The Opposite Behaviors of Proton and Electron Temperatures in Relation to Solar Wind Magnetic Energy: Parker Solar Probe Observations

• Published in: The Astrophysical journal 2024-05, Vol.966 (1), p.2
• Main Authors: Zhao, G. Q., Feng, H. Q., Wu, D. J., Xiang, L., Yang, H. F., Liu, Q., Ren, D. Y.
• Format: Article
• Language: English
• Subjects: Correlation coefficient; Correlation coefficients; Electron energy; Electron temperatures; Energy; Heating; Interplanetary turbulence; Magnetic fields; Mathematical analysis; Physics; Plasma physics; Protons; Solar coronal heating; Solar energy; Solar magnetic field; Solar probes; Solar wind; Solar wind particles; Solar wind properties; Solar wind velocity; Space plasmas; Turbulence; Wind speed; Wind velocities
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ad3636

Solar wind heating is an outstanding issue that has been discussed for decades. Research on the connection between solar wind particle temperatures and turbulence may provide insight into this issue. Based on Parker Solar Probe observations, this paper investigates the properties of solar wind proton and electron temperatures in relation to turbulent magnetic energy, via the calculation of correlation coefficients (CCs) between particle temperatures and magnetic energy. The calculations are regulated by the spatial scale, plasma beta ( β ), and the angle between the solar wind velocity and background magnetic field, where the plasma beta is the ratio of plasma thermal to magnetic pressure. Results show that the correlation between proton temperature and magnetic energy is positive and can be strong with a CC exceeding 0.8. The strong correlation preferentially occurs at ion scales, with the wind velocity and background magnetic field quasi-perpendicular and over a wide beta range ( β < 3.0). On the other hand, the correlation between electron temperature and magnetic energy is commonly negative, often with an intermediate or negligible CC, accordingly. The CC with an amplitude up to 0.8 can arise at larger scales with the wind velocity and background magnetic field quasi-(anti)parallel and in the low-beta case ( β < 0.6). The implication of these findings on the physics of turbulent heating in the solar wind is discussed.