Giant Planets around FGK Stars Probably Form through Core Accretion
文献类型：期刊论文
| 作者 | Wang,Wei1,2; Wang,Liang1,3; Li,Xiang1 ; Chen,Yuqin1,4; Zhao,Gang1,4
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| 刊名 | The Astrophysical Journal
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| 出版日期 | 2018-06-20 |
| 卷号 | 860期号:2 |
| 关键词 | planetary systems planets and satellites: formation planets and satellites: general surveys techniques: photometric techniques: spectroscopic |
| ISSN号 | 0004-637X |
| DOI | 10.3847/1538-4357/aac2cd |
| 英文摘要 | Abstract We present a statistical study of the planet–metallicity (P–M) correlation by comparing the 744 stars with candidate planets (SWPs) in the Kepler field that have been observed with LAMOST, and a sample of distance-independent, fake “twin” stars in the Kepler field with no planet reported (CKSNPs) yet. With well-defined and carefully selected large samples, we find for the first time a turnoff P–M correlation of Δ[Fe/H]SWPs–SNPs, which on average increases from ～0.00 ± 0.03 dex to 0.06 ± 0.03 dex, and to 0.12 ± 0.03 for stars with Earth-, Neptune-, and Jupiter-sized planets successively, and then declines to ～?0.01 ± 0.03 dex for more massive planets or brown dwarfs. Moreover, the percentage of those systems with positive Δ[Fe/H] has the same turnoff pattern. We also find that FG-type stars follow this general trend, but K-type stars are different. Moderate metal enhancement (～0.1–0.2 dex) for K-type stars with planets of radii between 2 and 4 R⊕, compared to CKSNPs is observed, which indicates much higher metallicities are required for Super-Earths and Neptune-sized planets to form around K-type stars. We point out that the P–M correlation is actually metallicity-dependent, i.e., the correlation is positive at solar and supersolar metallicities, and negative at subsolar metallicities. No steady increase of Δ[Fe/H] against planet sizes is observed for rocky planets, excluding the pollution scenario as a major mechanism for the P–M correlation. All these clues suggest that giant planets probably form differently from rocky planets or more massive planets/brown dwarfs, and the core accretion scenario is highly favored, and high metallicity is a prerequisite for massive planets to form. |
| 语种 | 英语 |
| WOS记录号 | IOP:0004-637X-860-2-AAC2CD |
| 出版者 | The American Astronomical Society |
| 源URL | [http://ir.bao.ac.cn/handle/114a11/21945]  |
| 专题 | 中国科学院国家天文台 |
| 作者单位 | 1.Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People’s Republic of China; wangw@nao.cas.cn 2.Chinese Academy of Sciences South America Center for Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People’s Republic of China 3.Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse, D-85748 Garching, Germany 4.School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, People’s Republic of China; gzhao@nao.cas.cn |
| 推荐引用方式 GB/T 7714 | Wang,Wei,Wang,Liang,Li,Xiang,et al. Giant Planets around FGK Stars Probably Form through Core Accretion[J]. The Astrophysical Journal,2018,860(2). |
| APA | Wang,Wei,Wang,Liang,Li,Xiang,Chen,Yuqin,&Zhao,Gang.(2018).Giant Planets around FGK Stars Probably Form through Core Accretion.The Astrophysical Journal,860(2). |
| MLA | Wang,Wei,et al."Giant Planets around FGK Stars Probably Form through Core Accretion".The Astrophysical Journal 860.2(2018). |
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来源：国家天文台
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