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Dynamics of the Spiral-Arm Corotation and Its Observable Footprints in the Solar Neighborhood

期刊

出版社

FRONTIERS MEDIA SA
DOI: 10.3389/fspas.2021.644098

关键词

galaxy; kinematics and dynamics; galaxy; solar neighborhood; galaxy; structure; galaxy; disk; galaxy; spiral structure; methods; numerical

资金

  1. FAPESP [2009/54006-4]
  2. DGAPA-PAPIIT [IG100319]
  3. Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq)
  4. Sao Paulo Research Foundation (FAPESP) [2016/13750-6]
  5. Brazilian agency Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) [302546/2004-9]

向作者/读者索取更多资源

The study reveals that the Sun and most of the stars in the Solar Neighborhood evolve inside a stable zone of the spiral corotation region, oscillating between the Sagittarius-Carina and Perseus arms. These findings provide new insights into our understanding of solar system evolution, changes in Earth's environment, and the preservation of life on Earth.
This article discusses the effects of the spiral-arm corotation on the stellar dynamics in the Solar Neighborhood (SN). All our results presented here rely on: (1) observational evidence that the Sun lies near the corotation circle, where stars rotate with the same angular velocity as the spiral-arm pattern; the corotation circle establishes domains of the corotation resonance (CR) in the Galactic disk; (2) dynamical constraints that put the spiral-arm potential as the dominant perturbation in the SN, comparing with the effects of the central bar in the SN; (3) a long-lived nature of the spiral structure, promoting a state of dynamical relaxing and phase-mixing of the stellar orbits in response to the spiral perturbation. With an analytical model for the Galactic potential, composed of an axisymmetric background deduced from the observed rotation curve, and perturbed by a four-armed spiral pattern, numerical simulations of stellar orbits are performed to delineate the domains of regular and chaotic motions shaped by the resonances. Such studies show that stars can be trapped inside the stable zones of the spiral CR, and this orbital trapping mechanism could explain the dynamical origin of the Local arm of the Milky Way (MW). The spiral CR and the near high-order epicyclic resonances influence the velocity distribution in the SN, creating the observable structures such as moving groups and their radially extended counterpart known as diagonal ridges. The Sun and most of the SN stars evolve inside a stable zone of the spiral CR, never crossing the main spiral-arm structure, but oscillating in the region between the Sagittarius-Carina and Perseus arms. This orbital behavior of the Sun brings insights to our understanding of questions concerning the solar system evolution, the Earth environment changes, and the preservation of life on Earth.

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