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Observational Signatures of Planet Formation in Recent Resolved Observations of Protoplanetary Disks

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Formation, Evolution, and Dynamics of Young Solar Systems

Part of the book series: Astrophysics and Space Science Library ((ASSL,volume 445))

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Abstract

Planets form in gaseous protoplanetary disks surrounding newborn stars. As such, the best way to learn how planets form from observations is to directly watch them forming in disks. By doing so, we can directly address the three most fundamental questions in planet formation : when, where, and how planets form. In the past, due to the difficulties in directly detecting planets in disks, planet formation has been a subject of theoretical astrophysics. Now, thanks to a fleet of new instruments with unprecedented resolving power that have come online in the past decade, we have just started to be able to directly resolve structures in protoplanetary disks that are unambiguously associated with planet formation activities. By comparing these observations with theoretical models of disk–planet interactions , we will be able to constrain the locations and properties of the (unseen) planets. This is the onset of a new field—observational planet formation. In this chapter, we highlight selected recent progresses in this field, with emphases on numerical modeling of observational signatures of planet-induced structures in disks, as well as the comparison between models and observations.

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Notes

  1. 1.

    The two most prolific techniques, radial velocity and transit surveys , demand the target star to be quiet and stable, so that the tiny signal introduced by the motion of a planet can be disentangled from the light curve of the star. Newborn stars tend to be too active, which largely washes out the planetary signal (although see David et al. 2016). Meanwhile, protoplanetary disks are often bright at near-to-mid-infrared wavelengths, which renders identifying planets through direct imaging difficult.

  2. 2.

    The inner working angle in scattered light imaging observations of disks indicates the minimum angular separation from the star, inside which disk structures cannot be accessed.

  3. 3.

    Really massive companions , such as stellar mass companions, may be able to open gaps wide enough, though their presences have generally been ruled out in direct imaging observations.

  4. 4.

    We note that in early stage protostellar disks, GI-induced spiral arms may have been found (Liu et al. 2016; Dong et al. 2016b); however, these arms are on the scale of hundreds of AU and are different from the arms in disks at late stages discussed in this chapter.

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Acknowledgements

We thank Jonathan Williams for sharing with us the mm transitional disk mozaic in Fig. 9.2. This project is partially supported by NASA through Hubble Fellowship grants HST-HF-51333.01-A (Z.Z.) and HST-HF-51320.01-A (R.D.) awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. J.F. gratefully acknowledges support from the Natural Sciences and Engineering Research Council of Canada, the Center for Integrative Planetary Science at the University of California, Berkeley, and the Sagan Fellowship Program under contract with the Jet Propulsion Laboratory (JPL) funded by NASA and executed by the NASA Exoplanet Science Institution.

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  1. Department of Astronomy, UC Berkeley, Berkeley, CA, 94705, USA

    Ruobing Dong & Jeffrey Fung

  2. Department of Astrophysical Sciences, Princeton University, Princeton, NJ, 08544, USA

    Zhaohuan Zhu

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  1. Ruobing Dong
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Correspondence to Ruobing Dong .

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  1. The Niels Bohr Institute, Niels Bohr International Academy, Copenhagen, Denmark

    Martin Pessah

  2. The Niels Bohr Institute, Niels Bohr International Academy, Copenhagen, Denmark

    Oliver Gressel

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Dong, R., Zhu, Z., Fung, J. (2017). Observational Signatures of Planet Formation in Recent Resolved Observations of Protoplanetary Disks. In: Pessah, M., Gressel, O. (eds) Formation, Evolution, and Dynamics of Young Solar Systems. Astrophysics and Space Science Library, vol 445. Springer, Cham. https://doi.org/10.1007/978-3-319-60609-5_9

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