh (2006) we present new, spatially resolved, monochromatic imaging data of a sunspot region at transition region temperatures, combined with simultaneous bandpass imaging of the emerging coronal loops. The 3-minute umbral oscillations are observed in the transition region, and are then observed to propagate along the sunspot coronal loop system. These propagating waves are interpreted as the transmission of global p-modes that undergo absorption, slow mode conversion, and are wave-guided into the corona by the strong magnetic field. A complete, simultaneous, view of the atmosphere from the photosphere, chromosphere, transition region and corona is required. ivo://sot.lmsal.com/VOEvent#2007-08-21T04:50:00Z