Estudio observacional de la dinámica de puntos brillantes en una zona del sol en calma

ilustraciones, fotografías, graficas

Autores:: Berrios Saavedra, Yeimy Gerardine

Tipo de recurso:

Fecha de publicación:: 2021

Institución:: Universidad Nacional de Colombia

Repositorio:: Universidad Nacional de Colombia

Idioma:: spa

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network_acronym_str	UNACIONAL2
network_name_str	Universidad Nacional de Colombia
repository_id_str
dc.title.spa.fl_str_mv	Estudio observacional de la dinámica de puntos brillantes en una zona del sol en calma
dc.title.translated.eng.fl_str_mv	Observational study of dynamics bright spots in an area of the quiet sun
title	Estudio observacional de la dinámica de puntos brillantes en una zona del sol en calma
spellingShingle	Estudio observacional de la dinámica de puntos brillantes en una zona del sol en calma 520 - Astronomía y ciencias afines::523 - Cuerpos y fenómenos celestes específicos Sol Puntos magnéticos brillantes Fotosfera Campo magnético Técnicas de procesamiento de imágenes Sun Magnetic bright points Photosphere Magnetic field Image processing techniques Sol Radiación solar
title_short	Estudio observacional de la dinámica de puntos brillantes en una zona del sol en calma
title_full	Estudio observacional de la dinámica de puntos brillantes en una zona del sol en calma
title_fullStr	Estudio observacional de la dinámica de puntos brillantes en una zona del sol en calma
title_full_unstemmed	Estudio observacional de la dinámica de puntos brillantes en una zona del sol en calma
title_sort	Estudio observacional de la dinámica de puntos brillantes en una zona del sol en calma
dc.creator.fl_str_mv	Berrios Saavedra, Yeimy Gerardine
dc.contributor.advisor.none.fl_str_mv	Vargas Dominguez, Santiago Utz, Dominik
dc.contributor.author.none.fl_str_mv	Berrios Saavedra, Yeimy Gerardine
dc.contributor.researchgroup.spa.fl_str_mv	Group of Solar Astrophysics
dc.subject.ddc.spa.fl_str_mv	520 - Astronomía y ciencias afines::523 - Cuerpos y fenómenos celestes específicos
topic	520 - Astronomía y ciencias afines::523 - Cuerpos y fenómenos celestes específicos Sol Puntos magnéticos brillantes Fotosfera Campo magnético Técnicas de procesamiento de imágenes Sun Magnetic bright points Photosphere Magnetic field Image processing techniques Sol Radiación solar
dc.subject.proposal.spa.fl_str_mv	Sol Puntos magnéticos brillantes Fotosfera Campo magnético Técnicas de procesamiento de imágenes
dc.subject.proposal.eng.fl_str_mv	Sun Magnetic bright points Photosphere Magnetic field Image processing techniques
dc.subject.unesco.none.fl_str_mv	Sol Radiación solar
description	ilustraciones, fotografías, graficas
publishDate	2021
dc.date.accessioned.none.fl_str_mv	2021-06-08T16:21:05Z
dc.date.available.none.fl_str_mv	2021-06-08T16:21:05Z
dc.date.issued.none.fl_str_mv	2021
dc.type.spa.fl_str_mv	Trabajo de grado - Maestría
dc.type.driver.spa.fl_str_mv	info:eu-repo/semantics/masterThesis
dc.type.version.spa.fl_str_mv	info:eu-repo/semantics/acceptedVersion
dc.type.content.spa.fl_str_mv	DataPaper Dataset Model Software Text
dc.type.redcol.spa.fl_str_mv	http://purl.org/redcol/resource_type/TM
status_str	acceptedVersion
dc.identifier.uri.none.fl_str_mv	https://repositorio.unal.edu.co/handle/unal/79614
dc.identifier.instname.spa.fl_str_mv	Universidad Nacional de Colombia
dc.identifier.reponame.spa.fl_str_mv	Repositorio Institucional Universidad Nacional de Colombia
dc.identifier.repourl.spa.fl_str_mv	https://repositorio.unal.edu.co/
url	https://repositorio.unal.edu.co/handle/unal/79614 https://repositorio.unal.edu.co/
identifier_str_mv	Universidad Nacional de Colombia Repositorio Institucional Universidad Nacional de Colombia
dc.language.iso.spa.fl_str_mv	spa
language	spa
