XRT: AR Q90 1x1 512x512
2008-03-18T08:34:54 to 2008-03-18T17:59:54
Science Goal: WHI One-Week Campaign #1: Linking the Corona to the Solar Wind at Ulysses (to occur at the NE limb of the Sun), WHI ToO #1: Active Regions, WHI ToO #2: Equatorial Coronal Hole Study, WHI ToO #3: Activity in Filaments and Filament Channels
Program: AR_Q90_1x1_512x512
Target: AR
xcen=-1000000000 ycen=-1000000000
Instrument: XRT
HOP/JOP: 0
Description:
Daily Note: Observe AR all period AOCS: - For this week, orbital element upload to be performed on Tuesday, not on Monday. [Maintenance Note (Ishikawa), for CP/RT Toban] Command planning machines will be rebooted on Tuesday Mar. 18th 9:30-10:00 (JST). The machines for AOCS windows ,cpws ,cpwin will not be available during this time period. Please email to manager@solar.isas.jaxa.jp if you have any questions. Be sure to please write any subject 'manager: xxxxxxxx'.
Request to XRT HOP Number 0064: Hinode/XRT -- campaign contact: Taro Sakao, Alphonse Sterling. Filters: Al/poly, Ti/Poly filters appear adequate to image soft X-ray plume plasma. Occasionally thin/Be images may be taken to check on the presence of hotter material, possibly with longer exposures (~50 s).
Other Instruments: Various. See WHI main webpage. Further Details: ------------- More details can be found at the following page: http://ihy2007.org/WHI/WHI.shtml (especially under ""targeted observing plans"").
Scientific Objectives: Our main scientific objective is to derive the solar wind speed profile from coordinated SOHO/UVCS and radio scintillation data, over a wide range of heliocentric distances (2 to 50 R_sun), with the terminal wind speed being given by in situ Ulysses data. The goal of this study is twofold: on one side, we will provide the solar community with a composite wind speed vs. heliocentric distance profile based on measurements which refer to the same plasma parcels measured by different experiments at different distances - thanks to the SOHO-Sun-Ulysses quadrature configuration. While this is ""per se"" a valid objective, the wind profile we will come up to will serve as a benchmark input for the construction of a reference solar minimum heliosphere, as described later in this document. A further objective we aim to as a by-product of the campaign observations is to get a better understanding of polar plumes morphology and physical conditions, with special emphasis to their temporal variation, practically unknown so far. The role of plumes in solar wind is still to be ascertained, hence, although we will build a wind profile averaged over the plume/interplume plasma in our main objective, we also plan to contribute to a better understanding of the solar wind by investigating polar plumes. Observations from COMP will provide measurements of alfvenic plasma motions and pos magnetic field diagnostics from the limb to 1.4 solar radii in the 10747 and 10830 lines. These measurements will help characterize the magnetic structures present, their inclination and the multitude of wave motions present - essential to understanding the roots of the fast solar wind.
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.
Kotoku, J.
