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通过低于10 keV能量的中性原子观测研究日球层和本地星际介质

The Heliosphere and Local Interstellar Medium from Neutral Atom Observations at Energies Below 10 keV.

作者信息

Galli André, Baliukin Igor I, Bzowski Maciej, Izmodenov Vladislav V, Kornbleuth Marc, Kucharek Harald, Möbius Eberhard, Opher Merav, Reisenfeld Dan, Schwadron Nathan A, Swaczyna Paweł

机构信息

Physics Institute, University of Bern, Bern, Switzerland.

Space Research Institute of Russian Academy of Sciences, Moscow, Russia.

出版信息

Space Sci Rev. 2022;218(4):31. doi: 10.1007/s11214-022-00901-7. Epub 2022 May 23.

DOI:10.1007/s11214-022-00901-7
PMID:35673597
原文链接:https://pmc.ncbi.nlm.nih.gov/articles/PMC9165285/
Abstract

As the heliosphere moves through the surrounding interstellar medium, a fraction of the interstellar neutral helium, hydrogen, and heavier species crossing the heliopause make it to the inner heliosphere as neutral atoms with energies ranging from few eV to several hundred eV. In addition, energetic neutral hydrogen atoms originating from solar wind protons and from pick-up ions are created through charge-exchange with interstellar atoms. This review summarizes all observations of heliospheric energetic neutral atoms and interstellar neutrals at energies below 10 keV. Most of these data were acquired with the Interstellar Boundary Explorer launched in 2008. Among many other IBEX breakthroughs, it provided the first ever all-sky maps of energetic neutral atoms from the heliosphere and enabled the science community to measure in-situ interstellar neutral hydrogen, oxygen, and neon for the first time. These observations have revolutionized and keep challenging our understanding of the heliosphere shaped by the combined forces of the local interstellar flow, the local interstellar magnetic field, and the time-dependent solar wind.

摘要

当日光层在周围的星际介质中移动时，穿越日球层顶的一部分星际中性氦、氢及更重的元素会以能量范围从几电子伏特到几百电子伏特的中性原子形式进入内日光层。此外，源自太阳风质子和拾取离子的高能中性氢原子是通过与星际原子的电荷交换产生的。本综述总结了所有能量低于10keV的日光层高能中性原子和星际中性原子的观测结果。这些数据大多是由2008年发射的星际边界探测器获取的。在星际边界探测器取得的诸多突破中，它首次提供了来自日光层的高能中性原子全天图，并使科学界首次能够原位测量星际中性氢、氧和氖。这些观测结果彻底改变了并持续挑战着我们对由当地星际流、当地星际磁场和随时间变化的太阳风共同作用塑造的日光层的理解。

https://cdn.ncbi.nlm.nih.gov/pmc/blobs/2302/9165285/a4f425d9424e/11214_2022_901_Fig17_HTML.jpg
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https://cdn.ncbi.nlm.nih.gov/pmc/blobs/2302/9165285/a4f425d9424e/11214_2022_901_Fig17_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/2302/9165285/1cca949edb92/11214_2022_901_Fig1_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/2302/9165285/6dae5eca4a05/11214_2022_901_Fig2_HTML.jpg
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https://cdn.ncbi.nlm.nih.gov/pmc/blobs/2302/9165285/05d0fe5166dc/11214_2022_901_Fig5_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/2302/9165285/cb002f563622/11214_2022_901_Fig6_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/2302/9165285/01ba24c287ff/11214_2022_901_Fig7_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/2302/9165285/00ea4b9745ec/11214_2022_901_Fig8_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/2302/9165285/01613356f2a6/11214_2022_901_Fig9_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/2302/9165285/d3e5f0108640/11214_2022_901_Fig10_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/2302/9165285/07d3434f79b4/11214_2022_901_Fig11_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/2302/9165285/760783986a23/11214_2022_901_Fig12_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/2302/9165285/eef51e36745a/11214_2022_901_Fig13_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/2302/9165285/0b335e0718e0/11214_2022_901_Fig14_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/2302/9165285/1549b4f52af4/11214_2022_901_Fig15_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/2302/9165285/84b3f7554c7a/11214_2022_901_Fig16_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/2302/9165285/a4f425d9424e/11214_2022_901_Fig17_HTML.jpg

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