JOP149 Onset on flaring activity and Coronal mass ejections

between space and ground based instruments in Europe (Poland, 
Ondrejov, Canaries....).

Received: September 7, 2001

List of applicants:

B.Schmieder, Mein P., Malherbe J.M., Vilmer N., van Driel L., Mein N.
Tziotziou K. (Observatoire de Paris),
Vial J.-C. ( IAS Orsay)
 J.Staiger (KIS), 
 Heinzel P. (Ondrejov CS), 
Kucera T. and Poland A.(GSFC),
DeLuca E., and Golub L. (Harvard-Smithonian Center for Astrophysics)
Rompolt B., Rudawy P. ( Wroclaw , Poland).

For the  ground based instruments we have 2 windows of possible supports :

October : 3-10 included

- VTT  at Tenerife
        Time allocation 3-10 Oct (8-18 UT)
        H-alpha and Ca 8542 observation with the MSDP: profiles, intensities 
        and velocities

October 18-23 (during the MEDOC campaign)
       this jop or the JOP 131: Spectro-polarimetric diagnostics
        of prominences and filaments

- THEMIS
        Time allocation 18-23 Oct  (8-18 UT) 
       . Halpha 6563, 
       . Ca II 8542 line with the MSDP: profiles, intensities and velocities.
          The choice of this line is suggested by previous results:
          Yuan Yong Deng et al. A&A,1999, 349, 927, 
           P.Mein et al A&A 2000, 555,1146,
       . Magnetic field in Na D1
       . slit jaw (Halpha) filter
-CDS   Bright regions in the TR lines correspond often to network,
             locations where the magnetic field in enhanced.
             We would like to check  the destabilization
             of filaments at their footpoints due either to EMF or flux
             cancellation. We expect to see new bright regions close to the
             footpoints or moving bright features.
             He and OV lines would be useful to align all the observations.

        For all these purpose we want to use the studies:  EFINAR1
                                                           EFINAR2
                                                           FILOBS1

- SUMER - 
        3-10 October No observation with SUMER in this JOP: AR would be on 
        the disk, not on the SUMER slit at x=-980 

        17-23 October JOP 131 " spectro polarimetric diagnostics of 
        fil/prominences" if opportunity

- EIT -  

 -1- CME watch with your possible cadence (17 mn) will be the basis-program
     for our two programs.

 Occasionally, if the target needs it, we shall ask the possibility to run:

either :
 
 -2-  Active region program ( full resolution, 1/4 Sun ) at 195 A
      for 2 to 4 hours (with the highest cadence as possible).
or

 -3- Filament eruption program at 304 A, also full resolution, also for
     2 to 4 hours (with the highest cadence as possible)

  We shall ask only one of these two items ( item 2 or item 3) by day.

- MDI -
      . One large full disc magnetic map each 96 mn will be sufficient.
        This will be a good extension to the THEMIS observations,
        permitting magnetic fields extrapolations. THEMIS providing fast 
        observation and MDI large field of view
        
        Observations are required between 8 and 18 UT.
        The target and precise schedule will be given daily.   
   

- TRACE - 

      - Program 1
      The coronal loops are good diagnostics to derive the magnetic field 
      lines and to study the interaction of emerging and pre-existing magnetic
      fields. With MDI and THEMIS we would have data of photospheric magnetic
      fields. Magnetic extrapolation allows to understand where the energy 
      can be released. Separatrices and bald patches (Demoulin et al.) would
      be computed and compared with the bright regions.               
         
      - Program 2.
      We would like to continue our program on the absorption of coronal
      lines by H and He continua. We would derive the hydrogen column density
      of the cold plasma related to the destabilization of filaments.
      Halpha and CaII lines giving more informations on electron density
      and temperature
      
      For these two programs, we would like to observe 171, 195 A lines and 
      white light during our observing times ( 8 - 18 UT).

- Yohkoh SXT
       As we expect flares, soft X-ray images of the AR, are required as
       frequently as possible.

-if HESSI  is operating we will be happy to collaborate

Scientific motivation of the program:

 Onsets of Flaring Activity and Coronal Mass Ejections.

                             1.Introduction:

Recent observations have shown that the ejection of plasma from the
Sun, called coronal mass ejection (CME) is the major cause of
interplanetary shocks and geomagnetic storms. Although a number of
studies give insight, until now, the physical mechanism which causes
CME initiation is unclear.

Multi wavelength studies are required to determine what causes the
CME.  We would like to be able to detect the magnetic origin, the
dynamics of the plasma at different temperatures. We expect that a
campaign involving ground based instruments ( in particular Canaries
telescopes: THEMIS,VTT) and space instruments (SOHO,TRACE,
HESSI,Yohkoh) would provide information on the causes of CMEs: new
emerging flux at the solar surface dynamics of the phenomena (filament
eruption, ejection) reconnection and flaring process

                         2. Aim

Earlier it was suggested that a CME was initiated by the impulsive
expulsion of the overlying corona due to the energy released from the
associated flare. However this suggestion was not supported by
observations. Many CMEs are not accompagnied by flares. Furthermore,
it was pointed out that CMEs are found to precede or at best to start
at about the same time, as the associated flare.  The recently added
capability of SOHO/Yohkoh and TRACE observations significantly
improved our ability to determine the relative times of flares and
CMEs.  Only half or less than half of CMEs are directly related to
flares in active region.  Some filament eruptions are precursors of
CMEs but no statistics are really convincing.

