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首页> 外文期刊>The Astrophysical journal >THE DYNAMICAL EVOLUTION OF THE SHORT-PERIOD EXTRASOLAR PLANET AROUND v ANDROMEDAE IN THE PRE-MAIN-SEQUENCE STAGE
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THE DYNAMICAL EVOLUTION OF THE SHORT-PERIOD EXTRASOLAR PLANET AROUND v ANDROMEDAE IN THE PRE-MAIN-SEQUENCE STAGE

机译：主序阶段初中围绕v ANDROMEDAE的短时太阳系外行星的动力学演化

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We study the dynamical evolution of short-period planets in the multiple planetary system during the epoch of protostellar disk depletion. Through a detailed case analysis for the triple-planet system around v Andromedae, we identify the necessary condition for the survival of its short-period planet b. In this study, we calculate the planets' orbit evolution including effects of the post-Newtonian potential of the host star, the potential of an evolving disk, and the potential due to the flattening of the star produced by the stellar rotation and the tide from the planet. At its present-day semimajor axis of 0.059 AU, the negligible eccentricity of planet b is most likely damped by the dissipation of the tidal perturbation induced by the star on the planet. But this process also leads to the heating of the planets' interior and probably the inflation of their sizes. If planet b once had an eccentricity greater than 0.1 at its present location, the tidal dissipation process would induce it to overflow its Roche lobe, lose its mass, and undergo an orbital expansion. Using this constraint, we reconstruct the eccentricity evolution of planet b. We find that even if planet b arrives at its present location on a nearly circular orbit, its eccentricity could have been excited by the sweeping secular resonances of two outer planets, c and d, during the disk depletion. In addition to the contribution from the disk potential, the resonant condition is also modified by the precession of planet b due to the post-Newtonian correction and rotational distortion of v And's gravitational potential. Today, the former effect offsets the secular resonance, whereas the latter effect is weak. But during the depletion of the disk, precession due to the relativistic correction is outpaced by that due to the disk potential. The passage of the sweeping secular resonance near the surface of v And cannot be avoided unless it had a sufficiently fast spin to provide a flattened shape with a finite quadrupole moment, which dominates the precession of the planet's orbit. Finally, we show that the survival of planet b requires its eccentricity to be low at all times, which would be possible only if the spin period of v And was shorter than 2 days during the depletion of the disk.
机译：我们研究了在原恒星盘耗尽时期多行星系统中短周期行星的动力学演化。通过围绕v Andromedae的三行星系统的详细案例分析，我们确定了其短周期行星b生存的必要条件。在这项研究中，我们计算了行星的轨道演化，包括主恒星的牛顿后势，旋转盘的势以及恒星自转和潮汐产生的恒星产生的扁平化所产生的势的影响。星球。在当今的0.059 AU半长轴上，行星b的微不足道的偏心极有可能被恒星引起的潮汐扰动的消散所抑制。但是，这一过程也会导致行星内部发热，并可能导致其尺寸膨胀。如果b行星在当前位置曾经有一个大于0.1的偏心率，潮汐消散过程将使它溢出Roche瓣，失去其质量，并经历轨道膨胀。利用这个约束，我们重建了行星b的离心率演化。我们发现，即使行星b在接近圆形的轨道上到达其当前位置，在盘耗尽期间，两个外行星c和d的广泛的长期共振也可能激发了它的偏心率。除了来自磁盘电位的贡献外，由于牛顿后修正和v And引力电位的旋转畸变，行星b的进动也改变了共振条件。今天，前者的作用抵消了长期的共振，而后者的作用却很弱。但是在磁盘耗尽期间，由于相对论性校正而导致的进动被由于磁盘势能所导致的进动超过了。除非存在足够快的自旋以提供具有有限四极矩的扁平形状（这主导了行星轨道的进动），否则无法避免在v and表面附近掠过的长期共振通过。最后，我们表明，行星b的生存要求其偏心率始终保持较低，只有当v And的自转周期小于磁盘耗尽期间的2天时，这才有可能。

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