Relationship of great soft X-ray flares with other solar activity phenomena
Relationship of great soft X-ray flares with other solar activity phenomena
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DOI：
10.1007/s10509-011-0716-8
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发表时间：
2011-05
影响因子：
1.9
通讯作者：
V. Verma
中科院分区：
文献类型：
--
作者：
V. Verma
本文研究了GSXR耀斑与Hα耀斑、硬X射线（HXR）爆发、15.4GHz微波（MW）爆发、II/IV型射电爆发、日冕物质抛射（CMEs）、质子耀斑（>10 MeV）和地面增强（GLE）事件的关系，发现GSXR耀斑与H α耀斑、硬X射线爆发、15.4GHz微波爆发、II/IV型射电爆发、日冕物质抛射（CMEs）、质子耀斑（>10 MeV）和地面增强（GLE）事件的关系分别为85.7%、93%、97%、69%、60%、11.1%、79%、46%、23%的GSXR耀斑分别与观测到的Hα耀斑、HXR爆发、15.4GHz微波爆发、II型射电爆发、IV型射电爆发、GLE事件、日冕物质抛射、晕日冕物质抛射和质子耀斑（>10 MeV）有关。本文研究了GSXR耀斑与Hα爆发、HXR爆发和MW爆发的爆发时间延迟。结果表明，在大多数GSXR耀斑中，SXR爆发分别先于Hα爆发、HXR爆发和MW爆发开始，而在15-20%的GSXR耀斑中，SXR爆发分别先于Hα爆发、HXT爆发和MW爆发开始，表明存在两种类型的耀斑。SXR辐射与II型射电爆发、IV型射电爆发、GLE事件CME、晕CME和质子耀斑的起始时间间隔分别为1-15 min、1-20 min、21-30 min、21 -40 min、21 -40 min和1-4 h。根据大多数结果，我们认为，目前的调查支持太阳耀斑模型，表明耀斑触发首先在日冕，然后移动到色球/光球开始在其他波长的排放。本工作的结果与Kahler（1982）提出的“大耀斑综合征”基本一致。
We present study of relationship of GSXR flares with Hαflares, hard X-ray (HXR) bursts, microwave (MW) bursts at 15.4 GHz, type II/IV radio bursts, coronal mass ejections (CMEs), protons flares (>10 MeV) and ground level enhancement (GLE) events we find that about 85.7%, 93%, 97%, 69%, 60%, 11.1%, 79%, 46%, and 23%% GSXR flares are related/associated with observed Hαflares, HXR bursts, MW bursts at 15.4 GHz, type II radio bursts, type IV radio bursts, GLE events, CMEs, halo CMEs, and proton flares (>10 MeV), respectively. In the paper we have studied the onset time delay of GSXR flares with Hαflares, HXR, and MW bursts which shows the during majority GSXR flares SXR emissions start before the Hα, HXR and MW emissions, respectively while during 15–20% of GSXR flares the SXR emissions start after the onset of Hα, HXT and MW emissions, respectively indicating two types of solar flares. The, onset time interval between SXR emissions and type II radio bursts, type IV radio bursts, GLE events CMEs, halo CMEs, and protons flares are 1–15 min, 1–20 min, 21–30 min, 21–40 min, 21–40 min, and 1–4 hrs, respectively. Following the majority results we are of the view that the present investigations support solar flares models which suggest flare triggering first in the corona and then move to chromospheres/ photosphere to starts emissions in other wavelengths. The result of the present work is largely consistent with “big flare syndrome” proposed by Kahler (1982).