Categorization of Coronal Mass Ejection-driven Sheath Regions: Characteristics of STEREO Events

• Published in: The Astrophysical journal Vol. 921; no. 1; pp. 57 - 69
• Main Authors: Salman, Tarik M., Lugaz, Noé, Winslow, Reka M., Farrugia, Charles J., Jian, Lan K., Galvin, Antoinette B.
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 01.11.2021; IOP Publishing
• Subjects: Astrophysics; Classification; Coronal mass ejection; Field strength; Interplanetary magnetic fields; Least squares method; Magnetic fields; Magnetic properties; Propagation; Sheaths; Solar coronal mass ejections; Solar cycle; Solar wind; Statistical analysis
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ac11f3

Abstract We present a comprehensive statistical analysis of 106 sheath regions driven by coronal mass ejections and measured near 1 au. Using data from the STEREO probes, this extended analysis focuses on two discrete categorizations. In the first categorization, we investigate how the generic features of sheaths change with their potential formation mechanisms (propagation sheaths and expansion sheaths), namely, their associations with magnetic ejectas (MEs), which are primarily propagating or expanding in the solar wind. We find propagation sheaths to be denser and driven by stronger MEs, whereas expansion sheaths are faster. Exploring the temporal profiles of these sheaths with a superposed epoch technique, we observe that most of the magnetic field and plasma signatures are more elevated in propagation sheaths relative to expansion sheaths. The second categorization is based on speed variations across sheaths. Employing linear least-squares regression, we categorize four distinct speed profiles of the sheath plasma. We find that the associated shock properties and solar cycle phase do not impact the occurrence of such variations. Our results also highlight that the properties of the driving MEs are a major source of variability in the sheath properties. Through logistic regression, we conclude that the magnetic field strength and the ME speed in the solar wind frame are likely drivers of these speed variations.