Novel scaling laws to derive spatially resolved flare and CME parameters from sun-as-a-star observables

IF 5.4 2区 物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS Astronomy & Astrophysics Pub Date : 2024-11-06 DOI:10.1051/0004-6361/202451072
Atul Mohan, Natchimuthuk Gopalswamy, Hemapriya Raju, Sachiko Akiyama
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Abstract

Coronal mass ejections (CMEs) are often associated with X-ray (SXR) flares powered by magnetic reconnection in the low corona, while the CME shocks in the upper corona and interplanetary (IP) space accelerate electrons often producing the type II radio bursts. The CME and the reconnection event are part of the same energy release process as highlighted by the correlation between reconnection flux (ϕrec) that quantifies the strength of the released magnetic free energy during the SXR flare, and the CME kinetic energy that drives the IP shocks leading to type II bursts. Unlike the Sun, these physical parameters cannot be directly inferred in stellar observations. Hence, scaling laws between unresolved sun-as-a-star observables, namely SXR luminosity (LX) and type II luminosity (LR), and the physical properties of the associated dynamical events are crucial. Such scaling laws also provide insights into the interconnections between the particle acceleration processes across low-corona to IP space during solar-stellar “flare-CME-type II” events. Using long-term solar data in the SXR to radio waveband, we derived a scaling law between two novel power metrics for the flare and CME-associated processes. The metrics of “flare power” ( ) and “CME power” ( ), where VCME is the CME speed, scale as . In addition, LX and ϕrec show power-law trends with PCME with indices of 1.12 ± 0.05 and 0.61 ± 0.05, respectively. These power laws help infer the spatially resolved physical parameters, VCME and ϕrec, from disk-averaged observables, LX and LR during solar-stellar flare-CME-type II events.
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从太阳即恒星观测数据推导空间分辨率耀斑和 CME 参数的新缩放定律
日冕物质抛射(CME)通常与由低日冕中的磁重联驱动的 X 射线(SXR)耀斑有关,而上日冕和行星际(IP)空间中的 CME 冲击会加速电子,通常会产生 II 型射电暴。CME和重联事件是同一能量释放过程的一部分,这一点从重联通量(ϕrec)与CME动能之间的相关性(CME动能可量化SXR耀斑期间释放的磁自由能的强度,而CME动能可驱动行星际冲击,从而产生II型射电暴)可以看出。与太阳不同,恒星观测无法直接推断出这些物理参数。因此,未解决的太阳-恒星观测值(即 SXR 光度(LX)和 II 型光度(LR))与相关动力学事件的物理特性之间的比例关系至关重要。这种缩放规律还有助于深入了解太阳-恒星 "耀斑-CME II 型 "事件期间从低日冕到 IP 空间的粒子加速过程之间的相互联系。利用从 SXR 到射电波段的长期太阳数据,我们得出了耀斑和 CME 相关过程的两个新功率指标之间的比例定律。耀斑功率"( )和 "CME 功率"( ),其中 VCME 是 CME 速度,它们的比例为 。此外,LX 和 ϕrec 与 PCME 呈幂律趋势,指数分别为 1.12 ± 0.05 和 0.61 ± 0.05。这些幂律有助于从太阳-恒星耀斑-CME-II 型事件中的磁盘平均观测值 LX 和 LR 推断空间分辨物理参数 VCME 和 ϕrec。
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来源期刊
Astronomy & Astrophysics
Astronomy & Astrophysics 地学天文-天文与天体物理
CiteScore
10.20
自引率
27.70%
发文量
2105
审稿时长
1-2 weeks
期刊介绍: Astronomy & Astrophysics is an international Journal that publishes papers on all aspects of astronomy and astrophysics (theoretical, observational, and instrumental) independently of the techniques used to obtain the results.
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