Byline: Rasa nelson
One part of the Alabama system, Huntsville (UAH) is a graduate research assistant at the University of Alabama (UAH) Published a paper Astronomy and Physics Journal that is made on one First study To help understand why solar corona is so hot than the surface of the sun. To put forward light on this age-old mystery, Syed Ayaz, a Ph.D. The UAH Center for Space Plasma and Aeronomic Research (CSPAR) appoints a candidate, a statistical model, which is known as a kappa distribution to describe the velocity of particles in Space Plasma, while Kinetic Alphawen Waves (KAWS) By incorporating the interaction of superthorous particles with.
Kaws are charged particles and oscillations of magnetic fields as they run through solar plasma, which is caused by the movements in the photofare, the outer shell of the sun. The waves are a valuable tool for modeling of various phenomena in the solar system, including particle acceleration and wave-class interactions.
Ayaz explains, “Our earlier work focused on how Kaws contributes to the mysterious capacity of the Sun to heat his corona more than one lakh degrees despite a very cold surface,” Ayaz says. . “Using the CAIRNS distribution function, we discovered magnetic energy conversion, plasma transport and particle acceleration mechanisms into solar corona. However, the carren’s distribution, while the practical, lacks a strong statistical foundation. In this new paper, we create our earlier conclusions by employing Cuppa distribution, providing a statistically recognized strong structure in space plasma research. ,
In Heliopizics, a kappa distribution is a statistical model that describes the velocity distribution of particles in the space plasmas, especially in the solar air. “By increasing our work for this delivery, the researcher says,” we highlight new and attractive details about solar coronal heating, especially how Kaws facilitates energy transfer and particle acceleration. “
“For the first time, Syed has provided a deep understanding of the role of energetic particles on the characteristics of Kinetic alphabet waves, which achieve significant insight into the disintegration of coronal plasma by these important waves, and hence heating,” Dr. Director of Gary Zank, Aergeet/RocketDen Curse and CSPAR in Space Sciences. “Kaws represents the last point of energy transfer in a turbulent magnetized plasma and is an important element in understanding how corona reaches such a high temperature. This is an important step in understanding this long problem about the Sun’s atmosphere. ,
When charged particles interact with wave electrical areas in a plasma, kaws can transfer energy to particles, causing plasma heating at the extended distance.
“This new approach strengthens our understanding of interaction between waves and particles, the mechanisms running the extreme temperature of solar wind and corona,” Ayaz Note. “Cuppa distribution allows us to involve the effects of superthorial particles, which significantly affect the wave-class interaction and dynamics of kaws.”
Supremal particles are charged to ions and electrons that are found throughout the space that moves hundreds of times faster than the thermal plasma of the solar air.
“Our analysis highlights the effect of superthrous particles with electron-to-ion temperature ratio and variation in height relative to the solar radius of the Sun,” Ayaz says. “This broad view shows how these parameters affect the wave-class interaction and energy dynamics in the solar corona.”
In addition, the researcher’s work complements NASA Parker Solar Investigation and ESA’s solar orbiter missions.
“One of the most important findings is our ability to address NASA’s Parker Solar Investigation (PSP) and ESA’s solar orbiter to address the observation difference, which struggles to examine the important area within 10 solar readys, “Ayaz says. “While the closest approach of PSP on 24 December 2024, partially investigates the region, our theoretical structure provides insight into the alphawen wave behavior and their heating contribution to the unwanted 0–10 ready-day region.
“By reducing this difference, our study not only complements observation data, but also provides a forecasting model to understand the dynamics of the wave in the solar corona and the particle acceleration mechanism, ‘one in solving the coronal heating problem Important steps forward. “
Christina Hendrix
256-824-6341
(Email protected)
Julie Jansen
256-824-6926
(Email protected)
ESA’s Solar Orbiter (T) University of Alabama Huntsville