Structure of convective flows on supergranular scales in the solar photosphere
The exploration of the velocity field of the real solar convection was performed using neutral iron line λ ≈ 639.3 nm profile from the observations with high spatial resolution. The inverse procedure was applied for each profile to reproduce the velocity field in the solar photosphere. Acoustic wave...
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| Published in: | Advances in Astronomy and Space Physics |
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| Date: | 2012 |
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| Format: | Article |
| Language: | English |
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Головна астрономічна обсерваторія НАН України
2012
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| Online Access: | https://nasplib.isofts.kiev.ua/handle/123456789/119189 |
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| Journal Title: | Digital Library of Periodicals of National Academy of Sciences of Ukraine |
| Cite this: | Structure of convective flows on supergranular scales in the solar photosphere / O.A. Baran // Advances in Astronomy and Space Physics. — 2012. — Т. 2., вип. 2. — С. 153-156. — Бібліогр.: 14 назв. — англ. |
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Digital Library of Periodicals of National Academy of Sciences of Ukraine| _version_ | 1862678977535016960 |
|---|---|
| author | Baran, O.A. |
| author_facet | Baran, O.A. |
| citation_txt | Structure of convective flows on supergranular scales in the solar photosphere / O.A. Baran // Advances in Astronomy and Space Physics. — 2012. — Т. 2., вип. 2. — С. 153-156. — Бібліогр.: 14 назв. — англ. |
| collection | DSpace DC |
| container_title | Advances in Astronomy and Space Physics |
| description | The exploration of the velocity field of the real solar convection was performed using neutral iron line λ ≈ 639.3 nm profile from the observations with high spatial resolution. The inverse procedure was applied for each profile to reproduce the velocity field in the solar photosphere. Acoustic waves were removed by k − ω filtration. To study supergranulation in the solar photosphere we selected motions with horizontal velocities less than 0.5 km/s. As the lifetime of the supergranule is larger than the observation time, we have averaged images of the vertical velocity in time. Supergranulation becomes more apparent on the distribution of the vertical velocity (the range of ∆V variations on the supergranular scales is constrained by ∼ 0.04 km/s). The velocity field within such cells has been studied and compared with the distributions of the vertical velocity on smaller scales. The upward supergranular flows expand with height and intensify (as distinct from decreasing of the velocity variations on the smaller scales), and the distribution of the line of sight velocity inside supergranular flows becomes more asymmetric in the higher layers of the photosphere. The downward supergranular flows are more compact and have a complicated structure too.
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| first_indexed | 2025-12-07T15:42:17Z |
| format | Article |
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| id | nasplib_isofts_kiev_ua-123456789-119189 |
| institution | Digital Library of Periodicals of National Academy of Sciences of Ukraine |
| issn | 2227-1481 |
| language | English |
| last_indexed | 2025-12-07T15:42:17Z |
| publishDate | 2012 |
| publisher | Головна астрономічна обсерваторія НАН України |
| record_format | dspace |
| spelling | Baran, O.A. 2017-06-04T19:38:40Z 2017-06-04T19:38:40Z 2012 Structure of convective flows on supergranular scales in the solar photosphere / O.A. Baran // Advances in Astronomy and Space Physics. — 2012. — Т. 2., вип. 2. — С. 153-156. — Бібліогр.: 14 назв. — англ. 2227-1481 https://nasplib.isofts.kiev.ua/handle/123456789/119189 The exploration of the velocity field of the real solar convection was performed using neutral iron line λ ≈ 639.3 nm profile from the observations with high spatial resolution. The inverse procedure was applied for each profile to reproduce the velocity field in the solar photosphere. Acoustic waves were removed by k − ω filtration. To study supergranulation in the solar photosphere we selected motions with horizontal velocities less than 0.5 km/s. As the lifetime of the supergranule is larger than the observation time, we have averaged images of the vertical velocity in time. Supergranulation becomes more apparent on the distribution of the vertical velocity (the range of ∆V variations on the supergranular scales is constrained by ∼ 0.04 km/s). The velocity field within such cells has been studied and compared with the distributions of the vertical velocity on smaller scales. The upward supergranular flows expand with height and intensify (as distinct from decreasing of the velocity variations on the smaller scales), and the distribution of the line of sight velocity inside supergranular flows becomes more asymmetric in the higher layers of the photosphere. The downward supergranular flows are more compact and have a complicated structure too. The authors are grateful to Dr. N. G. Shchukina for kindly proving the results of observations and to Dr. R. I. Kostik for data reduction. en Головна астрономічна обсерваторія НАН України Advances in Astronomy and Space Physics Structure of convective flows on supergranular scales in the solar photosphere Article published earlier |
| spellingShingle | Structure of convective flows on supergranular scales in the solar photosphere Baran, O.A. |
| title | Structure of convective flows on supergranular scales in the solar photosphere |
| title_full | Structure of convective flows on supergranular scales in the solar photosphere |
| title_fullStr | Structure of convective flows on supergranular scales in the solar photosphere |
| title_full_unstemmed | Structure of convective flows on supergranular scales in the solar photosphere |
| title_short | Structure of convective flows on supergranular scales in the solar photosphere |
| title_sort | structure of convective flows on supergranular scales in the solar photosphere |
| url | https://nasplib.isofts.kiev.ua/handle/123456789/119189 |
| work_keys_str_mv | AT baranoa structureofconvectiveflowsonsupergranularscalesinthesolarphotosphere |