Solar-Terrestrial PhysicsSolar-Terrestrial PhysicsСолнечно-земная физика / Solnechno-Zemnaya Fizika / Solar-Terrestrial Physics2712-9640475610.12737/7487ОбзорыReviews ОбзорыWaves and oscillations in sunspot atmosphere: a reviewВолны и колебания в атмосфере солнечных пятен: обзорСычРоберт АндреевичSychRobert Andreevichsych@iszf.irk.ru
кандидат физико-математических наук;
candidate of physical and mathematical sciences;
Институт солнечно-земной физики СО РАНИркутскРоссияInstitute of Solar Terrestrial Physics SB RASIrkutskRussian Federation170620151706201512321https://naukaru.ru/en/nauka/article/4756/view
Сделан обзор проведенных в последнее время экспериментальных и теоретических исследований источников колебаний и волн в атмосфере солнечных пятен. Представлены результаты наблюдений на наземных и космических инструментах. Показана важная роль механизма частотного обрезания в формировании пространственного распределения узкополосных источников колебаний в атмосфере пятен. Обсуждаются альтернативные методы исследования структуры магнитного поля с использованием полученных гелиосейсмологических результатов. Исследована динамика распространяющихся волновых фронтов с использованием метода попиксельной вейвлет-фильтрации. Прове-ден анализ параметров колебаний с высотой. Рассмотрена возможность инициации вспышечного энерговыделения МГД-волнами, проникающими из области пятен в область вспышки вдоль магнитных волноводов. Уделено внимание процессам усиления волновой активности в пятнах перед началом вспышки. Дано краткое описание теоретической модели на основе подфотосферного низкочастотного резонатора.
The review focuses on recent experimental and theoretical studies of sources of oscillations in the sunspot atmosphere. The results of observations with ground-based and spaceborne instruments are presented. An important role of the cut-off frequency in forming the spatial distribution of narrowband sources of oscillations above sunspot is shown. The alternative techniques for studying the magnetic field structure by using helioseismological data are discussed. The dynamics of propagating wave fronts is studied by applying the pixelized wavelet filtering technique. The height analysis of oscillation parameters is performed. A possibility to initiate flare energy release by MHD waves propagating along magnetic waveguides from sunspots into the flare region is discussed. The attention is paid to processes of the increase in wave activity in sunspots before the flare energy release. A brief description of the theoretical model for oscillations based on the subphotospheric low-frequency resonator is provided.
1.ВВЕДЕНИЕИзучение магнитогидродинамических (МГД) волн и колебаний в солнечной атмосфере является одной из наиболее быстро развивающихся областей солнечной физики и лежит в основном русле использования данных солнечных инструментов. Волновые процессы привлекают наше внимание из-за их возможной роли в разогреве короны, подготовке условий для возникновения вспышек и корональных выбросов массы, ускорения солнечного ветра. Волны являются природными зондами, поскольку наблюдаемые свойства волн содержат информацию о среде распространения.Наблюдаемая периодичность излучения в активных областях определяется следующими факторами: глобальными подфотосферными турбулентными процессами, генерирующими широкополосные пульсации в виде звуковых волн, условиями среды распространения волн и параметрами частотных резонаторов (фотосферных, хромосферных), которые определяют частоту обрезания излучения. Существование этих факторов приводит к появлению в наблюдательных данных следующих периодов волн: a) высокочастотных в диапазоне от 2 до 4 мин (средний период около 3 мин), регистрируемых в солнечных пятнах и связанных с распространением медленных магнитоакустических волн; б) 5-минутных колебаний с максимумом мощности в нижних слоях атмосферы; в) длиннопериодных колебаний с периодами десятки-сотни минут [Goldvarg et al., 2005; Gelfreikh et al., 2006; Efremov et al., 2007]; г) ультрадлиннопериодных колебаний с периодами порядка нескольких дней, связанных с предполагаемыми крутильными колебаниями групп пятен [Гопасюк, 2004].Особое место в исследовании волновых процессов занимает анализ квазипериодических пульсаций (КПП) излучения над пятнами, впервые обнаруженных Beckers, Tallant [1969] и названных «вспышки в тени». Несмотря на то, что 3-минутные колебания в солнечных пятнах наблюдаются на протяжении нескольких десятилетий [Bogdan, Judge, 2006; Thomas, Weiss, 2008], мы все еще далеки от понимания многих вопросов, касающихся физики волновых процессов в пятнах. Например, до сих пор не ясна связь между 3-минутными волнами в тени и 5-минутными бегущими волнами в полутени. Исследователи приходят к взаимоисключающим выводам: одни говорят о существовании предпосылок того, что волны в полутени возникают из колебаний в тени пятна [Christopoulou et al., 2001], другие рассматривают их как независимые феномены [Christopoulou et al., 2000; Kobanov, Makarchik, 2004]. Недавние исследования [Tziotziou et al., 2006, 2007; Thomas, Weiss, 2008] показали, что вспышки в тени и бегущие волны в полутени - проявления общего волнового процесса с волновыми фронтами, распространяющимися через тень и полутень пятна.Общепринято, что магнитоакустические волны двигаются с локальной звуковой скоростью вдоль магнитных силовых линий из фотосферных слоев через хромосферу в корону. Однако до сих пор не-ясно, как высоко они распространяются в корону. Что определяет их свойства? Как изменяется частота обрезания волн в пятнах? Как пространственно распределены параметры осцилляций в зависимости от периода колебаний? Связаны ли они напрямую с распространяющимися долготными волнами, обычно наблюдаемыми в ультрафиолетовом диапазоне в корональных магнитных структурах типа EUV-вееров (fans) [De Moortel еt al., 2012]? Какова природа недавно открытой связи 3-минутных колебаний в пятнах и колебаний с подобной периодичностью во вспышках [Sych et al., 2009]? Понимание этих вопросов даст нам возможность диагностики плазмы на различных уровнях солнечной атмосферы, так как эти волны несут информацию о природе их возникновения и свойствах среды, в которой они распространяются.Обзор построен следующим образом: в разделе 2 рассматривается пространственно-частотная морфология источников колебаний и волн в пятнах, включая их локализацию, размеры, периоды колебаний, высотное структурирование, а также приводится описание механизма частотного обрезания, формирующего наблюдаемую переменность излучения. Обзор динамических характеристик волновых процессов в пятнах представлен в разделе 3. Приведена информация о структуре волновых фронтов и их изменениях со временем, исследована частотная трансформация колебаний в зависимости от мощности энергии волн. В разделе 4 рассматриваются вопросы инициализации солнечных вспышек, вызванных триггерами в виде магнитоакустических волн, пучков ускоренных частиц и ударных волн. Особое внимание уделено связи между периодической инициализацией пересоединения во вспышках и динамикой медленных магнитоакустических волн в пятнах. Краткий обзор теоретических моделей пятенных колебаний представлен в разделе 5, раздел 6 является заключением.
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