Устойчивый метод определения напряженности магнитного поля в фотосфере Солнца
Рубрика:
| 1Присяжный, АИ, 1Стодилка, МИ, 2Щукина, НГ 1Астрономическая обсерватория Львовского национального университета имени Ивана Франко, Львов, Украина 2Главная астрономическая обсерватория Национальной академии наук Украины, Киев, Украина |
| Kinemat. fiz. nebesnyh tel (Online) 2018, 34(6):3-21 |
| Start Page: Физика Солнца |
| Язык: украинский |
Аннотация: Предложена модификация классического метода определения напряженности магнитного поля по расстоянию между положениями пиков синего и красного крыльев V-профиля Стокса магниточувствительной спектральной линии. Для уменьшения влияния шумов и более корректного определения расстояния между положениями пиков наблюдаемый профиль Стокса V был аппроксимирован модифицированной вейвлет-функцией. Оптимальные значения коэффициентов аппроксимационной функции были определены путем многомерной оптимизации. В рамках данного подхода напряженность магнитного поля может быть найдена аналитически по известным коэффициентам аппроксимационной функции. Для тестирования метода были использованы V-профили Стокса спектральной линии нейтрального железа Fe I λ 1564.8 нм. Профили были синтезированы с использованием трехмерной фотосферной модели магнитоконвекции Ремпеля. Показан результат применения предложенного метода к наблюдаемым V-профилям Стокса. Данный метод менее чувствителен к шумам и форме наблюдаемого сигнала, что позволяет получать более надежные значения напряженности магнитного поля из наблюдений по сравнению с классическим методом определения напряженности поля по расщеплению профиля Стокса V. |
| Ключевые слова: диагностика, магнитные поля, Солнце, фотосфера, эффект Зеемана |
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