[P-PS04] [EJ] アルマによる惑星科学の新展開

[PPS04-P14] アルマによるプラズモイド放出現象の観測

*下条 圭美¹、ハドソン ヒュー^2,3、スティーブン ホワイト⁴、ティム バスティアン⁵、岩井 一正⁶ (1.国立天文台、2.グラスゴー大学、3.カルフォルニア大学バークレー校、4.米空軍研究所、5.米国立電波天文台、6.情報通信研究機構)

キーワード：アルマ、太陽、プラズモイド

Eruptive phenomena such as plasmoid ejections or jets are an important feature of solar activity with the potential for improving our understanding of the dynamics of the solar atmosphere. Such ejections are often thought to be signatures of the outflows expected in regions of fast magnetic reconnection. The EUV line of Helium, formed at around 10^5 K, is found to be a reliable tracer of such phenomena, but the determination of physical parameters from such observations is not straightforward. We have observed a plasmoid ejection from an X-ray bright point simultaneously at millimeter wavelengths with ALMA, at EUV wavelengths with AIA, in soft X-rays with Hinode/XRT. This paper reports the physical parameters of the plasmoid obtained by combining the radio, EUV and X-ray data. As a result, we conclude that the plasmoid can consist either of (approximately) isothermal ~10^5 K plasma, or else a ~10^4 K core with a hot envelope. In both the cases, the 100 GHz emission detected by ALMA may be optically thin, confirming that the ALMA images show not only the tau=1 layer at 100 GHz located in chromosphere but also optically thin plasma located in transition region or corona. The analysis demonstrates the value of the additional temperature and density constraints that ALMA provides, and future science observations with ALMA will be able to match the spatial resolution of space-borne and other high-resolution telescopes.