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High-energy Processes in the Bubbles of Wolf-Rayet Stars: The Case of WR 102
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DOI：10.3847/1538-4357/ae5ca0.png)
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Abstract
En 中文
Supersonic winds from massive stars carry great amounts of kinetic power and modify the surrounding interstellar medium. Through this interaction, a stellar bubble is formed. Theoretical studies and recent observations suggest that the winds of massive stars could be sources of Galactic cosmic rays. The first detection of synchrotron emission from the bubble of a single star was reported, indicating the presence of relativistic electrons. Studying the nonthermal emission from a single massive star can help us to better understand the acceleration of particles taking place in massive star clusters. WR 102 is perfect for a case of study. In this work, we present the first high-energy model for the bubble of WR 102: G2.4+1.4. We aim at fitting the radio data and predicting gamma-ray emission. We assume that both electrons and protons are accelerated at the wind shock. We applied a classical model for the stellar bubble and adopted a one-zone model for estimating the radiation produced by the relativistic particles near the acceleration region. Additionally, we computed the expected emission from the protons that diffuse to the outer regions of the bubble. Also, we estimated the leptonic and hadronic contributions expected from cosmic rays. We fitted the observations considering that 3% of the wind kinetic power goes into relativistic electrons and a magnetic field of 250 mu G. The dominant component at high energies is produced by locally accelerated protons reaching the shell. Protons might reach PeV energies in the wind bubble, but the predicted gamma-ray flux is too low to be detectable.
Keywords:
STELLAR WIND BUBBLES
X-RAY
PARTICLE-ACCELERATION
GALACTIC WC
EMISSION
RADIO
FERMI
EVOLUTION
NEBULAE
REGION
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IF:
5.4
Papers:
8.3W
Citations:
32.0W
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