Стійкий метод визначення напруженості магнітного поля у фотосфері Сонця

1Присяжний, АІ, 1Стоділка, МІ, 2Щукіна, НГ
1Астрономічна обсерваторія Львівського національного університету імені Івана Франка, Львів, Україна
2Головна астрономічна обсерваторія Національної академії наук України, Київ, Україна
Рубрика: Фізика Сонця
Мова: українська
Анотація: 

Запропоновано модифікацію класичного методу визначення напруженості магнітного поля за відстанню між положеннями піків синього і червоного крил V-профілю Стокса магніточутливої спектральної лінії. Для зменшення впливу шумів та більш коректного визначення відстані між положеннями піків спостережуваний профіль Стокса V було апроксимовано модифікованою вейвлет-функцією. Оптимальні значення коефіцієнтів апроксимаційної функції було визначено шляхом багатовимірної оптимізації. В рамках даного підходу напруженість магнітного поля можна знайти аналітично за відомими коефіцієнтами апроксимаційної функції. Для тестування методу було використано V-профілі Стокса спектральної лінії нейтрального заліза Fe Iλ 1564.8 нм. Профілі було синтезовано з використанням тривимірної фотосферної моделі магнітоконвекції Ремпеля. Показано результат застосування запропонованого методу до спостережуваних V-профілів Стокса. Даний метод менш чутливий до шумів та форми спостережуваного сигналу, що дозволяє отримувати більш надійні значення напруженості магнітного поля із спостережень у порівнянні з класичним методом визначення напруженості поля за розщепленням профілю Стокса V.

Ключові слова: діагностика, ефект Зеємана, магнітні поля, Сонце, фотосфера
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