dc.relation.references.spa.fl_str_mv	Babcock, H. (1961). The topology of the sun’s magnetic field and the 22-year cycle.TheAstrophysical Journal, 133:572. Beck, C., Mikurda, K., Bellot Rubio, L., Schlichenmaier, R., and S ̈utterlin, P. (2007). Mag-netic properties of g-band bright points. In Modern solar facilities-advanced solar science,page 165. Berger, T. (1998). Measurements of solar magnetic element motion from high-resolutionfiltergrams.The Astrophysical Journal, 495:973. Berger, T. et al. (1996). On the dynamics of small-scale solar magnetic elements.TheAstrophysical Journal, 463:365. Blanco, J., Cabello, I., Vargas, S., Balmaceda, L., and Domingo, V. (2017). Observing timeproposal form 2017 for sst at the observatorio del roque de los muchachos la palma, spain. Chaplin, W. J. (2006).Music of the Sun. Choudhuri, A. R., Auffret, H., and Priest, E. R. (1993). Implications of rapid footpointmotions of photospheric flux tubes for coronal heating.Solar physics, 143(1):49–68. De Pontieu, B., Mart ́ınez-Sykora, J., and Chintzoglou, G. (2017). What causes the high appa-rent speeds in chromospheric and transition region spicules on the sun?The AstrophysicalJournal Letters, 849(1):L7. Del Moro, D., Berrilli, F., Duvall, T., and Kosovichev, A. (2004). Dynamics and structureof supergranulation.Solar Physics, 221(1):23–32. Denker, C., Kuckein, C., Verma, M., Manrique, S. J. G., Diercke, A., Enke, H., Klar, J.,Balthasar, H., Louis, R. E., and Dineva, E. (2018). High-cadence imaging and imagingspectroscopy at the gregor solar telescope—a collaborative research environment for high-resolution solar physics.The Astrophysical Journal Supplement Series, 236(1):5. Dikpati, M. and Gilman, P. A. (2008). Global solar dynamo models: Simulations and pre-dictions.Journal of Astrophysics and Astronomy, 29(1-2):29–39. Domingo, V., Ermolli, I., Fox, P., Fr ̈ohlich, C., Haberreiter, M., Krivova, N., Kopp, G.,Schmutz, W., Solanki, S., Spruit, H., et al. (2009). Solar surface magnetism and irradianceon time scales from days to the 11-year cycle.Space Science Reviews, 145(3-4):337–380. Dunn, R. B. and Zirker, J. B. (1973). The solar filigree.Solar Physics, 33(2):281–304. Gibson, E. G. (1973). The quiet sun. Hurlburt, N., Slater, G., Tarbell, T., Berger, T., and Katsukawa, Y. (2009). Hinode solaroptical telescope data analysis guide.Version, 3:58. Karttunen, H., Kr ̈oger, P., Oja, H., Poutanen, M., and Donner, K. J. (2016).Fundamentalastronomy. Springer. Kawaguchi, I. (1980). Morphological study of the solar granulation. Solar Physics, 65(2):207–220. Keller, C. (1992). Resolution of magnetic flux tubes on the sun. Nature, 359(6393):307. Kitchatinov, L. (2014). The solar dynamo: Inferences from observations and modeling.Geo-magnetism and Aeronomy, 54(7):867–876. Kosugi, T., Matsuzaki, K., Sakao, T., Shimizu, T., Sone, Y., Tachikawa, S., Hashimoto, T.,Minesugi, K., Ohnishi, A., Yamada, T., et al. (2007). The hinode (solar-b) mission: anoverview. InThe Hinode Mission, pages 5–19. Springer. Kuckein, C., Denker, C., Verma, M., Balthasar, H., Manrique, S. G., Louis, R., and Diercke,A. (2016). stools–a data reduction pipeline for the gregor fabry-p ́erot interferometer andthe high-resolution fast imager at the gregor solar telescope. Proceedings of the Interna-tional Astronomical Union, 12(S327):20–24. Limpert, E., Stahel, W. A., and Abbt, M. (2001). Log-normal distributions across thesciences: keys and clues: on the charms of statistics, and how mechanical models resemblinggambling machines offer a link to a handy way to characterize log-normal distributions,which can provide deeper insight into variability and probability—normal or log-normal:that is the question.BioScience, 51(5):341–352. Liu, Y., Xiang, Y., Erdelyi, R., Liu, Z., Li, D., Ning, Z., Bi, Y., Wu, N., and Lin, J. (2018).Studies of isolated and non-isolated photospheric bright points in an active region observedby the new vacuum solar telescope.The Astrophysical Journal, 856(1):17. Martin, S., Bilimoria, R., Tracadas, P. W., Rutten, R., and