Güneş Patlaması Kaynaklı Koronal Yağmurların Zürich Güneş Lekesi Sınıfları ile İlişkisi

Öz

Koronal yağmur, güneş koronasındaki termal kararsızlığın önemli bir göstergesidir. Bu yapılar, Güneşin dış atmosferindeki kütle ve enerji dengesini anlamak için bir anahtar görevindedir. Bu çalışmada, koronal yağmur oluşumunun ve yaşam süresinin, hem güneş patlaması enerjisine (C-, M- ve X-sınıfı) hem de güneş lekelerine ev sahipliği yapan aktif bölgelerin manyetik yapısını nasıl bağlı olduğu incelenmiştir. Sonuçlar, koronal yağmur oluşma olasılığının güneş patlaması enerjisiyle güçlü bir şekilde arttığını göstermektedir. C sınıfı güneş patlamaları daha az sıklıkla yağmur üretirken, M ve X sınıfı güneş patlamaları çok daha yüksek oluşum oranları göstermektedir. Bu eğilim neredeyse tüm güneş leke gruplarında gözlemlenmektedir. Bazı durumlarda, yüksek güneş patlaması enerjisine rağmen yağmur görülmemektedir ki bu da manyetik topolojinin önemli bir rol oynadığını düşündürmektedir. Ayrıca, yağmur süresinin patlama enerjisiyle birlikte arttığı da bulunmuştur. Tipik süreler, C sınıfı patlamalarda on dakikadan X sınıfı olaylarda 150-200 dakikaya kadar yükselmektedir. Bu, daha güçlü patlamaların, uzun süreli soğuma ve yoğunlaşma çevrimlerini sürdürebilen daha uzun ömürlü patlama sonrası koronal luplar ürettiğini göstermektedir. Leke sınıfları arasındaki farklılıklar, koronal lup geometrisinin ve manyetik karmaşıklığın koronal yağmur evrimini etkilediğini de göstermektedir. Genel olarak, sonuçlarımız koronal yağmurun hem patlama enerjisi hem de manyetik yapı tarafından kontrol edildiğini göstermektedir. Bu bulgular, koronal luplarda termal dengesizliği yönlendirmede kütle-enerji girdisi ve manyetik topolojinin birleşik rolünü vurgulamaktadır.

Anahtar Kelimeler

• Koronal yağmur
• Güneş Patlaması
• Güneş lekeleri

The Relationship Between Flare-Driven Coronal Rain and Zürich Sunspot Classes

Öz

Coronal rain is a significant indicator of thermal instability within the solar corona. These structures serve as a key to understanding the balance of mass and energy in the Sun's outer atmosphere. In this study, we investigated how the occurrence and duration of coronal rain depend on both the energy of solar flares (C-,M-, and X-class) and the magnetic structure of the active regions hosting the sunspots. The results indicate that the probability of coronal rain occurrence increases strongly with solar flare energy. While C-class flares produce rain less frequently, M- and X-class flares exhibit much higher formation rates. This trend is observed across almost all sunspot groups. In some instances, despite high flare energy, no rain is observed, suggesting that magnetic topology plays a significant role. Furthermore, it was found that the duration of the rain increases with flare energy. Typical durations range from ten minutes for C-class flares to 150–200 minutes for X-class events. This suggests that more powerful flares generate longer-lived post-flare coronal loops capable of sustaining prolonged cycles of cooling and condensation. Differences observed among sunspot classes also indicate that coronal loop geometry and magnetic complexity influence the occurrence of coronal rain. Overall, our results demonstrate that coronal rain is governed by both flare energy and magnetic structure. These findings underscore the combined role of mass-energy input and magnetic topology in driving thermal instability within coronal loops.

Anahtar Kelimeler

• Coronal Rain
• Solar Flare
• Sunspots

Kaynakça

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