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Modeling an X-ray flare on Proxima Centauri: Evidence of two flaring loop components and of two heating mechanisms at work

机译:在半人马座Proxima上模拟X射线耀斑:两个燃烧环组件和两个加热机制的证据

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摘要

We model in detail a flare observed on Proxima Centauri with the EPIC-PN on board XMM-Newton at high statistics and high time resolution and coverage. Time-dependent hydrodynamic loop modeling is used to describe the rise and peak of the light curve, and a large fraction of the decay, including its change of slope and a secondary maximum, over more than 2 h. The light curve, the emission measure and the temperature derived from the data allow us to constrain the loop morphology and the heating function and to show that this flare can be described with two components: a major one triggered by an intense heat pulse injected in a single flaring loop with half-length ≈1.0 × 1010 cm, the other one by less intense heat pulses released about 1/2 h after the first one in related loop systems, probably arcades, with the same half-length. The heat functions of the two loop systems appear very similar: an intense pulse located at the loop footpoints followed by a low gradual decay distributed in the coronal part of the loop. The latter result and the similarity to at least one solar event (the Bastille Day flare in 2000) indicate that this pattern may be common to solar and stellar flares.\ud\udBased on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member states and the USA (NASA).
机译:我们使用XMM-Newton上的EPIC-PN在Proxima Centauri上观测到的耀斑进行了详细建模,具有很高的统计量,较高的时间分辨率和覆盖范围。随时间变化的流体动力学回路建模用于描述光曲线的上升和峰值,以及超过2小时的大部分衰减,包括其斜率和次要最大值的变化。根据数据得出的光曲线,辐射测量值和温度使我们能够限制回路的形态和加热功能,并表明该耀斑可以由两个部分来描述:一个主要部分是由注入一个高强度热脉冲触发的。单个火炬环的长度为≈1.0×1010 cm,另一个火炬环是由强度较小的热脉冲在第一个火炬环之后约1/2小时释放的,而相关的火星系统(可能是拱廊)中的火星具有相同的半长度。两个回路系统的热功能看起来非常相似:位于回路脚点的强烈脉冲,然后在回路的冠状部分分布的梯度逐渐减小。后一项结果和与至少一个太阳事件(2000年的巴士底日耀斑)的相似性表明,这种模式可能是太阳耀斑和恒星耀斑的共同特征。\ ud \ ud基于通过XMM-Newton获得的观测结果,ESA的一项ESA科学任务由ESA成员国和美国(NASA)直接资助的工具和捐款。

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