Power spectra of convective motions in the solar photosphere
We reproduced the convective velocity field and the temperature structure of the solar photosphere using neutral iron line λ ≈ 639.3 nm profiles from the observations with high spatial resolution taken around the centre of the solar disc in the non-perturbed region. We obtained power spectra of vert...
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| Veröffentlicht in: | Advances in Astronomy and Space Physics |
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| Datum: | 2013 |
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| Format: | Artikel |
| Sprache: | Englisch |
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Головна астрономічна обсерваторія НАН України
2013
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| Online Zugang: | https://nasplib.isofts.kiev.ua/handle/123456789/119618 |
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| Назва журналу: | Digital Library of Periodicals of National Academy of Sciences of Ukraine |
| Zitieren: | Power spectra of convective motions in the solar photosphere / O.A. Baran // Advances in Astronomy and Space Physics. — 2013. — Т. 3., вип. 2. — С. 89-93. — Бібліогр.: 17 назв. — англ. |
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Digital Library of Periodicals of National Academy of Sciences of Ukraine| _version_ | 1862582820687314944 |
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| author | Baran, O.A. |
| author_facet | Baran, O.A. |
| citation_txt | Power spectra of convective motions in the solar photosphere / O.A. Baran // Advances in Astronomy and Space Physics. — 2013. — Т. 3., вип. 2. — С. 89-93. — Бібліогр.: 17 назв. — англ. |
| collection | DSpace DC |
| container_title | Advances in Astronomy and Space Physics |
| description | We reproduced the convective velocity field and the temperature structure of the solar photosphere using neutral iron line λ ≈ 639.3 nm profiles from the observations with high spatial resolution taken around the centre of the solar disc in the non-perturbed region. We obtained power spectra of vertical velocity and temperature variations at different photospheric levels in order to separate and study convective motions on different spatial scales. In the lower photosphere the main power is localized on the granular scales with a peak at scales of about 1-1.5 Mm (for the velocity variations) and 1.5 2 Mm (for the temperature variations) and it decreases with height. In the higher layers of the solar photosphere the peaks of the spectra of long-lived structures (T > 20 min) are slightly shifted to the larger scales (≈ 3 Mm at the height h = 400 km), but still present granulation. So, a separate regime of mesogranulaton at scales 5-10 Mm distinct from granulation by a power gap has not been found. Mesostructures appear as a part of a broad distribution of granular scales without further distinction from granulation.
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| first_indexed | 2025-11-26T23:38:13Z |
| format | Article |
| fulltext | |
| id | nasplib_isofts_kiev_ua-123456789-119618 |
| institution | Digital Library of Periodicals of National Academy of Sciences of Ukraine |
| issn | 2227-1481 |
| language | English |
| last_indexed | 2025-11-26T23:38:13Z |
| publishDate | 2013 |
| publisher | Головна астрономічна обсерваторія НАН України |
| record_format | dspace |
| spelling | Baran, O.A. 2017-06-07T18:14:21Z 2017-06-07T18:14:21Z 2013 Power spectra of convective motions in the solar photosphere / O.A. Baran // Advances in Astronomy and Space Physics. — 2013. — Т. 3., вип. 2. — С. 89-93. — Бібліогр.: 17 назв. — англ. 2227-1481 https://nasplib.isofts.kiev.ua/handle/123456789/119618 We reproduced the convective velocity field and the temperature structure of the solar photosphere using neutral iron line λ ≈ 639.3 nm profiles from the observations with high spatial resolution taken around the centre of the solar disc in the non-perturbed region. We obtained power spectra of vertical velocity and temperature variations at different photospheric levels in order to separate and study convective motions on different spatial scales. In the lower photosphere the main power is localized on the granular scales with a peak at scales of about 1-1.5 Mm (for the velocity variations) and 1.5 2 Mm (for the temperature variations) and it decreases with height. In the higher layers of the solar photosphere the peaks of the spectra of long-lived structures (T > 20 min) are slightly shifted to the larger scales (≈ 3 Mm at the height h = 400 km), but still present granulation. So, a separate regime of mesogranulaton at scales 5-10 Mm distinct from granulation by a power gap has not been found. Mesostructures appear as a part of a broad distribution of granular scales without further distinction from granulation. The authors are grateful to Dr. N. G. Shchukina for kindly proving the results of observations and to Dr. R. I. Kostyk for data reduction. en Головна астрономічна обсерваторія НАН України Advances in Astronomy and Space Physics Power spectra of convective motions in the solar photosphere Article published earlier |
| spellingShingle | Power spectra of convective motions in the solar photosphere Baran, O.A. |
| title | Power spectra of convective motions in the solar photosphere |
| title_full | Power spectra of convective motions in the solar photosphere |
| title_fullStr | Power spectra of convective motions in the solar photosphere |
| title_full_unstemmed | Power spectra of convective motions in the solar photosphere |
| title_short | Power spectra of convective motions in the solar photosphere |
| title_sort | power spectra of convective motions in the solar photosphere |
| url | https://nasplib.isofts.kiev.ua/handle/123456789/119618 |
| work_keys_str_mv | AT baranoa powerspectraofconvectivemotionsinthesolarphotosphere |