On the 31 may 1997, in the frame of a SOHO (SUMER, CDS, EIT, LASCO,
MDI) JoP 17 coordinated with the MSDP at Pic du Midi, we could observe
a disappearing filament in H$\alpha$ and related its disappearence to
large velocities observed in Lyman lines and to a CME observed by
LASCO. (Schmieder et al. 2000 A et A, 358, 728).

The H$\alpha$ observations stopped too early (because of clouds),
SUMER and EIT started too late, thus we could not really have a good
timing of the event. We would like to obtain new observations of CMEs
and related active phenomena in the low atmosphere. Observations of
the magnetic field in the photosphere, the Dopplershifts in the
chromosphere, in the corona, and images of CMEs are suitable.

                     3.  Data set needs

We propose a coordinated campaign involving ground based instruments
as well as space instruments. On the ground THEMIS will provide the
magnetic field vector at different altitudes in the solar atmosphere,
VTT/MSDP the dynamics of the chromosphere, in space SOHO/SUMER CDS,
EIt will give information on the transition region and coronal
plasma. TRACE will give a 3D view of coronal loops, HESSI the X rays
coming from the flaring regions.

    Multiwavelength campaign in coordination with satellites :\\
    SOHO ( Vial J.-C., Kucera T, Poland A.\\
    TRACE ( De Luca E., Golub L.)\\
    Yohkoh  \\
    HESSI (Vilmer N.) \\

   and ground-based observatories:\\

    VTT - MSDP (Schmieder B., Mein P.) Bidimensional spectroscopy in 
    Halpha line. 
    Sequences with good time resolution for active phenomena,
    reconnections, mass ejections, instabilities connected with CMEs...\\
    
    THEMIS - (Mein P.) MSDP mode : 4 lines   with good
    time resolution and polarization analysis  
    to get the stratification of the magnetic field and the chromospheric 
    dynamics.\\  
    
    Ondrejov - ( Heinzel P.) Spectroscopy in Balmer lines. 

    Nan\c{c}ay - ( Vilmer N.) radio-heliograph observations
  
    Wroclaw - (Rompolt B.) filtergrams and bidimensional spectroscopy in 
    chromospheric lines\\
   

           4.  Project management plan

The campaign coordinator will distribute the target of the
observations to all the observatories from China, Europe and US which
are interested to follow the campaign.

           5. Results of previous campaigns.

The results obtained with previous international campaigns are
published in teh reference list.  They concern: the 3D magnetic
configuration of prominence, and active regions the signatures of
emerging flux in the chromosphere and corona, the formation of
sunspots fibrils, diagnostics of densities of cool structures. \\

 van Driel,L, Schmieder B.,  Gauzzi G., Mein N., Hofmann A., Nitta N.,\\
 Kurokawa H.,  Mein P. and Staiger J.:\\
   X Ray Bright Point Flares due to Magnetic Reconnection\\
 1996, {\it Sol. Phys.}, 163, 145.\\

Mein P., Mein N., Malherbe J-M., Heinzel P., Kneer F., Von Uexk\"ull M.
and Staiger J.\\
Flare multi-line 2D-spectroscopy\\
1997, {\it Sol. Phys.}, 172, 161.\\

Aulanier G. and D\'emoulin P.\\
 3-D magnetic configurations supporting prominences. I The natural 
presence of lateral feet\\
1998, {\it Astron. Astrophys.}, 329, 1125.\\

 Aulanier G., D\'emoulin P., van Driel-Gesztelyi L., Mein P.,De Forest C.\\
 3-D magnetic configurationss supporting prominences. II The lateral feet 
as a pertubation of a twisted flux-tube\\
 1998, {\it Astron. Astrophys.}, 335, 309.\\

 Malherbe J.M., Schmieder B., Mein P., Mein N., van Driel-Gesztelyi L. and
 von Uexk\"ull M.\\
 Arch Filament systems associated with X-ray loops\\
1998, {\it Sol. Phys.}, 180, 265.\\

 Aulanier G., D\'emoulin P., Mein N., Van Driel-Gesztelyi L., Mein P. and
   Schmieder B. \\
 3-D Magnetic Configurations Supporting Prominences:
III - Evolution of fine structures observed in a filament channel\\
 1999, {\it Astron. Astrophys.}, 342, 867.\\

Heinzel P., Mein N. and Mein P.\\
Cloud model with variable source function for solar Halpha structures
II - Dynamical models\\
1999, {\it Astron. Astrophys.}, 346, 322.\\

Rudawy P., Van Driel-Gesztelyi L., Cader-Sroka, Mein P., Mein N., Schmieder B., 
Malherbe J-M. and Rompolt B.\\
Analysis of evolution of NOAA7912 active region on 19 October 1995\\
1999, {\it Astron. Astrophys. Suppl.}, 139, 89.\\ 

Kucera T.A., Aulanier G., Schmieder B., Mein N. and Vial J-C.\\
Filament channel structures in a SiIV line related to a 3D magnetic model\\
1999, {\it Sol. Phys.}, 186, 259.\\

Tziotziou K., Heinzel P., Mein P. and Mein N.\\
Non-LTE inversion of chromospheric CaII cloud-like features\\
2001, {\it Astron. Astrophys.},366, 686.\\

Mein N., Schmieder B., DeLuca E., Heinzel P., Mein P., Malherbe J-M. and
Staiger J.\\
A study of hydrogen density in emerging flux loops from a coordinated
TRACE and Canary Islands observation campaign\\
2000, {\it ApJ}, 556, 438