{"id":{"repo_id":"njit","oai_identifier":"oai:digitalcommons.njit.edu:dissertations-1631"},"canonical_url":"https://search.dev.ndltd.org/etd/njit/oai:digitalcommons.njit.edu:dissertations-1631","repository":{"repo_id":"njit","name":"NJIT","base_url":"https://digitalcommons.njit.edu/do/oai/"},"display":{"title":"Application of adaptive optics to the spectroscopic investigation of small-scale solar structures","abstract":"We study bright points, umbral dots and the G-band using a two-dimensional spectrometer and an Adaptive Optics system, which allows us to record high-resolution dopplergrams and residual intensity images. We find evidence that bright points are smaller than 120 km in diameter. Bright points are situated exclusively in regions of enhanced G-band brightness and do not show a change in their shape or a displacement in their position of more than 120 km horizontally over a height range from 0 km to 320 km above photospheric level T = 1. We do not find velocity differences of more than 100 m/s and a size of 120 km at the locations of bright points compared to the surroundings. Bright points have a higher contrast in the G-band as well as in the atomic spectral lines. We suspect the existence of two contrast enhancement mechanisms for bright points one exclusively for the G-band, one independent of specific spectral lines. We perform calculations using the results of a three-dimensional magneto-hydrodynamical model as input for a radiative transfer calculation, but find little agreement with our observations. The core intensity of the G-band CH lines is significantly influenced by the atmospheric conditions in heights of 160 km and 320 km, but not heights of 40 km. The velocity investigation of a sunspot shows that umbral dots seem to consist of two different types. The first type is the bright part of an intensity pattern of 1000-2000 km size with a corresponding negatively correlated velocity pattern which is probably related to umbral oscillations. The second type consists of localized brightening of a size of not more than 300 km that are associated with down-flowing plasma. Furthermore, we find penumbral grains that have penetrated the umbra and appear as brightenings. We study the velocity signature of penumbral grains and find strong up-flows of solar plasma associated with the inner, bright parts of penumbral grains, where as the general correlation between intensity and velocity within the penumbra is weak.","abstract_html":"We study bright points, umbral dots and the G-band using a two-dimensional spectrometer and an Adaptive Optics system, which allows us to record high-resolution dopplergrams and residual intensity images. We find evidence that bright points are smaller than 120 km in diameter. Bright points are situated exclusively in regions of enhanced G-band brightness and do not show a change in their shape or a displacement in their position of more than 120 km horizontally over a height range from 0 km to 320 km above photospheric level T = 1. We do not find velocity differences of more than 100 m/s and a size of 120 km at the locations of bright points compared to the surroundings. Bright points have a higher contrast in the G-band as well as in the atomic spectral lines. We suspect the existence of two contrast enhancement mechanisms for bright points one exclusively for the G-band, one independent of specific spectral lines. We perform calculations using the results of a three-dimensional magneto-hydrodynamical model as input for a radiative transfer calculation, but find little agreement with our observations. The core intensity of the G-band CH lines is significantly influenced by the atmospheric conditions in heights of 160 km and 320 km, but not heights of 40 km. The velocity investigation of a sunspot shows that umbral dots seem to consist of two different types. The first type is the bright part of an intensity pattern of 1000-2000 km size with a corresponding negatively correlated velocity pattern which is probably related to umbral oscillations. The second type consists of localized brightening of a size of not more than 300 km that are associated with down-flowing plasma. Furthermore, we find penumbral grains that have penetrated the umbra and appear as brightenings. We study the velocity signature of penumbral grains and find strong up-flows of solar plasma associated with the inner, bright parts of penumbral grains, where as the general correlation between intensity and velocity within the penumbra is weak.","abstract_has_math":false,"creators":["Hartkorn, Klaus"],"institution":null,"degree_name":"Doctor of Philosophy in Applied Physics - (Ph.D.)","degree_level":null,"degree_discipline":"Federated Physics Department","degree_department":null,"school":null,"contributors":["Ken K. Chin","Carsten J. Denker","Dale E. Gary"],"advisors":[],"committee_chairs":[],"committee_members":[],"year":2003,"date_issued":"2003-05-31T07:00:00Z","date_published":"2003-05-31T07:00:00Z","updated_at":"2026-07-24T03:22:52Z","subjects":["sun","photosphere","bright points","g-band","sunspot","umbral dots","Other Physics"],"languages":[],"rights":[],"rights_urls":[],"identifier_entries":[]},"links":{"outbound_url":"https://digitalcommons.njit.edu/dissertations/576","outbound_label":"Repository record","outbound_source":"dc:identifier"},"metadata_groups":[{"id":"people","label":"People","entries":[{"key":"dc:contributor","label":"Contributor","values":["Ken K. Chin","Carsten J. Denker","Dale E. 