Schrijver, C. (1994). Solar surfacemagnetism.RJ Rutten and CJ. Mehltretter, J. (1974). Observations of photospheric faculae at the center of the solar disk.Solar Physics, 38(1):43–57. M ̈ostl, C., Hanslmeier, A., Sobotka, M., Puschmann, K., and Muthsam, H. (2006). Dynamicsof magnetic bright points in an active region. Solar Physics, 237(1):13–23. Muller, R., Roudier, T., Vigneau, J., and Auffret, H. (1994). The proper motion of networkbright points and the heating of the solar corona.Astronomy and Astrophysics, 283:232–240. Nisenson, P., Van Ballegooijen, A., De Wijn, A., and S ̈utterlin, P. (2003). Motions of isolatedg-band bright points in the solar photosphere.The Astrophysical Journal, 587(1):458. Petrie, G. (2012). Evolution of active and polar photospheric magnetic fields during the riseof cycle 24 compared to previous cycles.Solar Physics, 281(2):577–598. Petrie, G. J. (2015). Solar magnetism in the polar regions.Living Reviews in Solar Physics,12(1):5. S ́anchez, J., M ́arquez, I., Bonet, J., Cerde ̃na, I. D., and Muller, R. (2004). Bright points inthe internetwork quiet sun. The Astrophysical Journal Letters, 609(2):L91. Solanki, S. K., Inhester, B., and Sch ̈ussler, M. (2006). The solar magnetic field.Reports onProgress in Physics, 69(3):563. Steiner, O., Bruls, J., and Hauschildt, P. (2001). Why are g-band bright points bright? InAdvanced Solar Polarimetry–Theory, Observation, and Instrumentation, volume 236, page453. Stix, M. (2012). The sun: an introduction. Springer Science & Business Media. Sweet, P. (1969). Mechanisms of solar flares.Annual Review of Astronomy and Astrophysics,7(1):149–176. Tobias, S. (2002). The solar dynamo.Philosophical Transactions of the Royal Society ofLondon. Series A: Mathematical, Physical and Engineering Sciences, 360(1801):2741–2756. Tsuneta, S., Ichimoto, K., Katsukawa, Y., Nagata, S., Otsubo, M., Shimizu, T., Suematsu,Y., Nakagiri, M., Noguchi, M., Tarbell, T., et al. (2008). The solar optical telescope forthe hinode mission: an overview.Solar Physics, 249(2):167–196. Twidell, J. and Weir, T. (2006). Renewable energy resources. by taylor and francis.Newyork,USA. Utz, D. (2007). Dynamics of magnetic bright points in the solar photosphere. Master’sthesis, University of Graz. Utz, D., del Toro Iniesta, J., Rubio, L. B., Jurˇc ́ak, J., Pillet, V. M., Solanki, S., and Sch-midt, W. (2014). The formation and disintegration of magnetic bright points observed bysunrise/imax.The Astrophysical Journal, 796(2):79. Utz, D., Hanslmeier, A., M ̈ostl, C., Muller, R., Veronig, A., and Muthsam, H. (2009a). The size distribution of magnetic bright points derived from hinode/sot observations.Astronomy and Astrophysics, 498(1):289–293. Utz, D., Hanslmeier, A., Muller, R., Veronig, A., Ryb ́ak, J., and Muthsam, H. (2009b).Dynamics of isolated magnetic bright points derived from hinode/sot g-band observations.Astronomy and Astrophysics, 511:A39. Utz, D. t., Jurˇc ́ak, J., Hanslmeier, A., Muller, R., Veronig, A., and K ̈uhner, O. (2013).Magnetic field strength distribution of magnetic bright points inferred from filtergramsand spectro-polarimetric data.Astronomy & Astrophysics, 554:A65. Wiegelmann, T., Thalmann, J. K., and Solanki, S. K. (2014). The magnetic field in the solaratmosphere.The Astronomy and Astrophysics Review, 22(1):78. Wiehr, E., Bovelet, B., and Hirzberger, J. (2004). Brightness and size of small-scale solarmagnetic flux concentrations.Astronomy and Astrophysics, 422(3):L63–L66. W ̈oger, F., Von der L ̈uhe, O., and Reardon, K. (2008). Speckle interferometry with adaptiveoptics corrected solar data.Astronomy and Astrophysics, 488(1):375–381
dc.rights.coar.fl_str_mv	http://purl.org/coar/access_right/c_abf2
dc.rights.license.spa.fl_str_mv	Atribución-NoComercial-SinDerivadas 4.0 Internacional
dc.rights.uri.spa.fl_str_mv	http://creativecommons.org/licenses/by-nc-nd/4.0/
