2026/02/23 by Zesen Huang, Marco Velli, Olga Panasenco +19 · 1 voice
Biochemistry, Genetics and Molecular Biology · Physics and Astronomy · #Geomagnetism and Paleomagnetism Studies #Ionosphere and magnetosphere dynamics #Solar and Space Plasma Dynamics
paper · doi:10.3847/2041-8213/ae43ec
openalex publication_date 2026/02/23 · openalex created_date 2026/02/24 · openalex updated_date 2026/06/22
Abstract The Sun’s surface vibrates in characteristic 5 minute oscillations, known as p -modes, generated by sound waves trapped within the convection zone. Although these oscillations have long been hypothesized to reach into the solar wind, direct in situ evidence has remained elusive, even during previous close encounters by Parker Solar Probe (PSP). Here, we present strong in situ evidence of 5 minute oscillations in the upper solar corona, based on observations from PSP’s three closest perihelia. In two events at 9.9 solar radii ( R ⊙ ), we identify statistically significant (∼6 σ ) 3.1–3.2 mHz peaks in the magnetic field power spectrum, each appearing as a large-amplitude, spherically polarized Alfvénic wave train lasting approximately 35 minutes. These results demonstrate that global solar oscillations can reach the solar wind.