2012A&A...548A..86L


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.02CET03:34:19

2012A&A...548A..86L - Astronomy and Astrophysics, volume 548A, 86-86 (2012/12-1)

A DEBRIS disk around the planet hosting M-star GJ 581 spatially resolved with Herschel.

LESTRADE J.-F., MATTHEWS B.C., SIBTHORPE B., KENNEDY G.M., WYATT M.C., BRYDEN G., GREAVES J.S., THILLIEZ E., MORO-MARTIN A., BOOTH M., DENT W.R.F., DUCHENE G., HARVEY P.M., HORNER J., KALAS P., KAVELAARS J.J., PHILLIPS N.M., RODRIGUEZ D.R., SU K.Y.L. and WILNER D.J.

Abstract (from CDS):

Debris disks have been found primarily around intermediate and solar mass stars (spectral types A-K) but rarely around low mass M-type stars. We have spatially resolved a debris disk around the remarkable M3-type star GJ 581 hosting multiple planets using deep PACS images at 70, 100 and 160µm as part of the DEBRIS Program on the Herschel Space Observatory. This is the second spatially resolved debris disk found around an M-type star, after the one surrounding the young star AU Mic (12Myr). However, GJ 581 is much older (2-8Gyr), and is X-ray quiet in the ROSAT data. We fit an axisymmetric model of the disk to the three PACS images and found that the best fit model is for a disk extending radially from 25±12 AU to more than 60 AU. Such a cold disk is reminiscent of the Kuiper belt but it surrounds a low mass star (0.3M) and its fractional dust luminosity Ldust/L* of ∼10–4 is much higher. The inclination limits of the disk found in our analysis make the masses of the planets small enough to ensure the long-term stability of the system according to some dynamical simulations. The disk is collisionally dominated down to submicron-sized grains and the dust cannot be expelled from the system by radiation or wind pressures because of the low luminosity and low X-ray luminosity of GJ 581. We suggest that the correlation between low-mass planets and debris disks recently found for G-type stars also applies to M-type stars. Finally, the known planets, of low masses and orbiting within 0.3 AU from the star, cannot dynamically perturb the disk over the age of the star, suggesting that an additional planet exists at larger distance that is stirring the disk to replenish the dust.

Abstract Copyright:

Journal keyword(s): circumstellar matter - planetary systems - planets and satellites: formation

Simbad objects: 15

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Number of rows : 15

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NAME Tau-Aur Complex SFR 04 30 +25.0           ~ 1246 0
2 HD 50281B ** 06 52 18.0414038629 -05 11 24.039080436   11.47 10.05 9.870   M2.5V 108 0
3 NGC 2547 OpC 08 09 52.360 -49 10 35.01           ~ 326 0
4 HD 69830 PM* 08 18 23.9469692487 -12 37 55.810202572   6.74 5.95     G8:V 474 1
5 * bet Leo dS* 11 49 03.57834 +14 34 19.4090 2.30 2.22 2.13 2.08 2.06 A3Va 548 0
6 * 61 Vir PM* 13 18 24.3142756 -18 18 40.304648 5.710 5.440 4.740     G6.5V 605 1
7 * alf Boo RG* 14 15 39.67207 +19 10 56.6730 2.46 1.18 -0.05 -1.03 -1.68 K1.5IIIFe-0.5 2165 0
8 BD-07 4003c Pl 15 19 26.8271336166 -07 43 20.190958776           ~ 99 1
9 BD-07 4003 BY* 15 19 26.8271336166 -07 43 20.190958776 13.403 11.76 10.560 9.461 8.911 M3V 550 2
10 BD-07 4003d Pl 15 19 26.8271336166 -07 43 20.190958776           ~ 139 1
11 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3133 1
12 V* AU Mic LM* 20 45 09.5323695486 -31 20 27.241710746   10.05 8.627 9.078 6.593 M1VeBa1 930 0
13 HD 204961b Pl 21 33 33.9749932664 -49 00 32.403471949           ~ 44 1
14 HD 204961 PM* 21 33 33.9749932664 -49 00 32.403471949 11.359 10.176 8.672 7.665 6.479 M2/3V 220 1
15 BD-15 6290 BY* 22 53 16.7323107416 -14 15 49.303409936 12.928 11.749 10.192 9.013 7.462 M3.5V 877 1

    Equat.    Gal    SGal    Ecl

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2021.03.02-03:34:19

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