dc.rights.accessrights.spa.fl_str_mv	info:eu-repo/semantics/openAccess
rights_invalid_str_mv	Atribución-NoComercial-SinDerivadas 4.0 Internacional http://creativecommons.org/licenses/by-nc-nd/4.0/ http://purl.org/coar/access_right/c_abf2
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dc.format.extent.spa.fl_str_mv	1 recurso en linea (114 paginas)
dc.format.mimetype.spa.fl_str_mv	application/pdf
dc.publisher.spa.fl_str_mv	Universidad Nacional de Colombia
dc.publisher.program.spa.fl_str_mv	Bogotá - Ciencias - Maestría en Ciencias - Astronomía
dc.publisher.department.spa.fl_str_mv	Observatorio Astronómico Nacional
dc.publisher.faculty.spa.fl_str_mv	Facultad de Ciencias
dc.publisher.place.spa.fl_str_mv	Bogotá, Colombia
dc.publisher.branch.spa.fl_str_mv	Universidad Nacional de Colombia - Sede Bogotá
institution	Universidad Nacional de Colombia
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spelling	Atribución-NoComercial-SinDerivadas 4.0 Internacionalhttp://creativecommons.org/licenses/by-nc-nd/4.0/info:eu-repo/semantics/openAccesshttp://purl.org/coar/access_right/c_abf2Vargas Dominguez, Santiago84b9c649a144d9db1945760e44b42c6dUtz, Dominik5e68c63fd1dae300c8204828e0b4a5e6Berrios Saavedra, Yeimy Gerardinea8de4bd1370dfe97299c38b4148b33b7Group of Solar Astrophysics2021-06-08T16:21:05Z2021-06-08T16:21:05Z2021https://repositorio.unal.edu.co/handle/unal/79614Universidad Nacional de ColombiaRepositorio Institucional Universidad Nacional de Colombiahttps://repositorio.unal.edu.co/ilustraciones, fotografías, graficasLas observaciones en alta resolución de la fotosfera solar han revelado la existencia de estructuras compuestas de diminutos Puntos Magnéticos Brillantes o MBPs (por sus siglas en inglés). Tales estructuras a pequeña escala están asociadas con regiones de campo magnético fuerte del orden de kilogauss (kG) (Beck et al., 2007). Diversas investigaciones han encontrado que el diámetro promedio de un MBP está en el rango de 100 - 300 km, su velocidad horizontal promedio entre 0,2 - 5 kms−1 y su tiempo de vida de 2,5 a 10 minutos en promedio (Utz et al., 2009b). Es relevante estudiar estos elementos magnéticos y establecer su contribución al comportamiento de la atmósfera solar, y particularmente al bien conocido problema del calentamiento coronal. Aunque pequeños, los MBPs podrían contribuir significativamente a la energía requerida en la corona debido a que cubren toda la superficie del Sol y albergan intensos campos magnéticos. Teóricamente, el movimiento del punto de anclaje de un MBP genera un flujo de energía que asciende a la corona y puede contribuir a su calentamiento (Choud-huri et al., 1993). En este trabajo, el análisis de MBPs se hace a través del uso de series de tiempo de imágenes de la fotosfera solar adquiridas con telescopios solares de alta resolución, tanto en tierra como espaciales i.e., el instrumento SOT/Hinode (Telescopio Óptico Solar) y HiFI/GREGOR (generador de imágenes de alta resolución) en la banda G (4308 ̊A). Con el fin de detectar los MBPs, se hace uso de un algoritmo automático de segmentación e identificación, a partir del cual se rastrean estos elementos pequeños para medir su movimiento propio. Posteriormente, se lleva a cabo un análisis estadístico de cientos de MBPs por medio de histogramas de área y diámetro, así como analizando curvas de luz que evidencian su variación en intensidad. Adicional a esto, se mide la velocidad horizontal promedio de estas estructuras para caracterizarlas durante la evolución de la región solar bajo estudio. Los resultados establecen que las medidas de los parámetros dinámicos de los MBPs están influenciadas por el instrumento utilizado, ya que con el cambio de la resolución espacial y temporal se obtienen parámetros diferentes. Con una resolución de 0,108 arcseg/px se obtuvo para el área de los MBPs un valor medio de 37000·\|÷1,7 km2, para el diámetro promedio260· \| ÷1,5 km y una