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We find evidence that bright points are smaller than 120 km in diameter. Bright points are situated exclusively in regions of enhanced G-band brightness and do not show a change in their shape or a displacement in their position of more than 120 km horizontally over a height range from 0 km to 320 km above photospheric level T = 1. We do not find velocity differences of more than 100 m/s and a size of 120 km at the locations of bright points compared to the surroundings. Bright points have a higher contrast in the G-band as well as in the atomic spectral lines. We suspect the existence of two contrast enhancement mechanisms for bright points one exclusively for the G-band, one independent of specific spectral lines. We perform calculations using the results of a three-dimensional magneto-hydrodynamical model as input for a radiative transfer calculation, but find little agreement with our observations. The core intensity of the G-band CH lines is significantly influenced by the atmospheric conditions in heights of 160 km and 320 km, but not heights of 40 km. The velocity investigation of a sunspot shows that umbral dots seem to consist of two different types. The first type is the bright part of an intensity pattern of 1000-2000 km size with a corresponding negatively correlated velocity pattern which is probably related to umbral oscillations. The second type consists of localized brightening of a size of not more than 300 km that are associated with down-flowing plasma. Furthermore, we find penumbral grains that have penetrated the umbra and appear as brightenings. We study the velocity signature of penumbral grains and find strong up-flows of solar plasma associated with the inner, bright parts of penumbral grains, where as the general correlation between intensity and velocity within the penumbra is weak."]},{"key":"dc:title","label":"Title","values":["Application of adaptive optics to the spectroscopic investigation of small-scale solar structures"]}]}],"canonical_facts":{"dc:contributor":["Ken K. Chin","Carsten J. Denker","Dale E. Gary"],"dc:creator":["Hartkorn, Klaus"],"dc:description.abstract":["We study bright points, umbral dots and the G-band using a two-dimensional spectrometer and an Adaptive Optics system, which allows us to record high-resolution dopplergrams and residual intensity images. We find evidence that bright points are smaller than 120 km in diameter. Bright points are situated exclusively in regions of enhanced G-band brightness and do not show a change in their shape or a displacement in their position of more than 120 km horizontally over a height range from 0 km to 320 km above photospheric level T = 1. We do not find velocity differences of more than 100 m/s and a size of 120 km at the locations of bright points compared to the surroundings. Bright points have a higher contrast in the G-band as well as in the atomic spectral lines. We suspect the existence of two contrast enhancement mechanisms for bright points one exclusively for the G-band, one independent of specific spectral lines. We perform calculations using the results of a three-dimensional magneto-hydrodynamical model as input for a radiative transfer calculation, but find little agreement with our observations. The core intensity of the G-band CH lines is significantly influenced by the atmospheric conditions in heights of 160 km and 320 km, but not heights of 40 km. The velocity investigation of a sunspot shows that umbral dots seem to consist of two different types. The first type is the bright part of an intensity pattern of 1000-2000 km size with a corresponding negatively correlated velocity pattern which is probably related to umbral oscillations. The second type consists of localized brightening of a size of not more than 300 km that are associated with down-flowing plasma. Furthermore, we find penumbral grains that have penetrated the umbra and appear as brightenings. We study the velocity signature of penumbral grains and find strong up-flows of solar plasma associated with the inner, bright parts of penumbral grains, where as the general correlation between intensity and velocity within the penumbra is weak."],"dc:identifier":["https://digitalcommons.njit.edu/dissertations/576"],"dc:subject":["sun","photosphere","bright points","g-band","sunspot","umbral dots","Other Physics"],"dc:title":["Application of adaptive optics to the spectroscopic investigation of small-scale solar structures"],"dc:type":["Dissertation"],"thesis:degree_discipline":["Federated Physics Department"],"thesis:degree_name":["Doctor of Philosophy in Applied Physics - (Ph.D.)"]},"updated_at":"2026-07-24T03:22:52Z"}