2021/04/15 by K. Sasikumar Raja, Prasad Subramanian, Madhusudan Ingale +3
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysics #Atomic physics #Classical mechanics #Computational physics #Geophysics and Gravity Measurements #Kinetic energy #Meteorology #Modulation (music) #Nuclear physics #Physics #Plasma #Proton #Solar and Space Plasma Dynamics #Solar wind #Stellar, planetary, and galactic studies #Turbulence #astro-ph.SR #physics.plasm-ph #physics.space-ph
paper · pdf · doi:10.3847/1538-4357/abfcd1
18 Pages, 4 Figures, 1 Table - accepted for publication in the Astrophysical Journal
arxiv created 2021/04/15 · openalex created_date 2021/04/26 · openalex publication_date 2021/06/01 · arxiv updated 2021/06/30 · openalex updated_date 2026/08/05
Abstract Various remote sensing observations have been used so far to probe the turbulent properties of the solar wind. Using the recently reported density modulation indices that are derived using angular broadening observations of Crab Nebula during 1952–2013, we measured the solar wind proton heating using the kinetic Alfvén wave dispersion equation. The estimated heating rates vary from ≈1.58 × 10 −14 to 1.01 × 10 −8 erg cm −3 s −1 in the heliocentric distance range of 5–45 R ⊙ . Further, we found that heating rates vary with the solar cycle in correlation with density modulation indices. The models derived using in situ measurements (for example, electron/proton density, temperature, and magnetic field) that the recently launched Parker Solar Probe observations (planned closest perihelia 9.86 R ⊙ from the center of the Sun) are useful in the estimation of the turbulent heating rate precisely. Further, we compared our heating rate estimates with the one derived using previously reported remote sensing and in situ observations.