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HINODE Operation Plan (HOP)

accepted on


 HOP No.

 HOP title

HOP 0222

Chromospheric Solar Flares. Joint Observations with VTT/Gregor

plan term


@ @


 name : Rubio da Costa, Lagg, Krishnappa @  e-mail : rubio[at]mps.mpg.de

contact person in HINODE team

 name : Tarbell, Mariska @  e-mail : tarbell[at]lmsal.com

 abstract of observational proposal
We aim at an investigation of the impulsive phase of a flare by having multi-wavelength observations of the chromosphere and a comparison of the observations with the results from the RADYN radiative hydrodynamic code from Carlsson & Stein (1992, 1997) in order to determine the chromospheric response to non-thermal electrons.

During our observing campaign at the VTT/Gregor telescopes we are planning to use TIP (Tenerife Infrared Polarimeter, Collados et al., 2007). We will observe in He I (10830Å), covering the Si (10827Å), Ca I (10833.4Å) and Na I (10834.8Å) lines as well. We will also have the TESOS spectrometer (Kentischer et al., 1998) operating in H, with a FOV of 70" x 40" and/or the Gregor Fabry-Perot Interferometer (GFPI) at the Gregor Telescope. The PCO cameras will get imaging data in Ca II H, which will help us to coordinate precisely the pointing and co-align the images with the ones from HINODE.

The Hinode observations will compliment TIP and TESOS by determining the dynamic response of the chromosphere over a broader range of temperatures (EIS) and at different layers by studying the flare in different wavelengths (XRT and SOT).

 request to SOT
SOT will study the impulsive phase of flares: 109" x 109" FOV in Ca II H, G-band and red, green and blue continua at 60 second cadence. TESOS/GFPI and TIP-2  will be observing in H with its own cadence.

 request to XRT
It should point to an active region with a high probability of flaring and use its flare detection method to signal SOT and EIS as well. XRT should run in Standard Core Flare Program with 20 second cadence for the first 5 minutes, then 60 second cadence should be enough.
Rough estimate of the total data volume to be collected: 1800 Mbits for 4 hours.

 request to EIS
Run HH_Flare+AR_180x152H - this is a standard EIS flare study with the He II/256 line added.
Scanning sparse raster (2" slit, 6"steps) to catch flare impulsive phase.
Exposure: 9s, Raster duration: 5m 42s. Data Volume: 4.3 Mbit (JPEG75 - default), 5.1 Mbit (JPEG85)
Total data volume for 3hr: 140 Mbit (JPEG75)
Target: AR that is likely to flare
Notes for planners:
Centre raster on likely flare site in AR
Adjust raster repeat for maximum possible run time within TLM constraints
Default data compression is JPEG75 but for short timescale runs, use JPEG 85

 other participating instruments
VTT or Gregor with TIP-2: Stokes profiles in He I 10830 Å
TESOS/ GFPI: Spectrometry in H

Time period of proposed observations: We propose joint observations from Wednesday 17th October to Wednesday 24th October.

Time window in day: We require 3 hours per day, ideally from 09:00 UT to 12:00 UT.

Target of interest:
The target should be an active region with a high flaring probability (e.g. using the flaring probabilities given by SolarMonitor). The position on the solar disc is not important.

Our plan is to scan several times with a 2" slit an active region with a high change of flare occurrence in order to get the spectra of the impulsive phase of the flare.

The scheduling of the proposed HOP is determined by the seeing conditions in Tenerife at the time of the observing campaign, currently scheduled for 3 weeks in October 2012, with a priority for the flare program between 17th and 24th October. Typically, seeing conditions are good in the morning (09:00-12:00 UT). We therefore request that Hinode uses the XRT flare detection mode and observe the flares, preferably C1-class flare or greater.

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