File:Simulated stellar wind environment for the Proxima Cen system.jpg
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摘要
| 描述 |
English: Simulated stellar wind environment for the Proxima Centauri system. Multidomain models for activity minimum (left) and maximum (right) are shown. The top panels contain the dynamo-generated surface field distributions (in G) used to drive the AWSoM solution within the innermost module (SC; middle panels). This domain contains the orbits of Proxima b (white solid) and the tentative innermost planet Proxima d (white dashed). The purple isosurface corresponds to the Alfvén surface of the stellar wind (${M}_{{\rm{A}}}=1$; see the text for details). The steady-state solution is propagated from the coupling region (105–110 R★) to the entire IH domain (4500 R★ in each Cartesian direction; bottom panels). This domain contains the orbit of Proxima c (yellow). Magenta and green isosurfaces delimitate the slow (${U}_{{\rm{r}}}\lesssim 750$ km s−1) and fast (${U}_{{\rm{r}}}\gtrsim 1500$ km s−1) wind sectors, respectively. Color-coded is the wind dynamic pressure (${P}_{\mathrm{dyn =\rho \,{U}^{2}$) normalized to the nominal Sun–Earth value (∼ 1.5 nPa), visualized on the equatorial plane of both domains. Selected magnetic field lines are shown in white. |
| 来源 | |
| 作者 |
|date=2020-09-16 16:05:19 |source=https://iopscience.iop.org/article/10.3847/2041-8213/abb885 |author=Julián D. Alvarado-Gómez, Jeremy J. Drake, Cecilia Garraffo, Ofer Cohen, Katja Poppenhaeger, Rakesh K. Yadav, and Sofia P. Moschou |permission= |other versions= }}
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