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HINODE Operation Plan (HOP)

accepted on


 HOP No.

 HOP title

HOP 0119

Magnetic flux emergence - Joint campaign with CRISP/SST

plan term


@ @


 name : Carlsson @  e-mail : m.p.o.carlsson[at]astro.uio.no

contact person in HINODE team

 name : Hansteen @  e-mail : viggo.hansteen[at]astro.uio.no

 abstract of observational proposal
Magnetic flux emergence in quiet sun internetwork regions has been drawing attention due to recent progress in high-resolution observations. The launch of Hinode, and specifically the SP instrument, has allowed observers to detect the rising of hG horizontal magnetic loops in quiet Sun regions with no preexisting flux. Our aim is to observe both quiet Sun internetwork regions and active regions for magnetic flux emergence. We plan to follow the rising flux from its eruption through the photosphere and into the chromosphere, measuring the delay between the first manifestations of flux eruption in the photosphere until its effects on the chromospheric layers are visible. For this we aim at coordinating simultaneous observations from the SP instrument on board Hinode and the new CRISP spectropolarimeter recently installed on the Swedish 1-m Solar Telescope in La Palma. The objective is to combine CRISP's higher resolution, higher cadence and ability to measure full Stokes parameters in both the photosphere and chromosphere with SP's seeing-free and well-calibrated observations. Having simultaneous observations with both instruments will allow to calibrate the CRISP instrument and checking the sanity of its measurements. In addition, and if possible, we would like to observe with EIS to see if any larger scale changes in the transition region and coronal magnetic field configuration is evident as a result of emergence.

 request to SOT
Wavelengths: both 6302 Fe I lines.

  In the event of an AR present on the solar disk: use the 82"x82" FOV,
  normal mode (4.8 s/slit), single side mode (290 Mbits)

  If quiet Sun disk center, then use the 123"x123' FOV, normal mode
  (4.8 s/slit), single side mode (660 Mbits)

  Repeat scans until maximum data volume is reached.

 request to XRT

 request to EIS
EIS observations in multiple spectral lines covering a large range in temperatures. Either as a set of fairly low cadence rasters (such as defined in HH_FWHM_CAL_Norikura) taken at, say, hourly intervals of the same region to give a coranal/transition region magnetic field context, or (if telemetry restrictions allow) higher cadence slot observations (eg IUU_SLOT_148x400 or similar) to follow the changing field topology.

 other participating instruments

Time period of observations:
*  Start date: May 14, 2009 ; End date: May 19, 2009
  Reason: overlapping with our SST campaign.
*  Minimum # of observation days: 1 but preferably as many days in the period
  as possible to maximize the probability of catching good seeing on La Palma
*  Continuity of observations: if AR present, then observe as many days in the
  period as possible

Time window in day:
*  Minimum duration: 1 hour but preferably the 4 hours of highest probability
  of good seeing on La Palma: Start: 8:00 UT, End: 12:00 UT

Target of interest:
If available, active regions on the solar disk at any position; otherwise quiet Sun internetwork regions at disk center.

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