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HINODE Operation Plan (HOP)

accepted on

23-feb-2017


 HOP No.

 HOP title

HOP 0335

Observation-Driven Modelling of Solar Phenomena

plan term

ToO
2017/04/03-2017/04/10

@ @

proposer

 name : Madjarska on behalf of an ISSI team
Klaus Galsgaard (leader), Brian Welsch, Fernando Moreno-Insertis,
Gudiksen, Bourdin, Bradshaw, Kazachenko, Mou
@  e-mail : mariamadj[at]gmail.com madjarska[at]mps.mps.de welsch[at]ssl.berkeley.edu kg[at]nbi.ku.dk

contact person in HINODE team

 name : Shine @  e-mail : shine

 abstract of observational proposal
Main Objective:
In order to reach a new level of understanding of both large and small-scale solar phenomena, it is important to make increasingly realistic models that will allow a greater synergy between observations and models. The main objective of the proposed IHOP is to obtain Hinode SP & EIS and IRIS co-observations of coronal bright points that will be used for a fundamentally new approach in modelling solar phenomena called observation- (or data-) driven modelling, in which the required gboundaryh conditions for realistic numerical models are directly obtained from observations.

Scientific Justification:
For a theoretical model to accurately represent the physical evolution of the solar atmosphere, the model must, minimally, be consistent with observations of the modelled system. Accordingly, a starting point for modeling such systems is to directly incorporate information obtained from solar observations, both to determine the modelfs initial state and to evolve the model forward in time over a given period. Progress has already been made on (i) extracting static magnetic field models for initial conditions - from potential-field to Non-Linear, Force-Free Field models - from observations, and (ii) deriving time-dependent boundary velocity and/or electric field components at the photosphere to evolve dynamic models forward in time. Employing such information, combined from various solar observations, in Magneto-Hydro-Dynamic (MHD) models will, however, require further exploration and development before such models are capable of producing results that can compare directly with corresponding observations. In this project, we attack open problems in the process of running such gobservation-drivenh simulations.

In particular, we shall investigate the development of small-scale magnetic structures, such as Coronal Bright Points. Our goal is to go from observations, through MHD modeling, to forward modelling, with the aim of eventually providing synthetic observations that can be directly compared with the original observations.

We have created a team of researchers that will combine their expertise to solve a number of critical issues as a necessary step to lay the groundwork for this fundamentally new approach in solar physics research. The first step of this research project is to acquire suitable solar observations that include high-resolution, high-cadence vector magnetic field observations coupled with imaging and spectral information of Coronal Bright Points. Although the Helioseismic and Magnetic Imager onboard the Solar Dynamic Observatory provides full disk vector magnetograms, the transverse component strength in quiet solar regions is not sufficient for the purpose of our study and we, therefore, require observations from the Spectropolarimeter (SP) on board Hinode combined with EIS and IRIS spectral co-observations. We have searched the whole SP archive for suitable data (please see below the SP/EIS/IRIS data requirements), but unfortunately we have not found any suitable dataset. The vector magnetic field data are crucial for deriving the time-dependent boundary velocity and/or electric field components at the photosphere to evolve dynamic models forward in time, while the spectral IRIS and EIS data are essential for the forward modelling.

 request to SOT
SP
Field-of-view - minimum 60" x 60"
Cadence - 12 min
Duration - minimum 2 hrs

 request to XRT
None

 request to EIS
Study: BP_response1_raster; ID #562
Mode: raster
Exposure time: 30 sec
Slit: 2"
Duration: 56m 30s min (2 raster repeat), please repeat the study to fill the time slot
Volume: 30 Mb
Target(s) of interest: Coronal Bright Point, TOO
Target: Coronal Bright Point, Target of opportunity
Remark: The study now includes an exposure time of 30 sec.

 other participating instruments
IRIS: OBS-ID: 3600011676 and 3600261676.
Additional instrument coordination: none

 remarks
Dates: TOO; 4 runs during March, April or June (Madjarska is not available in May) Time window: minimum 2 hrs uninterrupted

Previous HOP information:
Madjarska was a proposer of 4 HOPs and co-proposer of another 4.
Madjarska is the author/co-author of 11 refereed papers based on Hinode data plus one more submitted for publication in ApJ (a statistical study based on numerous EIS datasets). She has been a co-supervisor (primary) of 3 PhD theses that were based on Hinode data. Currently she co-supervises one student working on Hinode data and one on IRIS data.

Madjarska is the co-author of 5 IRIS refereed papers.

Additional Remarks:
Pointing: Requires "last minute" spacecraft pointing adjustment because of the short lifetime (often up to 24 hrs) of the BPs. This is to be achieved by re-pointing Hinode just after the AOCS table upload (non-upload day). The table should be updated as close as possible to the observations. David Brooks is willing to help during his CP shifts by selecting and adjusting the pointing in communication with Maria Madjarska.

The study requires target tracking, i.e. compensation for the solar rotation.

The BP target should be selected at solar disk coordinates XCEN > - 300", < 300" and YCEN >- 300", and <300", i.e. as close as possible to the disk center because of the magnetic field observations.

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