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SUMMARY:A massive planet disruption as the source of dust in TW Hydra prot
 oplanetary disc
DTSTART;VALUE=DATE-TIME:20200513T084500Z
DTEND;VALUE=DATE-TIME:20200513T090500Z
DTSTAMP;VALUE=DATE-TIME:20240704T115619Z
UID:indico-contribution-58@meetings.aip.de
DESCRIPTION:Speakers: Sergei Nayakshin (University of Leicester)\nThe prot
 ostar TW Hydra features the best studied and one of the most unusual proto
 planetary discs. Its dust disc has a cliff-like rollover at 52 AU which co
 incides with a suspected sub-Neptune mass planet recently detected as an a
 zimuthally elongated AU-scale excess in ALMA 1.3 mm continuum (Tsukagoshi 
 +19). Here we build detailed models of dust growth\, dynamics and syntheti
 c disc emission to investigate the origin of TW Hydra's peculiarities.\n\n
 \nWe show that the standard scenario in which the dust in TW Hydra disc is
  primordial accounts neither for the dust morphology nor the excess emissi
 on. We propose an alternative model in which the primordial dust is long c
 onsumed by the star or locked in planets\; the dust currently observed in 
 the system is ejected by the suspected ALMA planet. We show that in this m
 odel the mm-sized dust particles are blown inside the planetary orbit\, na
 turally explaining the dust disc morphology and its relation to the 1.3 mm
  excess. Further\, dust lost by the planet performs a characteristic U-tur
 n relative to the planet producing an azimuthally elongated emission featu
 re similar to the one observed by ALMA. Finally\, the disruption scenario 
 provides an attractive explanation for why one of the oldest protoplanetar
 y discs happens to be tens times more massive in terms of dust than most d
 iscs a fraction of TW Hydra's age.\n\n\nWe consider two scenarios for the 
 nature of the dust-loosing planet. In the first\, a dusty pre-collapse gas
  envelope of a massive core growing in the Core Accretion framework is dis
 rupted\, e.g.\, as a result of a catastrophic encounter. In the second\, a
  massive dusty gas giant planet formed in the Gravitational Instability sc
 enario is disrupted by the energy release in its massive core. In the latt
 er case all of TW Hydra protoplanetary disc\, including its gaseous compon
 ent\, may originate in such a disruption\; the planet mass has to be no la
 rger than 2 Jupiter masses and it must be 5-10 times more abundant in meta
 ls than the Sun.\n\nIf these ideas are correct then future observations of
  TW Hydra\, and potentially other discs\, will allow us to study planet fo
 rmation in an entirely new way -- by analysing the flows of dust and gas r
 ecently belonging to giant planets. Reverse engineering of mass loss from 
 the planets may inform us about their density structure and elemental comp
 osition before the disruption.\n\nhttps://meetings.aip.de/event/1/contribu
 tions/58/
LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall
URL:https://meetings.aip.de/event/1/contributions/58/
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