Title: Eruptive and quiescent prominences Atlas with SOHO and Hinode Short title : Eruptive and quiescent prominences Atlas Authors: S. Parenti(1), N. Labrosse(2) and J.-C. Vial(3) (1). Royal Observatory of Belgium, Be (2). University of Glasgow, UK (3). I.A.S., Universite Paris Sud-CNRS, Fr Contact: s.parenti @ oma.be Update History: First Draft (January 17, 2008) Participating instruments and observatories SOHO/SUMER SOHO/CDS Hinode/XRT Hinode/SOT Hinode/EIS Scientific Justification The information contained in a spectral atlas is of prime importance to determine as many physical parameters of the observed structure as possible with the smallest uncertainties. These physical conditions determine the slow evolution of prominences and the instabilities which lead to their eruptions, in some cases to Coronal Mass Ejections in the context of space weather. Parenti at al. 2005a built a FUV spectra atlas of a quiescent prominence and QS using the SUMER spectrometer in the waveband 800-1250 A (detector A). They derived non-thermal velocities (NTV), Differential Emission Measure and pressure (Parenti & Vial 2007), which were used to investigate the energy balance. Parenti at al. 2005b also derived the electron temperature from the H I Ly-continuum. Vial et al 2007 investigated the H I Ly-alpha/ Ly-beta ratio showing its potentiality to diagnose geometrical and thermodynamic properties of prominences. Labrosse et al. 2007 studied the effect of radial motions of an erupting prominence on the He resonance lines to investigate the diagnostic possibilities using SOHO and Hinode. The results achieved until now require further coordinated investigations aiming at the following specific targets: * Extending the existing atlas of quiescent prominence over a larger range of temperatures and a consequently a larger waveband * Building a dedicated atlas for an activated prominence These results will be of great importance to contribute to several issues raised by these authors: - To quantify and model the H I and He I continuum absorption - To better constrain the models with the H I and He lines - To better constrain the Prominence Corona Transition Region (PCTR) and the coronal environment - To further study the dynamic of the PCTR (Doppler shift and NTV, dimming) - To compare these plasma properties for quiet and activated prominences The simultaneous use of SOHO/SUMER-CDS, and Hinode instruments will be of great advantage for the purposes above mentioned. SUMER will cover the full waveband on detector B (660 - 1500 A, first order) in order to complement the Parenti at al. 2005a existing atlas and to study the H I Lyman series in line with Vial et al. 2007 work. CDS observations will extend the atlas towards lower wavelengths, including the He I 584 A and the He II 304 lines, proven to be very useful for diagnostic (Labrosse et al. 2007). EIS will provide critical information on the line profiles at shorter wavelengths. In particular, the data will be used for studying the He continuum absorption and the He II 256 A line. EIS will also produce a context image of the observed prominence. SOT will provide morphology and dynamic information of the cooler part of the prominence. XRT will be used to study the prominence cavity and surrounding hot environment. This first campaign will be followed by the request for a second one, possibly in autumn 2008, which will aim at THEMIS magnetic field measurements in prominences. Detailed Observing Sequences per Instrument The pointing should be at quiescent or erupting prominence. Targets of opportunity will be chosen on the basis of their probability of eruption. CDS, SUMER and EIS studies should be run also on QS, on the same day of the prominence and at Sun centre if possible. SUMER: Full spectra on detector B. Slit 1" x 120", exposure time 100 sec. The SUMER slit should possibly include some off-limb corona. A full spectrum taken in the off-limb corona at the height of the prominence will be useful for evaluating the background/ stray light. CDS: Full NIS spectra. Study to be run: NISAT_S5, var 9, a raster of 40" x240". SOT: Ha center: half FOV (160"x160") 2x2 sum and CaII H: half FOV (108"x108") 2x2 sum 15 s cadence. Ha doppler : +/- 208 mA. To be run before and after Ha center. Depending on the prominence morphology, the FOV may be extended and the cadence reduced. XRT: XOB#: 1371 Filter : Al/Poly FOV : 512x512" with 1x1"-res and 2048x2048" with 2x2"-res Exposure : non-saturated AEC and 4096 msec (fixed) cadence : 30 s and 1 min Occasionally the Gband EIS: Slot of 266" at He II 256 A for a context image before and after the spectra sequence. Rastering with full EIS spectra (e.g. study HPW008_FULLCCD_RAST or similar).