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首页> 外文期刊>The Astrophysical Journal. Letters >EVIDENCE OF MULTIPLE SLOW ACOUSTIC OSCILLATIONS IN THE STELLAR FLARING LOOPS OF PROXIMA CENTAURI
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EVIDENCE OF MULTIPLE SLOW ACOUSTIC OSCILLATIONS IN THE STELLAR FLARING LOOPS OF PROXIMA CENTAURI

机译：Proxima Centauri Stellar Flaring环中多个慢声振荡的证据

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摘要

We present the first observational evidence of multiple slow acoustic oscillations in the post-flaring loops of the corona of Proxima Centauri using XMM-Newton observations. We find the signature of periodic oscillations localized in the decay phase of the flare in its soft (0.3-10.0 keV) X-ray emissions. Using the standard wavelet tool, we find multiple periodicities of 1261 s and 687 s. These bursty oscillations persist for durations of 90 minutes and 50 minutes, respectively, for more than three cycles. The intensity oscillations with a period of 1261 s may be the signature of the fundamental mode of slow magnetoacoustic waves with a phase speed of 119 km s~(?1) in a loop of length 7.5 × 10~9 cm, which is initially heated, producing the flare peak temperature of 33 MK and later cooled down in the decay phase and maintained at an average temperature of 7.2 MK. The other period of 687 s may be associated with the first overtone of slow magnetoacoustic oscillations in the flaring loop. The fundamental mode oscillations show dissipation with a damping time of 47 minutes. The period ratio P_1/P_2 is found to be 1.83, indicating that such oscillations are most likely excited in longitudinal density stratified stellar loops. We estimate the density scale height of the stellar loop system as ～23 Mm, which is smaller than the hydrostatic scale height of the hot loop system, and implies the existence of non-equilibrium conditions.
机译：我们使用XMM-Newton观察展示了在Proxima Centauri Corona的辐射回路中的多个慢声振荡的第一个观察证据。我们发现其在柔软（0.3-10.0keV）X射线排放中爆离的衰变阶段定期振荡的签名。使用标准小波工具，我们发现多个周期为1261秒和687秒。这些爆发振荡持续为90分钟和50分钟的持续时间，分别超过三个周期。具有1261秒的时段的强度振荡可以是慢磁声波的基本模式的签名，其速度为119 km s〜（Δ1），其长度为7.5×10〜9cm，最初加热，产生33 mk的眩光峰值温度，后来在衰变相中冷却，并保持在7.2 mk的平均气温。 687 s的另一个时段可以与喇叭形环中的慢磁声振荡的第一个泛音相关联。基本模式振荡显示出耗散的阻尼时间为47分钟。期间比率P_1 / P_2被发现为1.83，表明这种振荡很可能在纵向密度分层恒星环中激发。我们估计恒星环系统的密度刻度高度为〜23mm，其小于热回路系统的静水压刻度高度，并意味着存在非平衡条件。

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