Physical Parameters of the Multiplanet Systems HD 106315 and GJ 9827,The Astronomical Journal

当前位置： X-MOL 学术 › Astron. J. › 论文详情

Our official English website, www.x-mol.net, welcomes your feedback! (Note: you will need to create a separate account there.)

Physical Parameters of the Multiplanet Systems HD 106315 and GJ 9827
The Astronomical Journal ( IF 5.1 ) Pub Date : 2020-12-31 , DOI: 10.3847/1538-3881/abca39
Molly R. Kosiarek ₁ , David A. Berardo ₂ , Ian J. M. Crossfield ₃ , Cesar Laguna _{1,

4} , Caroline Piaulet ₅ , Joseph M. Akana Murphy ₁ , Steve B. Howell ₆ , Gregory W. Henry ₇ , Howard Isaacson _{8,

9} , Benjamin Fulton ₁₀ , Lauren M. Weiss ₁₁ , Erik A. Petigura ₁₂ , Aida Behmard ₁₃ , Lea A. Hirsch ₁₄ , Johanna Teske ₁₅ , Jennifer A. Burt ₁₆ , Sean M. Mills ₁₇ , Ashley Chontos ₁₈ , Teo Močnik ₁₉ , Andrew W. Howard ₁₇ , Michael Werner ₁₆ , John H. Livingston ₂₀ , Jessica Krick ₂₁ , Charles Beichman ₂₂ , Varoujan Gorjian ₁₆ , Laura Kreidberg _{23,

24} , Caroline Morley ₂₅ , Jessie L. Christiansen ₂₁ , Farisa Y. Morales ₁₆ , Nicholas J. Scott ₆ , Jeffrey D. Crane ₂₆ , Sharon Xuesong Wang _{27,

28} , Stephen A. Shectman ₂₆ , Lee J. Rosenthal ₁₇ , Samuel K. Grunblatt _{29,

30} , Ryan A. Rubenzahl ₁₇ , Paul A. Dalba ₃₁ , Steven Giacalone ₃₂ , Chiara Dane Villanueva _{1,

4} , Qingtian Liu _{1,

4} , Fei Dai ₁₃ , Michelle L. Hill ₃₁ , Malena Rice ₃₃ , Stephen R. Kane ₃₁ , Andrew W. Mayo _{32,

34}

Affiliation

Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
Department of Physics, and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
Department of Physics & Astronomy, University of Kansas, 1082 Malott,1251 Wescoe Hall Dr., Lawrence, KS 66045, USA
Department of Physics, University of California, Santa Cruz, CA 95064, USA
Department of Physics, and Institute for Research on Exoplanets, Universit de Montral, Montreal, H3T 1J4, Canada
NASA Ames Research Center, Moffett Field, CA 94035, USA
Center of Excellence in Information Systems, Tennessee State University, Nashville, TN 37209, USA
501 Campbell Hall, University of California at Berkeley, Berkeley, CA 94720, USA
Centre for Astrophysics, University of Southern Queensland, Toowoomba, QLD, Australia
NASA Exoplanet Science Institute/Caltech-IPAC, MC 314-6, 1200 E. California Blvd., Pasadena, CA 91125, USA
Institute for Astronomy, University of Hawai‘i, 2680 Woodlawn Dr., Honolulu, HI 96822, USA
Department of Physics & Astronomy, University of California Los Angeles, Los Angeles, CA 90095, USA
Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA
Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA, USA
Earth & Planets Laboratory, Carnegie Institution of Washington, 5241 Broad Branch Rd., NW, Washington, DC 20015, USA
Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91109, USA
Department of Astronomy, California Institute of Technology, Pasadena, CA 91125, USA
Institute for Astronomy, University of Hawai’i,, Honolulu, HI 96822, USA
Gemini Observatory/NSF’s NOIRLab, 670 N. A’ohoku Place, Hilo, HI 96720, USA
Department of Astronomy, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
Caltech/IPAC, 1200 E. California Blvd., Pasadena, CA 91125, USA
IPAC/NASA Exoplanet Science Institute, Caltech, Jet Propulsion Laboratory, USA
Max Planck Institute for Astronomy, Knigstuhl 17, D-69117 Heidelberg, Germany
Center for Astrophysics ∣ Harvard & Smithsonian, 60 Garden St., Cambridge, MA 02138, USA
University of Texas at Austin, Austin, TX 78712, USA
The Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91107, USA
Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USA
Department of Astronomy, Tsinghua University, Beijing 100084, People’s Republic of China
American Museum of Natural History, 200 Central Park West, Manhattan, NY 10024, USA
Center for Computational Astrophysics, Flatiron Institute, 162 5th Ave., Manhattan, NY 10010, USA
Department of Earth and Planetary Sciences, University of California, Riverside, CA 92521, USA
Department of Astronomy, University of California Berkeley, Berkeley, CA 94720-3411, USA
Department of Astronomy, Yale University, New Haven, CT 06511, USA
Centre for Star and Planet Formation, Natural History Museum of Denmark & Niels Bohr Institute, University of Copenhagen, ster Voldgade 5-7, DK-1350 Copenhagen K., Denmark

