In Situ Signature of Cyclotron Resonant Heating in the Solar Wind.
In Situ Signature of Cyclotron Resonant Heating in the Solar Wind.
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DOI：
10.1103/physrevlett.129.165101
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发表时间：
2021-11
影响因子：
8.6
通讯作者：
T. Bowen;B. Chandran;J. Squire;S. Bale;D. Duan;Kristopher G. Klein;D. Larson;A. Mallet;
中科院分区：
文献类型：
--
作者：
T. Bowen;B. Chandran;J. Squire;S. Bale;D. Duan;Kristopher G. Klein;D. Larson;A. Mallet;
磁化湍流的耗散是描述日冕和风等天体物理环境中加热和能量传递的重要范例;然而，耗散和加热背后的特定无碰撞过程仍然相对不受测量的约束。遥感观测表明，在日冕中存在强烈的温度各向异性，这与回旋共振加热相一致。在太阳风中，原位磁场测量揭示了回旋波的存在，而测量的离子速度分布函数暗示了回旋共振的活跃存在。在这里，我们提出了帕克太阳探测器的观测，连接的存在下，离子回旋波直接的共振阻尼在所观察到的质子速度分布的签名，使用准线性理论的框架。我们发现，观测到的分布函数的准线性演化应该吸收观测到的回旋波人口与加热率为10^{-14} W/m^{3}，表明显着加热的太阳风。
The dissipation of magnetized turbulence is an important paradigm for describing heating and energy transfer in astrophysical environments such as the solar corona and wind; however, the specific collisionless processes behind dissipation and heating remain relatively unconstrained by measurements. Remote sensing observations have suggested the presence of strong temperature anisotropy in the solar corona consistent with cyclotron resonant heating. In the solar wind, in situ magnetic field measurements reveal the presence of cyclotron waves, while measured ion velocity distribution functions have hinted at the active presence of cyclotron resonance. Here, we present Parker Solar Probe observations that connect the presence of ion-cyclotron waves directly to signatures of resonant damping in observed proton-velocity distributions using the framework of quasilinear theory. We show that the quasilinear evolution of the observed distribution functions should absorb the observed cyclotron wave population with a heating rate of 10^{-14} W/m^{3}, indicating significant heating of the solar wind.