2016A&A...591A.108O


C.D.S. - SIMBAD4 rel 1.7 - 2020.05.29CEST02:11:22

2016A&A...591A.108O - Astronomy and Astrophysics, volume 591A, 108-108 (2016/7-1)

Azimuthal asymmetries in the debris disk around HD 61005A massive collision of planetesimals?

OLOFSSON J., SAMLAND M., AVENHAUS H., CACERES C., HENNING T., MOOR A., MILLI J., CANOVAS H., QUANZ S.P., SCHREIBER M.R., AUGEREAU J.-C., BAYO A., BAZZON A., BEUZIT J.-L., BOCCALETTI A., BUENZLI E., CASASSUS S., CHAUVIN G., DOMINIK C., DESIDERA S., FELDT M., GRATTON R., JANSON M., LAGRANGE A.-M., LANGLOIS M., LANNIER J., MAIRE A.-L., MESA D., PINTE C., ROUAN D., SALTER G., THALMANN C. and VIGAN A.

Abstract (from CDS):

Context. Debris disks offer valuable insights into the latest stages of circumstellar disk evolution, and can possibly help us to trace the outcomes of planetary formation processes. In the age range 10 to 100Myr, most of the gas is expected to have been removed from the system, giant planets (if any) must have already been formed, and the formation of terrestrial planets may be on-going. Pluto-sized planetesimals, and their debris released in a collisional cascade, are under their mutual gravitational influence, which may result into non-axisymmetric structures in the debris disk.
Aims. High angular resolution observations are required to investigate these effects and constrain the dynamical evolution of debris disks. Furthermore, multi-wavelength observations can provide information about the dust dynamics by probing different grain sizes.
Methods. Here we present new VLT/SPHERE and ALMA observations of the debris disk around the 40Myr-old solar-type star HD 61005. We resolve the disk at unprecedented resolution both in the near-infrared (in scattered and polarized light) and at millimeter wavelengths. We perform a detailed modeling of these observations, including the spectral energy distribution.
Results. Thanks to the new observations, we propose a solution for both the radial and azimuthal distribution of the dust grains in the debris disk. We find that the disk has a moderate eccentricity (e∼0.1) and that the dust density is two times larger at the pericenter compared to the apocenter.
Conclusions. With no giant planets detected in our observations, we investigate alternative explanations besides planet-disk interactions to interpret the inferred disk morphology. We postulate that the morphology of the disk could be the consequence of a massive collision between ∼1000km-sized bodies at ∼61au. If this interpretation holds, it would put stringent constraints on the formation of massive planetesimals at large distances from the star.

Abstract Copyright: © ESO, 2016

Journal keyword(s): circumstellar matter - zodiacal dust - techniques: high angular resolution

VizieR on-line data: <Available at CDS (J/A+A/591/A108): list.dat sphere.fits>

Status at CDS:  

Simbad objects: 10

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Number of rows : 10

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 HD 15115 PM* 02 26 16.2457708887 +06 17 33.187984874   7.15 6.80   6.33 F4IV 149 0
2 IC 321 GiG 03 24 29.6043880536 -14 59 07.740946159   15   13.79   ~ 11 0
3 HD 61005 PM* 07 35 47.4624262763 -32 12 14.042600581   8.96 8.22     G8Vk 169 0
4 HD 95086 * 10 57 03.0216129217 -68 40 02.446874288   7.60 7.36     A8III 121 1
5 HD 109573 PM* 12 36 01.0317721349 -39 52 10.222698506   5.786 5.774 7.25 5.81 A0V 549 1
6 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2502 0
7 HD 181327 PM* 19 22 58.9434412361 -54 32 16.979671096   7.50 7.04   6.49 F6V 224 0
8 * alf PsA ** 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1112 3
9 HD 218396 El* 23 07 28.7156905667 +21 08 03.302133882   6.21 5.953     F0+VkA5mA5 888 1
10 NAME Argus Association As* ~ ~           ~ 159 0

    Equat.    Gal    SGal    Ecl

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2020.05.29-02:11:22

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