WHY IS THE GREAT SOLAR ACTIVE REGION 12192 FLARE-RICH BUT CME-POOR?

By Xudong Sun, Monica G. Bobra, J. Todd Hoeksema, Yang Liu, Yan Li, C. Shen, S. Couvidat, A. Norton, G. Fisher. 2015

164 citations recorded by the source corpus.

Solar active region (AR) 12192 of 2014 October hosts the largest sunspot group in 24 years. It is the most prolific flaring site of Cycle 24 so far, but surprisingly produced no coronal mass ejection (CME) from the core region during its disk passage. Here, we study the magnetic conditions that prevented eruption and the consequences that ensued. We find AR 12192 to be “big but mild”; its core region exhibits weaker non-potentiality, stronger overlying field, and smaller flare-related field changes compared to two other major flare-CME-productive ARs (11429 and 11158). These differences are present in the intensive-type indices (e.g., means) but generally not the extensive ones (e.g., totals). AR 12192's large amount of magnetic free energy does not translate into CME productivity. The unexpected behavior suggests that AR eruptiveness is limited by some relative measure of magnetic non-potentiality over the restriction of background field, and that confined flares may leave weaker photospheric and coronal imprints compared to their eruptive counterparts.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/6c2af096c465d55f180f777a5b8c4fecc70db51f

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In Astronomy and Astrophysics

1. M. Temmer
2. C. Schrijver
3. H. Hudson
4. S. Toriumi
5. L. Harra
6. K. Nagashima
7. A. Title
8. S. Solanki

Citations in the corpus

• MAGNETIC PROPERTIES OF SOLAR ACTIVE REGIONS THAT GOVERN LARGE SOLAR FLARES AND ERUPTIONS (2016, background): “0class flare (e.g., Kleint et al. 2015), and AR 12192, the largest sunspot group so far in the cycle, produced many (6 X- and 24 M-class) but CME-poor events (e.g., Sun et al. 2015; four Xand two M-class events are listed in Table 1).”
• Space weather: the solar perspective (2021, background): “Therefore, confined flares may produce strong X-ray emission but, presumably due to a strong bipolar overlying coronal magnetic field configuration, are not related to the opening of the large-scale magnetic field (e.g., Wang and Zhang 2007; Sun et al. 2015; Thalmann et al. 2015).”