XRT: WHI Filament cavities
2008-04-16T10:17:25 to 2008-04-16T14:48:08
Science Goal: One-Week Campaign #4: Quiet Sun (to occur on disk, near center), WHI ToO #1: Active Regions, WHI ToO #2: Equatorial Coronal Hole Study, WHI ToO #3: Activity in Filaments and Filament Channels
Program: WHI_Fillament_cavities
Target: QR
xcen=-650 ycen=-694
Instrument: XRT
HOP/JOP: 0
Description:
Daily Note: Yugma ID changes today
will be constant for next six months. Two-day plan. EIS: We would like to observe the southern polar coronal hole (boundary) for velocity maps of MK plasma. To be co-ordinated with SOHO. This is be in the plan uploaded today. Pointing: (0,-722), fixed (Harra and Gabriel). Observations: - EIS: 1"" slit scanning over a 140"" x 256"" area, running for 4 - 6 hours (SAA's permitting). - SOT: request Ca II FG over an area 140"" wide, on the disc, at a cadence that would allow you to support. (Maybe 4x4 binning.) - XRT: request ""normal"" polar dynamics programme (to be discussed). SOT: - WHI QS study support (McIntosh et al.). - SOT/SP O flat field. - Possible coordination with DST/IBIS. WHI ToO attempt: Cavity may be visible in NE on Wednesday, for Gibson et al. study. Be on the lookout for the return of last rotation's ARs (maybe on limb ~ 16 Apr).
Request to XRT HOP Number 0067: X-Ray Telescope [POC: Reeves] Filters: Al/poly (8 sec exposure), Ti/Poly (16 sec exposure) Cadence: ~30 sec cadence FOV: 250""x250"" centered on target region [capture aspects of global connectivity] Context: Al/poly (2048x2048, 2x2 binned), 5 thin Be (768""x384"" 23sec) every ~30 minutes Note: In the case of an active region on the sun, the long exposures can be replaced by multiple short exposures.
Other Instruments: STEREO/SECCHI SOHO/EIT SOHO/MDI TRACE Ground-based instruments (synoptic observations). (Consult web page - http://web.hao.ucar.edu/~sgibson/WHI/WHI-QS.html - for further details.)
Scientific Objectives: Our global objective is to make a detailed study of the response of the quiet solar chromosphere, transition region and corona to the constantly evolving photospheric magnetic field - these joint observations will show that there is no place in the solar atmosphere that is magnetically or dynamically quiet. With these observations we hope to gain reasonable estimates of the energy flux through the chromosphere and lower transition region. Further, this study will allow to study the structural elements [spicules, fibrils, mottles, etc] of the chromosphere and transition region, assess the relevance/importance of magneto-atmospheric [MA] wave energy versus direct magnetic energy release in the atmosphere below temperatures at which thermal conduction becomes significant. Further, we can use these observations to investigate MA mode generation, coupling and conversion as a result of photospheric motions and their interplay with magnetic structures. To reach the global objective we will need to make detailed measurements of the targeted magnetic environment, monitor the multitude of magneto-atmospheric waves and the radiative response of the plasma at multiple ""heights"" threading the atmosphere. We will perform the observations [detailed below] at chosen target locations during the WHI QS period.
Request to XRT HOP Number 0068: Hinode/XRT -- campaign contacts: Alphonse Sterling, and currrent XRT-CO. Filters: Al/poly (8 sec exposure), Ti/Poly (16 sec exposure) Cadence: ~30 sec cadence. FOV: 250""x250"" centered on target region [capture aspects of global connectivity]. Context: Al/poly (2048x2048, 2x2 binned), 5 thin Be (768""x384"" 23sec) every ~30 minutes. Note: In the case of an active region on the sun, the long exposures can be replaced by multiple short exposures.
Other Instruments: STEREO/SECCHI SOHO/EIT SOHO/MDI TRACE Ground-based instruments (synoptic observations). (Consult web page for further details.)
