Distribution and dynamics of the solar magnetic flux in the photosphere and heliosphere
ROSES ID: NNH06ZDA001N Selection Year: 2007
Program Element: Independent Investigation
Principal Investigator: Valentyna Abramenko
Affiliation(s): Big Bear Solar Observatory
Project Member(s):
Yurchyshyn, Vasyl Co-I New Jersey Institute of Technology
Zurbuchen, Thomas H Co-I University of Michigan
Fisk, Len Co-I University of Michigan
Summary:
This proposal is being written in response to a request by the TRT focus team
on "Solar and Heliospheric Magnetic Field" led by T.H. Zurbuchen, University of
Michigan. The team, and especially its lead, have encouraged to propose for a
third year of funding to allow a successful completion of the focus team work.
The need for this proposal arises from two reasons. First, our initial proposal
extended only over two years. We are well on the way to achieving the
statements of work (SOW) for this initially proposed research. Second, in
response to team-objectives, we have adjusted our SOW to be of maximum help to
the focus team and our work is now well connected to other parts of the
team-work.
During the first year of our collaboration we have analyzed dynamics of
emergence of new dipoles inside coronal holes and in adjacent quiet-Sun areas.
We have shown for the first time that the dipole emergence rate of the
magnetic flux inside coronal holes is suppressed as compared to the quiet sun
areas. This finding agrees with the idea that coronal holes are formed at
location where the dipole emergence rate is low and therefore open magnetic
flux can be accumulated at these places (theory of the coronal holes formation
and solar wind acceleration, Fisk 2005). This theory suggests that
reconnection between open magnetic flux and closed magnetic loops is an
essential diffusion mechanism for open filed lines.
We are currently improving and modifying our existing algorithms and numerical
codes to calculate power spectra of magnetic field fluctuations (both spatial
and temporal) as well as high statistical structure functions, which would
allow us to derive flatness functions and filling factor and estimate
intermittency of the magnetic field both in the photosphere and in the solar
wind. This analysis will then be compared to the results of other team members
(both observational and theoretical). Our funding is likely to run out before
the completion of this collaboration, which is an important part of the work
by the focus team.
During the third year, we will study magnetic flux distribution in the
photosphere both inside and outside of coronal holes. We intend to apply our
techniques to photospheric and solar wind measurements. Conclusions and
parameters obtained from the study will be used as input date
and/or constrain the models of coronal hole formation and solar wind
acceleration developed by our focus team.
Publications:
Performance Year | Reference | Investigation Type | Actions |
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1 | Abramenko, Valentyna; Yurchyshyn, Vasyl; Wang, Haimin; ...
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Presentations:
Performance Year | Reference | Actions |
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1 | Abramenko, Valentyna; Pevtsov, A.; (2007), Magnetic Diss...
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1 | Abramenko, V.; Yurchyshyn, V.; Wang, H.; (2008), Interm...
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1 | Abramenko, Valentyna; (2009), How the Magnetic Flux Insid...
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1 | Abramenko, Valentyna; (2011), Turbulent Diffusion on Very S...
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