JOP 186 Atmospheric Seismology Joint Observing Program Authors: Mike Marsh (GSFC) Email: mmarsh@uclan.ac.uk Draft v1.0: 19 May 2006 Proposed observing schedule: 2 week period between 13 July - 19 Aug 2006 Participating Instruments: CDS (EOF GSFC) TRACE (EOF GSFC) MDI (EOF GSFC) EIT (EOF GSFC) DST -UBF/SPINOR (Dunn Solar Telescope, Sac Peak) Contacts: SOC soc@soc.nascom.nasa.gov CDS A.Fludra@rl.ac.uk, P.R.Young@rl.ac.uk TRACE trace_planner@lmsal.com, dcm@chippewa.nascom.nasa.gov MDI gregory@mdisas.nascom.nasa.gov, mdi-ops@mdisas.nascom.nasa.gov, mdiers@mdisas.nascom.nasa.gov EIT gurman@gsfc.nasa.gov DST - UBF bala@nso.edu - SPINOR navarro@ucar.edu, elmore@ucar.edu Conflicts: SOHO 26m keyholes 26 May - 15 June 20 Aug - 20 Sept 23 Nov - 12 Dec TRACE eclipse 22 Sept - 1 March '07 JOP 171 28 June - 12 July (inc TBC MDI, TRACE) EIT Shutterless 26 July, 2 Aug Objective: This observing program aims to investigate MHD wave propagation within the atmosphere, using high cadence co-spatial, co-temporal, multi-temperature imaging and spectroscopic observations. Combining both space and ground based instrumentation to investigate the structure and dynamics within atmospheric structures, particularly the transmission of photospheric p-modes from the photosphere to the corona within quiescent active region systems. The propeties these waves may then be related to the measured parameters of the atmosphere, such as temperature and density, and theoretical models. Target Selection / Pointing Requirements: TARGET: The base of quiescent, long-lived AR loop on disk or on limb. Ideally located towards disk centre within the MDI HR field of view. Program Operations: CDS: i) UCLAN_MV ID:96 var:2 wide slit observations Lines : He I 584, O V 629, Mg IX 368 FOV: 90" x 240" Cadence: 26s ii) LOOPS2D_5 ID:31 var:8 high cadence rasters Lines: He I 584, O V 629, Mg IX 368 FOV: 20" x 120" Cadence: ~55s iii) Coronal densities raster SIG_FT44 Possible new densities raster including Transition region - O IV 625.85/554.51 Low corona - Mg VII 319.0/367.7 Corona - Si IX (342,345,349) iv) EJECT_V3 ID:11 var:18 context rasters Coronal context for pointing correlation with TRACE 171 Possible GENE variant ARCONT ID: 11 var:113 - 10 lines, 35s exp, 44 min dur ARCONT_1 ID:11 var:95 - 10 lines, 18s exp, 25 min dur TRACE: i) 171 high cadence coronal movie FOV: 512" x 512" Binning: 1 x 1 Cadence: <30s constant cadence ii) 1600 high cadence movie FOV: 512" x 512" Binning: 1 x 1 Cadence: <30s constant cadence iii) 171 high quality/cadence movie FOV: 512" x 512" Binning: 1 x 1 No JPEG compression Cadence: Constant, and as fast as possible iv) Alternating channel movies e.g. 171/1600 FOV: 512" x 512" Binning: If possible 1 x 1, otherwise 2 x 2 Cadence: <30s constant cadence v) EUV Triple filter image 171/195/284 FOV: 512" x 512" Binning: 1 x 1 Cadence: Single deep exposure in each channel. vi) At least WL & 171 context image to be taken at the beginning and end of each observing sequence for multi-instrument co-alignment. Preferably both WL, 171 and 1600 context images to be taken at the beginning and end of each sequence. MDI: i) High resolution Dopplergram, magnetogram, intensity. hr_ve_fe_me - 1 minute cadence, extracted Magnetograms, Dopplergrams and Filtergrams with a 620"x310" FOV. hr_t2_ve_fe_me - 1 minute cadence, extracted Magnetograms, Dopplergrams and Filtergrams with a 420"x420" FOV. ii) Full disk high cadence magnetogram, Dopplergrams. p30vr_fd_m1 - 1 minute cadence magnetogram, Dopplergram iii) Full disk context images WL continuum and magnetogram context images required at beginning and end of observing sequences. WL context is required for pointing correlation