2013 Fiscal Year Research-status Report
Determining the Plasma Parameters of Solar Prominences
| Project/Area Number |
25800108
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| Research Category |
Grant-in-Aid for Young Scientists (B)
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| Research Institution | Kyoto University |
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Principal Investigator |
HILLIER Andrew 京都大学, 理学(系)研究科(研究院), 研究員 (80624650)
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| Project Period (FY) |
2013-04-01 – 2016-03-31
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| Keywords | Statistical analysis / Code Development / New analysis methods / 国際研究者交流（アメリカとイギリス） |
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| Research Abstract |
Over the past 1 year I have achieved the following:
1) The first statistical study of oscillations in a solar prominence. These results show that the prominence oscillations are driven by the convective motion in the lower atmosphere. Similar spectra of the oscillations were found to exist in the solar chromosphere. Further investigation of this data is revealing how waves propagate through the prominence.
2) Analytical modelling of the formation of the Rayleigh-Taylor instability in an exploding prominence. Through this modelling we were able to determine the magnetic field strength in the high corona, something that is impossible to directly measure.
3) Development of new model to calculate the velocity fluctuations in a prominence. These fluctuations allow for the first time the spatial structuring of velocity to be investigated, which is a crucial tool to understand turbulence in prominences. Once the turbulence in understood, the nature of the 'hidden' parameters of the prominence will become clearer.
4) Development of 3D numerical code to solve the dynamics of ionised plasma and neutral gas, coupling the two fluids with collisions. This code, called PIP, is now on the verge of full completion, and it can be viewed as a large advancement on my previous code. Using this code I will be able to investigate the wave and turbulence dynamics of prominences, as planned for this academic year (平成26) of the project.
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| Current Status of Research Progress |
Current Status of Research Progress
2: Research has progressed on the whole more than it was originally planned.
Reason
Though there has been a small delay in some of the observational projects planned to be completed during year 1, this is because new data has become available to me that will greatly improve the accuracy of the study. This new data is now available to me and work on its analysis has begun.
However, though this one slight delay does exist, other areas of the project are proceeding more smoothly than originally planned. Therefore, this project can be seen as one average progressing rather smoothly.
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| Strategy for Future Research Activity |
Due to the complexity of the magnetic field of prominences, simulations of both transverse and compressional waves will be performed in the prominence model developed by the PI to help understand the observed prominence waves. A study of the different wave characteristics will be performed, matching these with the observations with the aim of understanding the nonlinear waves in a complex magnetic topology. These will be performed with the new PIP code of which I have led the development.
The final step in analysing the waves in prominences will be to use the compressional waves to determine the effective adiabatic index for the first time. This will be accomplished by extending the method to determine the adiabatic index in the solar corona as described by Van Doorsselaere et al. (2011) . This will require a new set of prominence observations using Hinode EUV Imaging Spectrometer or using data from the recently launched IRIS satellite (NASA). This will be performed in conjunction with analysis of Hinode SOT data where my new method to determine the velocity of the prominence will be invaluable.
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| Expenditure Plans for the Next FY Research Funding |
The money will be used to attend scientific meetings, so that I can promote my results, and visit collaborators to develop my research. This is an essential part of the promotion and development of my scientific ideas, making it necessary for the completion of the project.
Other money will be used to buy hard disks to store the data my simulations and analysis produce. This is necessary money to maintain best practice standards for my scientific work.
Also money to pay for the publication of papers. This is essential to make my results available to the scientific community.
In the next fiscal year, I plan to attend the 8th Hinode science meeting (Portland, Oregon), the 14th European Solar Physics meeting (Dublin, Ireland) and Asia-Oceania Geosciences Society 2014 meeting (Sapporo) which are spread throughout the next year so that I can present my latest results to the scientific community. I will also plan to visit my collaborator in America to proceed with the development and publication of my results.
As stated above, money for hard disk storage and paper publication will also be used.
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