# 2018A&A...616A.116P

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 Query : 2018A&A...616A.116P

2018A&A...616A.116P - Astronomy and Astrophysics, volume 616A, 116-116 (2018/8-1)

Particle accretion onto planets in discs with hydrodynamic turbulence.

PICOGNA G., STOLL M.H.R. and KLEY W.

Abstract (from CDS):

The growth process of protoplanets can be sped up by accreting a large number of solid, pebble-sized objects that are still present in the protoplanetary disc. It is still an open question on how efficient this process works in realistic turbulent discs. We investigate the accretion of pebbles in turbulent discs that are driven by the purely hydrodynamical vertical shear instability (VSI). For this purpose, we performed global 3D simulations of locally isothermal, VSI turbulent discs that have embedded protoplanetary cores from 5 to 100M, which are placed at 5.2 au distance from the star. In addition, we followed the evolution of a swarm of embedded pebbles of different sizes under the action of drag forces between gas and particles in this turbulent flow. Simultaneously, we performed a set of comparison simulations for laminar viscous discs where the particles experience stochastic kicks. For both cases, we measured the accretion rate onto the cores as a function of core mass and Stokes number (τs) of the particles and compared these values to recent magneto-rotational instability (MRI) turbulence simulations. Overall the dynamic is very similar for the particles in the VSI turbulent disc and the laminar case with stochastic kicks. For small mass planets (i.e. 5-10M), well-coupled particles with τs=1, which have a size of about 1m at this location, we find an accretion efficiency (rate of particles accreted over drifting inwards) of about 1.6-3%. For smaller and larger particles, this efficiency is higher. However, the fast inwards drift for τs=1 particles makes them the most effective for rapid growth, leading to mass doubling times of about 20000yr. For masses between 10 and 30M the core reaches the pebble isolation mass and the particles are trapped at the pressure maximum just outside of the planet, shutting off further particle accretion.

Journal keyword(s): accretion, accretion discs - turbulence - planets and satellites: formation - planet-disc interactions

Full paper

 Number of rows : 1
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 HAT-P-13b Pl 08 39 31.8073600797 +47 21 07.275628863           ~ 98 1

 Query : 2018A&A...616A.116P

Basic data :
 HAT-P-13b -- Extra-solar Planet Origin of the objects types : (Ref) Object type as listed in the reference "Ref" (acronym) Object type linked to the acronym according to the original reference () Anterior to 2007, before we can link the objet type to a reference, or given by the CDS team in some particular cases Other object types: Pl (), Pl? (HAT) Syntax of coordinates is : "ra dec (wtype) [error ellipse] quality bibcode" : ra dec : right ascension and declination (unit and frame defined according to your Output Options) Grey values are increasing the original precision due to the computation of frame transformations (wtype) : wavelength class for the origin of the coordinates (Rad, mm, IR, Optical, UV, Xray, Gam) [error ellipse] : measurement uncertainty, on (ra,dec) if the positional angle is 90 degrees, on (majaxis,minaxis) otherwise (in mas at defined epoch in the original catalogue), position angle (in degrees North celestial pole to East) quality : flag of quality E ≥ 10" D : 1-10" (and some old data) C : 0.1-1" B : 0.01-0.1" + 2MASS, Tyc A : VLBI, Hipparcos bibcode : bibcode of the coordinates reference ICRS coord. (ep=J2000) : 08 39 31.8073600797 +47 21 07.275628863 (Optical) [ 0.0271 0.0235 90 ] A Syntax of coordinates is : "ra dec (wtype) [error ellipse] quality bibcode" : ra dec : right ascension and declination (unit and frame defined according to your Output Options) Grey values are increasing the original precision due to the computation of frame transformations (wtype) : wavelength class for the origin of the coordinates (Rad, mm, IR, Optical, UV, Xray, Gam) [error ellipse] : measurement uncertainty, on (ra,dec) if the positional angle is 90 degrees, on (majaxis,minaxis) otherwise (in mas at defined epoch in the original catalogue), position angle (in degrees North celestial pole to East) quality : flag of quality E ≥ 10" D : 1-10" (and some old data) C : 0.1-1" B : 0.01-0.1" + 2MASS, Tyc A : VLBI, Hipparcos bibcode : bibcode of the coordinates reference FK4 coord. (ep=B1950 eq=1950) : 08 36 02.0034130049 +47 31 45.219534373 [ 0.0271 0.0235 90 ] Syntax of coordinates is : "ra dec (wtype) [error ellipse] quality bibcode" : ra dec : right ascension and declination (unit and frame defined according to your Output Options) Grey values are increasing the original precision due to the computation of frame transformations (wtype) : wavelength class for the origin of the coordinates (Rad, mm, IR, Optical, UV, Xray, Gam) [error ellipse] : measurement uncertainty, on (ra,dec) if the positional angle is 90 degrees, on (majaxis,minaxis) otherwise (in mas at defined epoch in the original catalogue), position angle (in degrees North celestial pole to East) quality : flag of quality E ≥ 10" D : 1-10" (and some old data) C : 0.1-1" B : 0.01-0.1" + 2MASS, Tyc A : VLBI, Hipparcos bibcode : bibcode of the coordinates reference Gal coord. (ep=J2000) : 172.4982471062774 +37.5420843820164 [ 0.0271 0.0235 90 ] Syntax of proper motions is : "pm-ra pm-dec [error ellipse] quality bibcode" pm-ra : mu-ra*cos(dec) (expressed in the ICRS system in mas/yr) pm-dec : mu-dec (expressed in the ICRS system in mas/yr) [error ellipse] : error major axis and minor axis (in mas), orientation angle (in deg) quality : flag of quality (A=best quality -> E=worst quality, {� } =unknown quality) bibcode : bibcode of the proper motion reference Proper motions mas/yr : -24.141 -26.346 [0.055 0.045 90] A Syntax of parallax is : 'value quality [error] bibcode' value : parallax value quality : flag of quality (A=best quality -> E=worst quality, {� } =unknown quality) [error] : mean error bibcode : bibcode of the parallax reference Parallaxes (mas): 4.0231 [0.0360] A
', {sourceSize:12, color:'#30a090'})); aladin.on('objectClicked', function(object) { var objName=object.data.MAIN_ID; aladin.showPopup(object.ra,object.dec,'',''+ objName+''); });" title="Show Simbad objects"> Overlay points in this preview
 All (CDSPortal) Send to within arcsec The VizieR photometry tool allows for easy visualization of photometry points extracted around the Simbad position from photometry-enabled catalogues in VizieR. The search radius has to be specified by the user. It is currently limited to a maximum of 30 arcsec. It depends mostly on the precision or quality of the coordinates (SIMBAD and VizieR catalogs), the resolution of the images from which the sources were extracted, source extent, and source crowding. Suggestions are: crowded field: 0.5 to 1.5 arcsec, 3 arcsec otherwise; uncertain coordinates (SIMBAD quality E or coordinates without reference): 5 to 30 arsec (risky!).
 Some important notes on this object about identifications and objects associations. notes: Possible planet (0.851$M_J$, P=2.92d) orbiting around HAT-P-13, see details about HAT-P-13b in the Extrasolar Planets Encyclopaedia.

Hierarchy : number of linked objects
whatever the membership probability is (see description here ) :

 : 1 : 2 Display criteria : All >=90% stars galaxies radio IR <2 arcsec #ref>50

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 HAT-P-13b

 References (98 between 1850 and 2022) (Total 98) Simbad bibliographic survey began in 1850 for stars (at least bright stars) and in 1983 for all other objects (outside the solar system). Follow new references on this object
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2022.08.09-04:24:31