Survey of Compressions Observed in the Heliosheath with the Spacecraft Voyager  

作　　者：Danie Benjamín Berdichevsky Danie Benjamín Berdichevsky(IFIR/CONICET-UNR, Esmeralda y 27 de Febrero, Rosario, Santa Fe, RA;TRIDENT-BERDICHEVSKY, DANIEL B. Partnership, Greenbelt, MD, USA)

机构地区：[1]IFIR/CONICET-UNR, Esmeralda y 27 de Febrero, Rosario, Santa Fe, RA [2]TRIDENT-BERDICHEVSKY, DANIEL B. Partnership, Greenbelt, MD, USA

出　　处：《Advances in Aerospace Science and Technology》2021年第1期43-66,共24页航空科学与技术（英文）

摘　　要：Examples of changes in the magnitude of the <b><span style="font-family:Verdana;">B</span></b><span style="font-family:Verdana;"><span style="font-family:Verdana;"><b><span style="font-family:Verdana;">-</span></b></span></span><span><span><span style="font-family:;" "=""><span style="font-family:Verdana;">field after the heliosphere termination shock (TS) with both Voyager spacecraft (SC) are presented. The work focuses on similarities and differences in the observations at their </span><i><span style="font-family:Verdana;">in-situ</span></i><span style="font-family:Verdana;"> measurements along divergent paths. The presented results were collected where the accuracy of the magnetometer is the highest. These locations are those wherein, four to seven times during the year, the SC performs about 330 minutes of slow rotations identified in the SC language as MAGROLs. They are next reviewed, with the understanding that after the TS, at MAGROLs, the solar wind (SW) flows appear to be mostly sub-magnetosonic and compressional in this region, region named helio-sheath (HS). This is a preliminary survey that uses </span><span style="font-family:Verdana;">48 sec</span> <b><span style="font-family:Verdana;">B</span></b><span style="font-family:Verdana;">-field averages. The time-intervals in this work fill gaps in the currently available studies for longer time intervals. The present study reinforces the view that in the HS after the TS the SW is most likely strongly compressional. </span><span style="font-family:Verdana;">Further</span><span style="font-family:Verdana;"> we discuss the fact that observed fluctuation intensity-modes of the </span><b><span style="font-family:Verdana;">B</span></b><span style="font-family:Verdana;">-field in our time-ranges appear to be much more pronounced at the Voyager 2 path than at the Voyager 1 path.</span></span></span></span>Examples of changes in the magnitude of the <b><span style="font-family:Verdana;">B</span></b><span style="font-family:Verdana;"><span style="font-family:Verdana;"><b><span style="font-family:Verdana;">-</span></b></span></span><span><span><span style="font-family:;" "=""><span style="font-family:Verdana;">field after the heliosphere termination shock (TS) with both Voyager spacecraft (SC) are presented. The work focuses on similarities and differences in the observations at their </span><i><span style="font-family:Verdana;">in-situ</span></i><span style="font-family:Verdana;"> measurements along divergent paths. The presented results were collected where the accuracy of the magnetometer is the highest. These locations are those wherein, four to seven times during the year, the SC performs about 330 minutes of slow rotations identified in the SC language as MAGROLs. They are next reviewed, with the understanding that after the TS, at MAGROLs, the solar wind (SW) flows appear to be mostly sub-magnetosonic and compressional in this region, region named helio-sheath (HS). This is a preliminary survey that uses </span><span style="font-family:Verdana;">48 sec</span> <b><span style="font-family:Verdana;">B</span></b><span style="font-family:Verdana;">-field averages. The time-intervals in this work fill gaps in the currently available studies for longer time intervals. The present study reinforces the view that in the HS after the TS the SW is most likely strongly compressional. </span><span style="font-family:Verdana;">Further</span><span style="font-family:Verdana;"> we discuss the fact that observed fluctuation intensity-modes of the </span><b><span style="font-family:Verdana;">B</span></b><span style="font-family:Verdana;">-field in our time-ranges appear to be much more pronounced at the Voyager 2 path than at the Voyager 1 path.</span></span></span></span>

关 键 词：Magnetic Field Measurement Techniques Solar Heliosphere’s Heliosheath MHD 

分 类 号：O17[理学—数学]