between MDI, CDS, TRACE and Sac Peak. Full disk WL + magnetogram available every 96 mins during high rate data flow. EIT: i) Routine 171 images required for context pointing of other instruments ii) If possible EIT high cadence shutterless mode coincident with TRACE 171 movie. DST-UBF: i) Fe I, H alpha 2-D imaging/Dopplergrams FOV: 169" x 169" Cadence: ~30s DST-SPINOR: Vector magnetogram maps - high cadence polarimetry 120" slit i) Chromospheric Ca II IR triplet 8498A 8542A, ii) Photospheric Fe I 5250A 5247A Scientific Case: Solar p-modes are acoustic waves generated by turbulent convective processes in the convection zone of the Sun (Stein, 1967). These processes force the stochastic excitation of standing acoustic modes within the atmosphere, observed as Doppler velocity oscillations within photospheric spectral lines (see Christensen-Dalsgaard 2002, and references within). The power spectrum of solar p-modes covers a distribution of multiplet frequencies, centered around oscillations with a period of approximately 5-minutes. 5-minute oscillations are observed within the umbral photosphere of sunspots, and are shown to be connected to the 5-minute global p-mode oscillations (Penn & Labonte 93; Balthasar et al. 1987; Braun et al. 1987). 3-minute intensity and velocity oscillations have been observed in the chromosphere above sunspots for over thirty years (Beckers & Tallant 1969; Beckers & 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 intensity propagations along diffuse, fan-like, coronal loop structures (Berghmans & Clette 99; Nightingale et al 1999, De Moortel 2002a). These propagations have velocities of the order ~100 km/s, short damping lengths, and are found to be periodic. 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. Depontieu et al. (2005) discuss the possibility of channeling the 5-min photospheric oscillations into the corona along the magnetic field. In Marsh & 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. It is now clear that slow magneto-acoustic modes are wave-guided and propagate along active region magnetic field. However, the photospheric p-mode driver of these waves has not been observed in conjunction with the observed response of the upper atmosphere to the passage of these waves. A complete, simultaneous, view of the atmosphere from the photosphere, chromosphere, transition region and corona is required. This will allow the driving, coupling and propagation of these magneto-acoustic p-modes to be investigated through the atmosphere. Combined imaging and spectroscopic observations will allow the effect of magnetic field geometry, bulk plasma flow, temperature and density, on the amplitude, frequency and phase of these modes to be investigated. References Balthasar, H., et al., 1987, Sol. Phys., 112, 37 Beckers, J.M., & Tallant, P.E., 1969, Sol. Phys., 7, 351 Beckers, J.M., & Schultz, R.B., 1972, Sol. Phys., 27, 61 Berghmans, D., & Clette, F., 1999, Sol. Phys., 186, 207 Braun, D.C., et al., 1987, ApJ, 319, L27 Brynildsen, N., et al., 2004, Sol. Phys., 221, 237 Cristensen-Dalsgaard, J., 2002, Rev Mod Phys, 74, 1073 De Moortel, I., et al., 2002a, Sol. Phys, 209, 61 De Moortel, I., et al., 2002b, A&A, 387, L13 De Pontieu, B., et al., 2005, ApJ, 624, L61 Fludra, A. 2001, A&A, 368, 639 Gurman, J.B., et al., 1982, ApJ, 253, 939 Lites, B.W., et al., 1982, ApJ, 253, 386 Marsh, M.S., et al., 2003, A&A, 404, L37 Marsh, M.S., & Walsh, R.W., 2006, ApJ, 643, in press Nightingale, R.W., et al., 1999, Sol. Phys., 190, 249 O'Shea, E., et al., 2002, A&A, 387, 642 Penn, M.J., & Labonte, B.J., 1993, ApJ, 415, 383 Rendtel, J., et al., 2003, A&A, 410, 315 Stein, R.F., 1967, Sol. Phys., 2, 385