TY - JOUR
T1 - Planet formation in intermediate-separation binary systems
AU - Panić, O.
AU - Haworth, T. J.
AU - Petr-Gotzens, M. G.
AU - Miley, J.
AU - Van Den Ancker, M.
AU - Vioque, M.
AU - Siess, L.
AU - Parker, R.
AU - Clarke, C. J.
AU - Kamp, I.
AU - Kennedy, G.
AU - Oudmaijer, R. D.
AU - Pascucci, I.
AU - Richards, A. M.S.
AU - Ratzka, T.
AU - Qi, C.
N1 - Publisher Copyright:
© 2021 2020 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.
PY - 2021/3/1
Y1 - 2021/3/1
N2 - We report the first characterization of the individual discs in the intermediate-separation binary systems KK Oph and HD 144668 at millimetre wavelengths. In both systems, the circumprimary and the circumsecondary discs are detected in the millimetre continuum emission, but not in 13CO nor C18O lines. Even though the disc structure is only marginally resolved, we find indications of large-scale asymmetries in the outer regions of the primary discs, most likely due to perturbation by the companion. The derived dust masses are firmly above debris disc level for all stars. The primaries have about three times more dust in their discs than the secondaries. In the case of HD 144668, the opacity spectral index of the primary and secondary differ by a large margin of 0.69, which may be a consequence of the secondary disc being more compact. Upper limits on the gas masses imply less than 0.1 Mjup in any of these discs, meaning that giant planets can no longer form in them. Considering that there have been no massive gas discs identified to date in intermediate-separation binaries (i.e. binaries at a few hundred au separation), this opens space for speculation whether their binarity causes the removal of gas, with tidal interaction truncating the discs and hence shortening the accretion time-scale. More systematic studies in this respect are sorely needed.
AB - We report the first characterization of the individual discs in the intermediate-separation binary systems KK Oph and HD 144668 at millimetre wavelengths. In both systems, the circumprimary and the circumsecondary discs are detected in the millimetre continuum emission, but not in 13CO nor C18O lines. Even though the disc structure is only marginally resolved, we find indications of large-scale asymmetries in the outer regions of the primary discs, most likely due to perturbation by the companion. The derived dust masses are firmly above debris disc level for all stars. The primaries have about three times more dust in their discs than the secondaries. In the case of HD 144668, the opacity spectral index of the primary and secondary differ by a large margin of 0.69, which may be a consequence of the secondary disc being more compact. Upper limits on the gas masses imply less than 0.1 Mjup in any of these discs, meaning that giant planets can no longer form in them. Considering that there have been no massive gas discs identified to date in intermediate-separation binaries (i.e. binaries at a few hundred au separation), this opens space for speculation whether their binarity causes the removal of gas, with tidal interaction truncating the discs and hence shortening the accretion time-scale. More systematic studies in this respect are sorely needed.
KW - (stars:) binaries: visual
KW - planets and satellites: formation
KW - protoplanetary discs
KW - stars: pre-main-sequence
KW - stars: variables: T Tauri, Herbig Ae/Be
KW - submillimetre: planetary systems
KW - techniques: interferometric
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U2 - 10.1093/mnras/staa3834
DO - 10.1093/mnras/staa3834
M3 - Article
AN - SCOPUS:85100764285
SN - 0035-8711
VL - 501
SP - 4317
EP - 4328
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 3
ER -