A 'Rosetta Stone' for protoplanetary disks

the synergy of multi-wavelength observations

A. Sicilia-Aguilar (Lead / Corresponding author), A. Banzatti, A. Carmona, T. Stolker, M. Kama, I. Mendigutia, A. Garufi, K. Flaherty, N. van der Marel, J. Greaves

Research output: Contribution to journalArticle

8 Citations (Scopus)
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Abstract

The recent progress in instrumentation and telescope development has brought us different ways to observe protoplanetary disks, including interferometers, space missions, adaptive optics, polarimetry, and time- and spectrally-resolved data. While the new facilities have changed the way we can tackle the existing open problems in disk structure and evolution, there is a substantial lack of interconnection between different observing techniques and their user communities. Here, we explore the complementarity of some of the state-of-the-art observing techniques, and how they can be brought together in a collective effort to understand how disks evolve and disperse at the time of planet formation.This paper was born at the "Protoplanetary Discussions" meeting in Edinburgh, 2016. Its goal is to clarify where multi-wavelength observations of disks converge in unveiling disk structure and evolution, and where they diverge and challenge our current understanding. We discuss caveats that should be considered when linking results from different observations, or when drawing conclusions based on limited datasets (in terms of wavelength or sample). We focus on disk properties that are currently being revolutionized by multi-wavelength observations. Specifically: the inner disk radius, holes and gaps and their link to large-scale disk structures, the disk mass, and the accretion rate. We discuss how the links between them, as well as the apparent contradictions, can help us to disentangle the disk physics and to learn about disk evolution.
Original languageEnglish
Article numbere059
Pages (from-to)1-31
Number of pages31
JournalPublications of the Astronomical Society of Australia
Volume33
DOIs
Publication statusPublished - 13 Dec 2016

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protoplanetary disks
rocks
wavelength
wavelengths
complementarity
interferometer
instrumentation
physics
planet
accretion
stone
polarimetry
space missions
adaptive optics
planets
interferometers
telescopes
radii

Keywords

  • Protoplanetary disks
  • Methods: observational
  • Planets: formation
  • Astronomical instrumentation, methods and techniques

Cite this

Sicilia-Aguilar, A. ; Banzatti, A. ; Carmona, A. ; Stolker, T. ; Kama, M. ; Mendigutia, I. ; Garufi, A. ; Flaherty, K. ; Marel, N. van der ; Greaves, J. / A 'Rosetta Stone' for protoplanetary disks : the synergy of multi-wavelength observations. In: Publications of the Astronomical Society of Australia. 2016 ; Vol. 33. pp. 1-31.
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Sicilia-Aguilar, A, Banzatti, A, Carmona, A, Stolker, T, Kama, M, Mendigutia, I, Garufi, A, Flaherty, K, Marel, NVD & Greaves, J 2016, 'A 'Rosetta Stone' for protoplanetary disks: the synergy of multi-wavelength observations', Publications of the Astronomical Society of Australia, vol. 33, e059, pp. 1-31. https://doi.org/10.1017/pasa.2016.56

A 'Rosetta Stone' for protoplanetary disks : the synergy of multi-wavelength observations. / Sicilia-Aguilar, A. (Lead / Corresponding author); Banzatti, A.; Carmona, A.; Stolker, T.; Kama, M.; Mendigutia, I. ; Garufi, A.; Flaherty, K.; Marel, N. van der; Greaves, J.

In: Publications of the Astronomical Society of Australia, Vol. 33, e059, 13.12.2016, p. 1-31.

Research output: Contribution to journalArticle

TY - JOUR

T1 - A 'Rosetta Stone' for protoplanetary disks

T2 - the synergy of multi-wavelength observations

AU - Sicilia-Aguilar, A.

AU - Banzatti, A.

AU - Carmona, A.

AU - Stolker, T.

AU - Kama, M.

AU - Mendigutia, I.

AU - Garufi, A.

AU - Flaherty, K.

AU - Marel, N. van der

AU - Greaves, J.

PY - 2016/12/13

Y1 - 2016/12/13

N2 - The recent progress in instrumentation and telescope development has brought us different ways to observe protoplanetary disks, including interferometers, space missions, adaptive optics, polarimetry, and time- and spectrally-resolved data. While the new facilities have changed the way we can tackle the existing open problems in disk structure and evolution, there is a substantial lack of interconnection between different observing techniques and their user communities. Here, we explore the complementarity of some of the state-of-the-art observing techniques, and how they can be brought together in a collective effort to understand how disks evolve and disperse at the time of planet formation.This paper was born at the "Protoplanetary Discussions" meeting in Edinburgh, 2016. Its goal is to clarify where multi-wavelength observations of disks converge in unveiling disk structure and evolution, and where they diverge and challenge our current understanding. We discuss caveats that should be considered when linking results from different observations, or when drawing conclusions based on limited datasets (in terms of wavelength or sample). We focus on disk properties that are currently being revolutionized by multi-wavelength observations. Specifically: the inner disk radius, holes and gaps and their link to large-scale disk structures, the disk mass, and the accretion rate. We discuss how the links between them, as well as the apparent contradictions, can help us to disentangle the disk physics and to learn about disk evolution.

AB - The recent progress in instrumentation and telescope development has brought us different ways to observe protoplanetary disks, including interferometers, space missions, adaptive optics, polarimetry, and time- and spectrally-resolved data. While the new facilities have changed the way we can tackle the existing open problems in disk structure and evolution, there is a substantial lack of interconnection between different observing techniques and their user communities. Here, we explore the complementarity of some of the state-of-the-art observing techniques, and how they can be brought together in a collective effort to understand how disks evolve and disperse at the time of planet formation.This paper was born at the "Protoplanetary Discussions" meeting in Edinburgh, 2016. Its goal is to clarify where multi-wavelength observations of disks converge in unveiling disk structure and evolution, and where they diverge and challenge our current understanding. We discuss caveats that should be considered when linking results from different observations, or when drawing conclusions based on limited datasets (in terms of wavelength or sample). We focus on disk properties that are currently being revolutionized by multi-wavelength observations. Specifically: the inner disk radius, holes and gaps and their link to large-scale disk structures, the disk mass, and the accretion rate. We discuss how the links between them, as well as the apparent contradictions, can help us to disentangle the disk physics and to learn about disk evolution.

KW - Protoplanetary disks

KW - Methods: observational

KW - Planets: formation

KW - Astronomical instrumentation, methods and techniques

UR - https://research-repository.st-andrews.ac.uk/handle/10023/10988

U2 - 10.1017/pasa.2016.56

DO - 10.1017/pasa.2016.56

M3 - Article

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SP - 1

EP - 31

JO - Publications of the Astronomical Society of Australia

JF - Publications of the Astronomical Society of Australia

SN - 1323-3580

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