HD 106315 and GJ 9827 are two bright, nearby stars that host multiple super-Earths and sub-Neptunes discovered by K2 that are well suited for atmospheric characterization. We refined the planets' ephemerides through Spitzer transits, enabling accurate transit prediction required for future atmospheric characterization through transmission spectroscopy. Through a multi-year high-cadence observing campaign with Keck/HIRES and Magellan/PFS, we improved the planets' mass measurements in anticipation of HST transmission spectroscopy. For GJ 9827, we modeled activity-induced radial velocity signals with a Gaussian process informed from the Calcium II H&K lines in order to more accurately model the effect of stellar noise on our data. We found planet masses of M_b = 4.87 ± 0.37 M_⊕, M_c = 1.92 ± 0.49 M_⊕, and M_d = 3.42 ± 0.62 M_⊕. For HD 106315, we found that such activity-radial velocity decorrelation was not effective due to the reduced presence of spots and speculate that this may extend to other hot stars as well (T_(eff) > 6200 K). We found planet masses of M_b = 10.5 ± 3.1 M_⊕ and M_c = 12.0 ± 3.8 M_⊕. We investigated all of the planets' compositions through comparing their masses and radii to a range of interior models. GJ 9827 b and GJ 9827 c are both consistent with an Earth-like rocky composition, GJ 9827 d and HD 106315 b both require additional volatiles and are consistent with moderate amounts of water or hydrogen/helium, and HD 106315 c is consistent with 10% hydrogen/helium by mass.

中文翻译：

多行星系统 HD 106315 和 GJ 9827 的物理参数

HD 106315 和 GJ 9827 是两颗明亮的邻近恒星，它们拥有 K2 发现的多个超级地球和亚海王星，非常适合大气表征。我们通过斯皮策凌日对行星的星历进行了改进，从而通过透射光谱法实现了未来大气表征所需的准确凌日预测。通过与 Keck/HIRES 和 Magellan/PFS 的多年高节奏观测活动，我们改进了行星的质量测量，以预测 HST 透射光谱。对于 GJ 9827，我们使用从 Calcium II H&K 线获得的高斯过程模拟了活动引起的径向速度信号，以便更准确地模拟恒星噪声对我们数据的影响。我们发现行星质量 M_b = 4.87 ± 0.37 M_⊕，M_c = 1.92 ± 0.49 M_⊕，M_d = 3.42 ± 0.62 M_⊕。对于 HD 106315，我们发现这种活动-径向速度去相关由于斑点的减少而无效，并推测这也可能扩展到其他热星（T_(eff) > 6200 K）。我们发现行星质量 M_b = 10.5 ± 3.1 M_⊕ 和 M_c = 12.0 ± 3.8 M_⊕。我们通过将它们的质量和半径与一系列内部模型进行比较来研究所有行星的成分。GJ 9827 b 和 GJ 9827 c 都与类地岩石成分一致，GJ 9827 d 和 HD 106315 b 都需要额外的挥发物并且与适量的水或氢/氦相一致，而 HD 106315 c 与 10 一致氢气/氦气质量百分比。我们发现这种活动-径向速度去相关由于斑点的减少而无效，并推测这也可能扩展到其他热星（T_(eff) > 6200 K）。我们发现行星质量 M_b = 10.5 ± 3.1 M_⊕ 和 M_c = 12.0 ± 3.8 M_⊕。我们通过将它们的质量和半径与一系列内部模型进行比较来研究所有行星的成分。GJ 9827 b 和 GJ 9827 c 都与类地岩石成分一致，GJ 9827 d 和 HD 106315 b 都需要额外的挥发物并且与适量的水或氢/氦相一致，而 HD 106315 c 与 10 一致氢气/氦气质量百分比。我们发现这种活动-径向速度去相关由于斑点的减少而无效，并推测这也可能扩展到其他热星（T_(eff) > 6200 K）。我们发现行星质量 M_b = 10.5 ± 3.1 M_⊕ 和 M_c = 12.0 ± 3.8 M_⊕。我们通过将它们的质量和半径与一系列内部模型进行比较来研究所有行星的成分。GJ 9827 b 和 GJ 9827 c 都与类地岩石成分一致，GJ 9827 d 和 HD 106315 b 都需要额外的挥发物并且与适量的水或氢/氦相一致，而 HD 106315 c 与 10 一致氢气/氦气质量百分比。通过将它们的质量和半径与一系列内部模型进行比较来确定组合物。GJ 9827 b 和 GJ 9827 c 都与类地岩石成分一致，GJ 9827 d 和 HD 106315 b 都需要额外的挥发物并且与适量的水或氢/氦相一致，而 HD 106315 c 与 10氢气/氦气质量百分比。通过将它们的质量和半径与一系列内部模型进行比较来确定组合物。GJ 9827 b 和 GJ 9827 c 都与类地岩石成分一致，GJ 9827 d 和 HD 106315 b 都需要额外的挥发物并且与适量的水或氢/氦相一致，而 HD 106315 c 与 10 一致氢气/氦气质量百分比。

更新日期：2020-12-31

点击分享查看原文

点击收藏

公开下载

阅读更多本刊最新论文