Origin of Anomalous Cosmic Rays and the Acceleration Mechanism

异常宇宙线的起源及加速机制

• 批准号: 05640353
• 负责人: HASEBE Nobuyuki
• 金额: $ 1.34万
• 依托单位: Ehime University
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for General Scientific Research (C)
• 财政年份: 1993
• 资助国家: 日本
• 起止时间: 1993 至 1994
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/en/grant/KAKENHI-PROJECT-05640353/
• 关键词: Cosmic Ray; Anomalous Cosmic Rays; Elemental Abundance; Solar Wind Termination shock; Solar Modulation; Particle Acceleration; Cosmic Rays; Anomalous Component; Intersttelar Matter; Abundances; Solar Wind; Solar Modulation; Particle Accelerati

We have measured cosmic ray particles during the period September 1992 through August 1994 using the particle telescopes MI-1/2 and HI onboard the GEOTAIL satellite orbiting at 1 AU.We have examined the quiet-time particles from He to Fe with the energies of 3-250 MeV/n. Remaekable enhancement of anomalous O,N and Ne in the energy spectra below 50 MeV/n was observed in the late 1992, just after the solar maximum. The anomalous Cis also evident though the C enhancement is small compared with them. The correlation between the anomalous cosmic ray data and the neutron monitor data is relatively good in the last two solar cycles but in the years 1992-1994 there is a large difference between the ACR and the neutron counting rate. The fluxes of O,N and Ne in this solar cycle have rapidly recovered to the level in the previous solar minimum although the origin of this rapid recovery of the ACR fluxes is presently unknown.Strong presence of anomalous cosmic ray N,O and Ne was shown well before the approaching solar minimum at solar cycle 22. Anomalous Ar was firstly observed at 1 AU though it was observed by the VOYAGER in deep space. We found the first evidence for the emergence of a measurable sulfur component of anomalous cosmic rays below 30 MeV/n. Comparing the fluxes of anomalous N,O and Ne with high first ionization potentials (FIPs) , the anomalous C and S fluxes, which have intermediate FIPs, are very small. These results could be qualitatively expected from the scenario for the origin of the anomalous cosmic rays proposed by Fisk et al. (1974) . It implies that they are significantly ionized in the very local interstellar medium.

我们用GEOTAIL卫星上的MI-1/2和HI粒子望远镜测量了1992年9月至1994年8月期间的宇宙线粒子。我们研究了从He到Fe的能量为3-250 MeV/n的静止期粒子。在太阳极大值之后的1992年底，观测到了低于50 MeV/n能谱中O、N和Ne的显著增强。异常顺式也很明显，尽管与它们相比，C增强较小。在过去的两个太阳周中，异常宇宙线数据与中子监测数据之间的相关性较好，但在1992-1994年，ACR与中子计数率之间存在较大的差异。在这个太阳周期中，O、N和Ne的通量已经迅速恢复到前一个太阳活动极小期的水平，尽管ACR通量的这种快速恢复的来源目前尚不清楚。在第22太阳周接近太阳活动极小值之前，显示出强烈的异常宇宙线N、O和Ne。虽然旅行者号在深空观测到了异常的Ar，但它是在1AU首次观测到的。我们首次发现了低于30 MeV/n的反常宇宙线的可测量硫组分的出现，与具有高第一电离势(FIPs)的反常N、O和Ne的通量相比，具有中间FIPs的反常C和S通量很小。这些结果可以从Fisk等人提出的反常宇宙线起源的场景中定性地预料到。(1974)。这意味着它们在非常局部的星际介质中被显著电离。

项目成果

N.Hasebe et al.: "Anomalous Composition and Energy Spectra of Cosmic Rays" Proc.8th Int.Symp.on Solar Terrestrial.Phys.Part-1. 42-42 (1994)

N.Hasebe 等人：“宇宙射线的异常成分和能量光谱”Proc.8th Int.Symp.on Solar Terrescial.Phys.Part-1。

N.Hasebe et al.: "The GEOTAIL Energetic Particle Telescopes" Proc.23rd ICRC (Calgary). 2. 552-555 (1993)

N.Hasebe 等人：“GEOTAIL 高能粒子望远镜”Proc.23rd ICRC（卡尔加里）。

N.Hasebe et al.: "The GEOTAIL Energetic Particle Telescopes" Proc.23th Int.Cosmic Ray Conf.,Calgary. 2. 552-555 (1993)

N.Hasebe 等人：“GEOTAIL 高能粒子望远镜”Proc.23th Int.Cosmic Ray Conf.，卡尔加里。

B.Wilken et al.: "Search for solar neutron decay electrons by GEOTAIL LD sensor" Geophys.Res.Letter. (1994)

B.Wilken 等人：“通过 GEOTAIL LD 传感器搜索太阳中子衰变电子”Geophys.Res.Letter。

T.Doke et al.: "The Energetic Particle Spectrometer HEP On board the GEOTAIL Spacecraft" J.Geomag.and Geoelectr.46. 713-733 (1994)

T.Doke 等人：“GEOTAIL 航天器上的高能粒子光谱仪 HEP”J.Geomag.and Geoelectr.46。