velocidad horizontal media de 1,1 - 2,3 kms−1(se encontraron dos poblaciones de MBPs en los resultados de velocidad). Por su parte, para una resolución de 0,0286 arcseg/px se encontraron dos poblaciones de MBPs cuyas áreas promedios fueron de 5700·\|÷1,6 km2 y 20000·\|÷1,6 km2 respectivamente, para el diámetro un valor medio de 80· \| ÷1,3 km para el primer grupo de MBPs y de 150· \| ÷1,5 km para el segundo y una velocidad promedio de 1,9 kms−1 y 7,5 kms−1 para cada una de las poblaciones.High-resolution observations of the solar photosphere reveal a large fine structure compo-sed of tiny Magnetic Bright Points (MBPs), which are small-scale features associated withstrong magnetic field regions of the order of kilogauss (kG) (Beck et al., 2007). Differentinvestigations have found that the average diameter of a MBP lays in a range of 100 - 300km, its horizontal average velocity between 0,2-5 kms−1and its lifetime of 2,5 to 10 minuteson average (Utz et al., 2009b).It is relevant to study these magnetic elements and establish their contribution to the beha-viour of the solar atmosphere, and ultimately to the well known coronal heating problem.Although being small, MBPs could significantly contribute to the energy budget in the coronaas they cover the entire surface of the Sun and harbour strong magnetic fields. Theoretically,the movement of the footpoint of an MBP generates a flow of energy that ascends to thecorona and can contribute to its heating (Choudhuri et al., 1993).In this work, the analysis of MBPs is done by means of time series of images of the solarphotosphere acquired with high resolution ground-based and space-borned solar telesco-pes, i.e. SOT/Hinode instrument (Solar Optical Telescope) and the HiFI/GREGOR (Hight-resolution Fast Imager) in the G-band (4308 ̊A).In order to detect MBPs, an automatic segmentation and identification algorithm is used,and these small elements are subsequently tracked to measure its proper motions. A statisti-cal analysis of hundreds of MBPs is carried out, as well as histograms of their area and size,and light curves displaying their variation in intensity. In addition, the average horizontalvelocity of these structures is measured to characterize them during the evolution of thesolar region under study. The results establish that the measurements of the dynamic parameters of the MBPs areinfluenced by the instrument used since with the change of the spatial and temporal reso-lution different values are obtained. With a resolution of 0,108 arcsec/px, was obtained forthe area of the MBPs an average value of 37000· \| ÷1,7 km2, for the mean diameter 260· \| ÷1,5 km and a mean horizontal velocity of 1,1 - 2,3 kms−1(two populations of MBPswere found in the velocity results).On the other hand, for a resolution of 0,0286 arcse/px, two populations of MBPs were foundwhose mean areas were 5700·\|÷1,6 and 20000·\|÷1,6 km2respectively, for the diameteran average value of 80·\|÷1,3 km for the first group of MBPs and 150·\|÷1,5 km for thesecond and an mean velocity of 1,9 kms−1and 7,5 kms−1for each of the populations.MaestríaMagister en Ciencias AstronomíaAstrofísica solar1 recurso en linea (114 paginas)application/pdfspaUniversidad Nacional de ColombiaBogotá - Ciencias - Maestría en Ciencias - AstronomíaObservatorio Astronómico NacionalFacultad de CienciasBogotá, ColombiaUniversidad Nacional de Colombia - Sede Bogotá520 - Astronomía y ciencias afines::523 - Cuerpos y fenómenos celestes específicosSolPuntos magnéticos brillantesFotosferaCampo magnéticoTécnicas de procesamiento de imágenesSunMagnetic bright pointsPhotosphereMagnetic fieldImage processing techniquesSolRadiación solarEstudio observacional de la dinámica de puntos brillantes en una zona del sol en calmaObservational study of dynamics bright spots in an area of the quiet sunTrabajo de grado - Maestríainfo:eu-repo/semantics/masterThesisinfo:eu-repo/semantics/acceptedVersionDataPaperDatasetModelSoftwareTexthttp://purl.org/redcol/resource_type/TMBabcock, H. (1961). The topology of the sun’s magnetic field and the 22-year cycle.TheAstrophysical Journal, 133:572.Beck, C., Mikurda, K., Bellot Rubio, L., Schlichenmaier, R., and S ̈utterlin, P. (2007). Mag-netic properties of g-band bright points. In Modern solar facilities-advanced solar science,page 165.Berger, T. (1998). Measurements of solar magnetic element motion from high-resolutionfiltergrams.The Astrophysical Journal, 495:973.Berger, T. et al. (1996). On the dynamics of small-scale solar magnetic elements.TheAstrophysical Journal, 463:365.Blanco, J., Cabello, I., Vargas, S., Balmaceda, L., and Domingo, V. (2017). Observing timeproposal form 2017 for sst at the observatorio del roque de los muchachos la palma, spain.Chaplin, W. J. (2006).Music of the Sun.Choudhuri, A. R., Auffret, H., and Priest, E. R. (1993). Implications of rapid footpointmotions of photospheric flux tubes for coronal heating.Solar physics, 143(1):49–68.De Pontieu, B., Mart ́ınez-Sykora, J., and Chintzoglou, G. (2017). What causes the high appa-rent speeds in chromospheric and transition region spicules on the sun?The AstrophysicalJournal Letters, 849(1):L7.Del Moro, D., Berrilli, F., Duvall, T., and Kosovichev, A. (2004). Dynamics and structureof supergranulation.Solar Physics, 221(1):23–32.Denker, C., Kuckein, C., Verma, M., Manrique, S. J. G., Diercke, A., Enke, H., Klar, J.,Balthasar, H., Louis, R. E., and Dineva, E. (2018). High-cadence imaging and imagingspectroscopy at the gregor solar telescope—a collaborative research environment for high-resolution solar physics.The Astrophysical Journal Supplement Series, 236(1):5.Dikpati, M. and Gilman, P. A. (2008). Global solar dynamo models: Simulations and pre-dictions.Journal of Astrophysics and Astronomy, 29(1-2):29–39.Domingo, V., Ermolli, I., Fox, P., Fr ̈ohlich, C., Haberreiter, M., Krivova, N., Kopp, G.,Schmutz, W., Solanki, S., Spruit, H., et al. (2009). Solar surface magnetism and irradianceon time scales from days to the 11-year cycle.Space Science Reviews, 145(3-4):337–380.Dunn, R. B. and Zirker, J. B. (1973). The solar filigree.Solar Physics, 33(2):281–304.Gibson, E. G. (1973). The quiet sun.Hurlburt, N., Slater, G., Tarbell, T., Berger, T., and Katsukawa, Y. (2009). Hinode solaroptical telescope data analysis guide.Version, 3:58.Karttunen, H., Kr ̈oger, P., Oja, H., Poutanen, M., and Donner, K. J. (2016).Fundamentalastronomy. Springer.Kawaguchi, I. (1980). Morphological study of the solar granulation. Solar Physics, 65(2):207–220.Keller, C. (1992). Resolution of magnetic flux tubes on the sun. Nature, 359(6393):307.Kitchatinov, L. (2014). The solar dynamo: Inferences from observations and modeling.Geo-magnetism and Aeronomy, 54(7):867–876.Kosugi, T., Matsuzaki, K., Sakao, T., Shimizu, T., Sone, Y., Tachikawa, S., Hashimoto, T.,Minesugi, K., Ohnishi, A., Yamada, T., et al. (2007). The hinode (solar-b) mission: anoverview. InThe Hinode Mission, pages 5–19. Springer.Kuckein, C., Denker, C., Verma, M., Balthasar, H., Manrique, S. G., Louis, R., and Diercke,A. (2016). stools–a data reduction pipeline for the gregor fabry-p ́erot interferometer andthe high-resolution fast imager at the gregor solar telescope. Proceedings of the Interna-tional Astronomical Union, 12(S327):20–24.Limpert, E., Stahel, W. A., and Abbt, M. (2001). Log-normal distributions across thesciences: keys and clues: on the charms of statistics, and how mechanical models resemblinggambling machines offer a link to a handy way to characterize log-normal distributions,which can provide deeper insight into variability and probability—normal or log-normal:that is the question.BioScience, 51(5):341–352.Liu, Y., Xiang, Y., Erdelyi, R., Liu, Z., Li, D., Ning, Z., Bi, Y., Wu, N., and Lin, J. 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