Scientific Objectives: To obtain multi-wavelength imaging and spectroscopic observations before, during and after any solar flares that may occur during the IHY Whole Heliosphere Interval (WHI
Carrington Rotation 2068: March 20 - April 16, 2008). The global objective is to make a detailed study of the response of the solar chromosphere, transition region and corona in and around an active region, to the constantly-evolving magnetic field. The manifestations of active regions extend from below the photosphere out through the solar atmosphere
and while flaring reconnection happens in the corona, its impact and influence extend down through the transition region and chromosphere. As such, we propose to probe those regions, and the interplay between the magnetic field and plasma motions (and magnetic and acoustic waves) and how these are affected by a solar flare.
Request to XRT HOP Number 0069: Hinode/XRT -- campaign contacts: T. Sakao. The primary observational interest is to take a series of long exposure (16s, or longer) XRT images with relatively thin filters (Ti-poly, or those more sensitive to low temperature coronal plasmas) with high or moderate exposure cadence (once in every 60s, or higher), in 512x512 FOV with 1x1 pixel binning, to identify sources of plasma outflows at or around low-latitude coronal holes. Occasional exposures with two different filters to obtain line-of-sight-averaged filter-ratio temperatures will also be performed. This would be made with Al-poly and Ti-poly filter pair.
Other Instruments: Other Instruments include: -------------------------- Various. Consult WHI web page for details. Further Details: ------------- More details can be found at the following page: http://ihy2007.org/WHI/WHI.shtml (especially under ""targeted observing plans"").
Scientific Objectives: To understand the origin of the solar wind from low-latitude coronal holes, including coronal hole boundaries by characterizing the physical properties of the coronal plasma (temperature, density, abundance, outflow velocity) with coordinated multi-spacecraft and ground-based observations in order to investigate the physical processes that lead to the origin of the solar wind. These observations would improve on previous studies by coordinating observations with a battery of instruments providing co-spatial, co-temporal and good coverage in heliocentric distance from the solar disk to solar wind locations over 1 AU. This study will combine spectroscopy, imaging, IPS and in-situ data to derive the plasma physical properties and the geometry of the coronal hole. The combination of these measurements would provide a 3-D view of solar wind properties. We are interested in observing holes producing fast or slow wind. Fast solar wind speeds above 600 km/s have been reported for large equatorial coronal holes (Nolte et al. 1976, Miralles et al. 2001a). Slower solar wind speeds were reported for low-latitude holes of smaller size, between 300 and 600 km/s, near solar minimum (Neugebauer et al. 1998). We are also interested in studying the temporal evolution of coronal and solar wind properties by monitoring plasma properties at different heights in the corona and in the solar wind during the campaign. Jets and plumes have been studied on polar holes, but there are not many studies of those in low-latitude holes. The contribution and role of both, plumes and jets, to the solar wind is still unknown. This campaign will also emphasize on identifying and tracing jets and plumes from the solar surface into the accelerating solar wind and determining their physical properties as a function of height and time.
Request to XRT HOP Number 0070: Hinode/XRT -- campaign contact Kathy Reeves Main Loop: Filters: Al/poly (8-16 sec exposure), Ti/Poly (16-23 sec exposure) Cadence: ~1.5 min for whole loop. FOV: 512""x512"". In the case of an active region on the sun, the long exposures can be replaced by multiple short exposures. Context: Al/poly (2048x2048, 2x2 binned), 5 thin Be (512""x512"" 23 sec) every ~30 minutes.
Other Instruments: TRACE -- campaign contact Kathy Reeves MLSO -- campaign contact Joan Burkepile HELIO -- campaign contact Sara Martin COMP -- campaign contact Steve Tomczyk Further Details: ---------------- More details can be found at the following page: http://ihy2007.org/WHI/WHI.shtml (especially under ""targeted observing plans"").
Scientific Objectives: To study filaments, filament channels, and filament cavities in order to (a) understand the time dependent, three dimensional density, temperature, and magnetic structure of filaments and filament channels and cavities (b) study how filaments form (c) study filament activation in the chromosphere and CMEs in the corona to better understand how this process works and how it is related to CMEs. In addition, if the observed structures erupt we will (d) study the evolution of the cavity during eruption, and (e) map the EUV signatures into the coronal structures as represented by the coronagraphs, with the goal of understanding more clearly the structure and manifestations of CMEs in the low corona.
