On the radio detectability of circumplanetary discs

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dc.citation.firstpage1850en_US
dc.citation.issueNumber2en_US
dc.citation.journalTitleMonthly Notices of the Royal Astronomical Societyen_US
dc.citation.lastpage1865en_US
dc.citation.volumeNumber479en_US
dc.contributor.authorZhu, Zhaohuanen_US
dc.contributor.authorAndrews, Sean M.en_US
dc.contributor.authorIsella, Andreaen_US
dc.date.accessioned2018-11-09T15:00:03Zen_US
dc.date.available2018-11-09T15:00:03Zen_US
dc.date.issued2018en_US
dc.description.abstractDiscs around young planets, so-called circumplanetary discs (CPDs), are essential for planet growth, satellite formation, and planet detection. We study the millimetre and centimetre emission from accreting CPDs by using the simple α disc model. We find that it is easier to detect CPDs at shorter radio wavelengths (e.g. λ ≲ 1 mm). For example, if the system is 140 pc away from us, deep observations (e.g. 5 h) at ALMA Band 7 (0.87 mm) are sensitive to as small as 0.03 lunar mass of dust in CPDs. If the CPD is around a Jupiter mass planet 20 au away from the host star and has a viscosity parameter α ≲ 0.001, ALMA can detect this disc when it accretes faster than 10−10M⊙yr−1⁠. ALMA can also detect the 'minimum mass sub-nebulae' disc if such a disc exists around a young planet in young stellar objects. However, to distinguish the embedded compact CPD from the circumstellar disc material, we should observe circumstellar discs with large gaps/cavities using the highest resolution possible. We also calculate the CPD fluxes at VLA bands, and discuss the possibility of detecting radio emission from jets/winds launched in CPDs. Finally we argue that, if the radial drift of dust particles is considered, the drifting time-scale for millimetre dust in CPDs can be extremely short. It only takes 102–103 yr for CPDs to lose millimetre dust. Thus, for CPDs to be detectable at radio wavelengths, mm-sized dust in CPDs needs to be replenished continuously, or the disc has a significant fraction of micron-sized dust or a high gas surface density so that the particle drifting time-scale is long, or the radial drift is prevented by other means (e.g. pressure traps).en_US
dc.identifier.citationZhu, Zhaohuan, Andrews, Sean M. and Isella, Andrea. "On the radio detectability of circumplanetary discs." <i>Monthly Notices of the Royal Astronomical Society,</i> 479, no. 2 (2018) Oxford University Press: 1850-1865. https://doi.org/10.1093/mnras/sty1503.en_US
dc.identifier.digitalsty1503en_US
dc.identifier.doihttps://doi.org/10.1093/mnras/sty1503en_US
dc.identifier.urihttps://hdl.handle.net/1911/103313en_US
dc.language.isoengen_US
dc.publisherOxford University Pressen_US
dc.rightsArticle is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.en_US
dc.subject.keywordradiation mechanisms: thermalen_US
dc.subject.keywordplanets and satellites: detectionen_US
dc.subject.keywordplanet-disc interactionsen_US
dc.subject.keywordprotoplanetary discsen_US
dc.subject.keywordbrown dwarfsen_US
dc.subject.keywordradio continuum: planetary systemsen_US
dc.subject.keywordsubmillimetre: planetary systemsen_US
dc.titleOn the radio detectability of circumplanetary discsen_US
dc.typeJournal articleen_US
dc.type.dcmiTexten_US
dc.type.publicationpublisher versionen_US
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