超级蓬松行星
超级蓬松行星（Super-puff）是一种系外行星，其质量仅比地球大几倍，但半径却比海王星大，因此它的平均密度非常低。[1]它们比膨胀的低密度热木星更冷，质量也更小。[1]
已知最极端的例子是开普勒-51周围的三颗行星，都接近木星大小，但密度均低于0.1g/cm 3。[1]这三颗行星于2012年被发现，但它们低密度的特性直到 2014 年才得到确认。[2]另一颗类似的行星是Kepler-87c 。[1]
一种假设是，超级蓬松行星大气层顶部具有大量尘埃连续流出（例如Gliese 3470 b ）——因此观测到的表面实际上是大气层顶部的尘埃。[2]
另一种可能性是，一些超级蓬松行星可能是具有巨大环系统的正常密度行星，如HIP 41378 f。[3]
参考
- ^ 1.0 1.1 1.2 1.3 The Featureless Transmission Spectra of Two Super-Puff Planets, Jessica E. Libby-Roberts, Zachory K. Berta-Thompson, Jean-Michel Desert, Kento Masuda, Caroline V. Morley, Eric D. Lopez, Katherine M. Deck, Daniel Fabrycky, Jonathan J. Fortney, Michael R. Line, Roberto Sanchis-Ojeda, Joshua N. Winn, 28 Oct 2019
- ^ 2.0 2.1 Astronomers Confirm the Existence of Planets That Have the Lightness of Cotton Candy. [2022-02-22]. （原始内容存档于2021-11-19）.
- ^ These So-Called 'Super-Puff' Worlds Could Be Exoplanets with Rings. Discover Magazine. [11 January 2020]. （原始内容存档于2021-11-19）.
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