\documentstyle[11pt]{article}

%\renewcommand{\leftline}[1]{\noindent{#1}\\ }

\pagestyle{empty}

\begin{document}
\centerline{{\bf JOINT CDS/EIT/MDI/SUMER/TRACE PROGRAMME}}
\vspace{0.5cm}
\centerline{{\bf The Temperature Range of the Sunspot 3-minute Oscillations}}
\vspace{0.5cm}
\leftline{Per Maltby, Nils Brynildsen, Olav Kjeldseth-Moe, ITA, University of
Oslo}
\leftline{Edward Breeveld, MSSL/UCL, Surrey, UK }
\leftline{Richard A. Shine, Lockheed Palo Alto Research Laboratory}
\leftline{Klaus Wilhelm, Max--Planck--Institut f{\"u}r Aeronomie, Germany}
\leftline{{\small Received 25 December 1999}}
\leftline{{\small Modified 8 February 2000}}

\vspace{0.5cm}
\leftline{{\it Scientific Justification:}}
\vspace{0.5cm}
This programme builds on the knowledge obtained from JOP018 about the
3-minute oscillations above sunspots, see Brynildsen et al. 1999, ApJ 511, L121,
Brynildsen et al. 1999, ApJ 517, L159, Brynildsen et al. 1999, Solar Phys.,
in press, Maltby et al. 1999, Solar Phys., in press.
Briefly, simultaneous SUMER measurements of the intensity and the line-of-sight
velocity show that the observations in the chromosphere and the transition
region are compatible with the hypothesis that the oscillations are caused by
upward-propagating acoustic waves.

Most recently we have studied the intensity oscillations observed with the
TRACE 171~{\AA} channel above the sunspot NOAA 8580, observed on 15 June 1999.
The power spectrum of the observation shows a maximum at 6.2 mHz,
corresponding to a period close to 160~s.
These 171~{\AA} intensity oscillations may be an extension of the sunspot
transition region oscillations into the corona.
However, this result is uncertain since the oscillations occur in an
area where the emission in the 171 channel is weak, most likely because
the coronal Fe~{\scriptsize IX/X} emission is weak.
Hence, without simultaneous spectroscopic observations we cannot exclude
the possibility that transition region lines, such as O~{\scriptsize VI} at
$\lambda$$\lambda$172.93, 173.08 contribute to the oscillations in the 171
channel.

To evaluate the feasibility of deriving spectroscopic information from
the CDS Grazing Incidence Spectrometer (GIS) we have studied GIS
observations of the sunspot in NOAA 7981, observed on 2 August 1996.
Comparing the results for different locations in the NOAA 7981 sunspot region
the GIS observations show that the contribution from the O~{\scriptsize VI}
$\lambda$$\lambda$172.93, 173.08 lines to the total emission within the
171 channel ranges from 3\% to 17\%.

\clearpage

We plan to increase our knowledge by simultaneous observations with:

\begin{itemize}

\item At least three wavelength bands of the CDS Grazing Incidence Spectrometer
(GIS). The intension is to measure the relative contributions of such transition
region lines as O~{\scriptsize VI} $\lambda$$\lambda$172.93, 173.08,
Ne~{\scriptsize VII} $\lambda$465.22, and O~{\scriptsize V} $\lambda$760.40,
to the intensity oscillations.

\item SUMER observations of the transition region lines O~{\scriptsize V}
$\lambda$629, N~{\scriptsize V} $\lambda$1238, $\lambda$1242 and the
chromospheric Si~{\scriptsize II} $\lambda$1260 line.

\item TRACE observations in the 171 channel with high cadence.

\item EIT when possible: observations in the 171 channel with high cadence.

\item MDI when possible: Doppler velocities and magnetic field measurements, 
with 
high spatial resolution and high cadence.
\end{itemize}

Note that CDS, SUMER and TRACE should be run without compensation for
solar rotation. The starting position is in front of the sunspot, letting
the solar rotation move the sunspot over the slit. Phase 1 (CDS and
SUMER) should be repeated until the image of the sunspot has moved
across the slit, then Phase 2 should run once. TRACE should repeat
Phase A + B during the whole study.

\bigskip

\centerline{CDS}

\leftline{Phase 1:}
\leftline{GIS Study: O{\_}SPOT10}

\leftline{Spectrometer: Grazing Incidence}
\leftline{Slit: 4$\times$4 arcsec}
\leftline{Raster Area: 4$\times$4 arcsec}
\leftline{Step (DX, DY): 0 arcsec, 0 arcsec}
\leftline{Raster Locations: 145}
\leftline{Exposure Time: 17 seconds}
\leftline{Duration of Raster: 2732 seconds}
\leftline{Number of Rasters:   1}
\leftline{Total Duration:  2732 seconds}
\leftline{Line Selection: Full GIS output}
\leftline{Pointing: Sunspot}
\bigskip

\leftline{Phase 2:}
\leftline{NIS Study: O{\_}SPOT2}

\leftline{Spectrometer: Normal Incidence}
\leftline{Slit: 2$\times$240 arcsec}
\leftline{Raster Area: 120$\times$120 arcsec}
\leftline{Step (DX, DY): 2 arcsec, 0 arcsec}
\leftline{Raster Locations: 60 x 1 = 60}
\leftline{Exposure Time: 20 seconds}
\leftline{Duration of Raster: 1430 seconds}
\leftline{Number of Rasters:   1}
\leftline{Total Duration:  1430 seconds}
\leftline{Line Selection: Mg VIII 315.02, Fe XIV 334.17, Fe XVI 360.76,}
\leftline{Mg IX 368.06, He I 522.20, O IV 554.52,Ne VI 562.83,}
\leftline{He I 584.33, O III 599.59,O V 629.73}
\leftline{Bins Across Line:  21}
\leftline{Telemetry/Compression: truncate to 12 bits}
\leftline{Pointing: Sunspot}
\bigskip

\centerline{SUMER}
\bigskip
\leftline{Phase 1:}
\leftline{Study: o{\_}spot3{\_}osc}
\leftline{Duration:  47 minutes}
\bigskip
\leftline{Study: o{\_}spot3{\_}osc{\_}f}
\leftline{Duration:  46 minutes (n times)}
\bigskip
\leftline{Phase 2:}
\leftline{Study: o{\_}spot3{\_}rast}
\leftline{Duration:  34 minutes}
\bigskip

\centerline{TRACE}

\leftline{Phase A:}
\bigskip
\leftline{Channel: WL}
\leftline{Exposure Time: 0.0032 seconds ?}
\leftline{Image Area: 768 pixels$\times$768 pixels}
\leftline{Pixel size: 0.5 arcsec}
\leftline{Number of images: 1}
\leftline{Duration:  0.0032 seconds}
\leftline{Pointing: Sunspot}
\bigskip

\leftline{Phase B:}
\bigskip
\leftline{Channel: 171}
\leftline{Exposure Time: 17 seconds}
\leftline{Image Area: 768 pixels$\times$768 pixels}
\leftline{Pixel size: 0.5 arcsec}
\leftline{Number of images: 160}
\leftline{Duration:  2720 seconds}
\leftline{Pointing: Sunspot}
\bigskip

\centerline{EIT}

\leftline{For a limited data set: Channel 171 with high cadence}

\centerline{MDI}

\leftline{When possible: Doppler velocities and longitudinal magnetic field 
with high cadence}

\end{document}


