The Cosmic-Ray Electron and Positron Spectra Measured at 1 AU during Solar Minimum Activity
The Cosmic-Ray Electron and Positron Spectra Measured at 1 AU during Solar Minimum Activity
复制标题
DOI：
10.1086/308545
复制
发表时间：
2000-03
期刊：
影响因子：
--
通讯作者：
M. Boezio;P. Carlson;T. Francke;N. Weber;M. Suffert;M. Hof;W. Menn;M. Simon;S. A. Stephens;R. Bellotti;F. Cafagna;M. Castellano;M. Circella;C. Marzo;N. Finetti;P. Papini;S. Piccardi;P. Spillantini;M. Ricci;M. Casolino;M. P. Pascale;A. Morselli;P. Picozza;R. Sparvoli;G. Barbiellini;U. Bravar;P. Schiavon;A. Vacchi;N. Zampa;C. Grimani;J. Mitchell;J. Ormes;R. Streitmatter;R. Golden;S. Stochaj
中科院分区：
文献类型：
--
作者：
M. Boezio;P. Carlson;T. Francke;N. Weber;M. Suffert;M. Hof;W. Menn;M. Simon;S. A. Stephens;R. Bellotti;F. Cafagna;M. Castellano;M. Circella;C. Marzo;N. Finetti;P. Papini;S. Piccardi;P. Spillantini;M. Ricci;M. Casolino;M. P. Pascale;A. Morselli;P. Picozza;R. Sparvoli;G. Barbiellini;U. Bravar;P. Schiavon;A. Vacchi;N. Zampa;C. Grimani;J. Mitchell;J. Ormes;R. Streitmatter;R. Golden;S. Stochaj
本文报道了一种新的宇宙射线电子和正电子能谱测量方法。这些数据是由1994年8月8日至9日从加拿大林恩湖起飞的气球载实验CAPRICE 94收集的，其高度相当于平均剩余大气的3.9 g cm-2。该实验使用NMSU-WIZARD/CAPRICE 94球载磁谱仪，该磁谱仪配备有固体辐射器环成像切伦科夫（RICH）探测器、飞行时间系统、由漂移室和多丝正比室组成的跟踪装置以及硅钨量能器。这是RICH探测器首次与成像量热计一起用于气球实验。总共有3211个电子，在光谱仪上的刚性在0.3到30 GV之间，734个正电子，在0.3到10 GV之间，被识别出具有来自其他粒子的小背景。绝对能谱确定在能量区域的顶部的大气中的电子和0.46和43.6 GeV之间的0.46和14.6 GeV之间的正电子。我们发现，所观察到的正电子光谱和正电子分数是一致的一个纯粹的二次起源。理论预测的星际电子谱的比较表明，初级电子的注入谱比宇宙线的核子成分的注入谱陡峭。此外，所观察到的电子和正电子的光谱可以从星际光谱再现太阳调制的球对称模型，因此，调制是独立的粒子电荷的符号。
We report on a new measurement of the cosmic-ray electron and positron spectra. The data were collected by the balloon-borne experiment CAPRICE94, which was flown from Lynn Lake, Canada, on 1994 August 8-9 at an altitude corresponding to 3.9 g cm-2 of average residual atmosphere. The experiment used the NMSU-WIZARD/CAPRICE94 balloon-borne magnet spectrometer equipped with a solid radiator Ring Imaging Cerenkov (RICH) detector, a time-of-flight system, a tracking device consisting of drift chambers and multiwire proportional chambers, and a silicon-tungsten calorimeter. This was the first time a RICH detector was used together with an imaging calorimeter in a balloon-borne experiment. A total of 3211 electrons, with a rigidity at the spectrometer between 0.3 and 30 GV, and 734 positrons, between 0.3 and 10 GV, were identified with small backgrounds from other particles. The absolute energy spectra were determined in the energy region at the top of the atmosphere between 0.46 and 43.6 GeV for electrons and between 0.46 and 14.6 GeV for positrons. We found that the observed positron spectrum and the positron fraction are consistent with a pure secondary origin. A comparison of the theoretically predicted interstellar spectrum of electrons shows that the injection spectrum of primary electrons is steeper than that of the nucleonic components of cosmic rays. Furthermore, the observed electron and positron spectra can be reproduced from the interstellar spectra by a spherically symmetric model for solar modulation; hence, the modulation is independent of the sign of the particle charge.