arXiv 2101.044162021-01-12astro-ph.SRastro-ph.EP

具有行星的早型恒星的化学分析

Chemical analysis of early-type stars with planets

C. Saffe, P. Miquelarena, J. Alacoria, M. Flores, M. Jaque Arancibia, D. Calvo, G. Martín Girardi, M. Grosso, A. Collado

备注：: 21 pages, 12 figures, 4 tables, A&A accepted
发表信息：: A&A 647, A49 (2021)
DOI：: 10.1051/0004-6361/202040132

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摘要：

目标。探索具有行星的早期型恒星的化学模式，寻找行星形成的可能特征。特别是，我们研究的λ Bootis化学图案和存在的巨行星之间的可能关系。方法.我们进行了详细的丰度测定的早期型恒星的样本，通过光谱合成的行星和没有。结果我们比较了样本中恒星的化学模式（13颗有行星的恒星和24颗没有探测到行星的恒星）与Lambda Bootis和其他化学性质特殊的恒星。我们在样本中发现了四颗牧夫座λ恒星，其中两颗存在行星和拱星盘（HR 8799和HD 169142），一颗没有检测到行星（HD 110058）。我们还发现了第一颗被棕矮星（zeta Del）环绕的牧夫座λ星。这对有趣的牧夫座λ星+褐矮星可以帮助测试恒星形成的场景。我们没有发现这组带有巨行星的早期型恒星的独特化学模式。然而，我们的研究结果支持，在原则上，一个建议的情况下，巨大的行星轨道前主序星可能会阻止磁盘的尘埃，并导致在一个lambda Bootis样的模式。另一方面，我们没有发现一个λ Bootis模式在不同的热木星行星的宿主恒星，这不支持的想法可能吸积从风的热木星，最近提出的文献。然后，其他机制应该解释主序恒星之间的λ牧夫座图案的存在。最后，我们认为，围绕Lambda Bootis恒星（如HR 8799和HD 169142）的行星也可能通过核心吸积过程而不仅仅是引力不稳定性形成。

英文摘要：

Aims. To explore the chemical pattern of early-type stars with planets, searching for a possible signature of planet formation. In particular, we study a likely relation between the lambda Bootis chemical pattern and the presence of giant planets. Methods. We performed a detailed abundance determination in a sample of early-type stars with and without planets via spectral synthesis. Results. We compared the chemical pattern of the stars in our sample (13 stars with planets and 24 stars without detected planets) with those of lambda Bootis and other chemically peculiar stars. We have found four lambda Bootis stars in our sample, two of which present planets and circumstellar disks (HR 8799 and HD 169142) and one without planets detected (HD 110058). We have also identified the first lambda Bootis star orbited by a brown dwarf (zeta Del). This interesting pair lambda Bootis star + brown dwarf could help to test stellar formation scenarios. We found no unique chemical pattern for the group of early-type stars bearing giant planets. However, our results support, in principle, a suggested scenario in which giant planets orbiting pre-main-sequence stars possibly block the dust of the disk and result in a lambda Bootis-like pattern. On the other hand, we do not find a lambda Bootis pattern in different hot-Jupiter planet host stars, which do not support the idea of possible accretion from the winds of hot-Jupiters, recently proposed in the literature. Then, other mechanisms should account for the presence of the lambda Bootis pattern between main-sequence stars. Finally, we suggest that the formation of planets around lambda Bootis stars such as HR 8799 and HD 169142 is also possible through the core accretion process and not only gravitational instability [abridged]

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