(ORDO NEWS) — Dr. He Zhicheng and his colleagues from the China University of Science and Technology of the Chinese Academy of Sciences discovered a new way to measure the physical properties of galactic ionized gas, and for the first time discovered that the acceleration of emissions from quasars occurs at distances of tens of parsecs.
According to current models of galaxy formation and evolution, the feedback mechanism from active galactic nuclei (AGNs) suggests that the evolution of a giant black hole located at the center of the galaxy is influenced by the blowing out of ionized gas, or ejections from the quasar, preventing potential overgrowth black hole.
These outflows, which return matter and energy to the host galaxy, represent one of the most important manifestations of feedback from the AGN.
However, until now, scientists’ knowledge of ejections from active galaxies has been very limited, since one of the most important factors, the scale of outflows, was mainly established from the observed spectral absorption lines shifted to the blue region. The results obtained in this way were unreliable, since they strongly depended on the adopted model.
Dr. He developed a new approach based on his previous research. He suggested that changes in the parameters of blueshifted absorption lines could be a powerful tool for studying outgoing galactic outflows.
In the new work, the scientist develops the proposed method, considering both the amplitude and the phase of the function that describes the reaction of an ionized gas to the action of radiation.
He and his team obtained kinetic data on outflows from the quasar and discovered that the acceleration occurs at distances of the order of tens of parsecs, which is much larger than previous estimates based on the traditional model of accretion disk winds.
Xe and his colleagues also found that dust in the interstellar medium may be responsible for the acceleration of quasar ejections, since the cross section of the interaction zone between dust and ultraviolet radiation from the accretion disk significantly exceeds the cross section of Thomson scattering by free electrons.
The calculations performed by the team confirmed this hypothesis, and the estimated scale of the distances at which the outgoing flow is formed coincided with the scale of the dust ring, which became a reliable confirmation of the above assumption.
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