2011A&A...533A.132E


Query : 2011A&A...533A.132E

2011A&A...533A.132E - Astronomy and Astrophysics, volume 533A, 132-132 (2011/9-1)

Multi-wavelength modeling of the spatially resolved debris disk of HD 107146.

ERTEL S., WOLF S., METCHEV S., SCHNEIDER G., CARPENTER J.M., MEYER M.R., HILLENBRAND L.A. and SILVERSTONE M.D.

Abstract (from CDS):

We aim to constrain the location, composition, and dynamical state of planetesimal populations and dust around the young, sun-like (G2V) star HD107146. We consider coronagraphic observations obtained with the Advanced Camera for Surveys (HST/ACS) onboard the Hubble Space Telescope (HST) in broad V (λc≃0.6µm) and broad I (λc≃0.8µm) filters, a resolved 1.3mm map obtained with the Combined Array for Research in Millimeter-wave Astronomy (CARMA), Spitzer/IRS low resolution spectra in the range of 7.6µm to 37.0µm, and the spectral energy distribution (SED) of the object at wavelengths ranging from 3.5µm to 3.1mm. We complement these data with new coronagraphic high resolution observations of the debris disk using the Near Infrared Camera and Multi-Object Spectrometer (HST/NICMOS) aboard the HST in the F110W filter (λc≃1.1µm). The SED and images of the disk in scattered light as well as in thermal reemission are combined in our modeling using a parameterized model for the disk density distribution and optical properties of the dust. A detailed analytical model of the debris disk around HD107146 is presented that allows us to reproduce the almost entire set of spatially resolved and unresolved multi-wavelength observations. Considering the variety of complementary observational data, we are able to break the degeneracies produced by modeling SED data alone. We find the disk to be an extended ring with a peak surface density at 131AU. Furthermore, we find evidence for an additional, inner disk probably composed of small grains released at the inner edge of the outer disk and moving inwards due to Poynting-Robertson drag. A birth ring scenario (i.e., a more or less broad ring of planetesimals creating the dust disk trough collisions) is found to be the most likely explanation of the ringlike shape of the disk.

Abstract Copyright:

Journal keyword(s): stars: individual: HD107146 - techniques: high angular resolution - methods: data analysis - circumstellar matter - infrared: stars

Simbad objects: 11

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Number of rows : 11
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 * eps Eri BY* 03 32 55.8449634 -09 27 29.731165 5.19 4.61 3.73 3.00 2.54 K2V 1752 1
2 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1718 1
3 V* LQ Hya BY* 09 32 25.5684079124 -11 11 04.687410738 9.316 8.761 7.891 7.288 6.815 K1Vp 412 0
4 HIP 56001 * 11 28 35.3158453684 -42 40 39.916028121   7.84 7.68     ~ 15 0
5 HD 107146 PM* 12 19 06.5022221429 +16 32 53.870713669   7.61   6.7   G2V 236 0
6 HD 109573 PM* 12 36 01.0317721349 -39 52 10.222698506   5.786 5.774 7.25 5.81 A0V 569 1
7 HD 118100 Er* 13 34 43.2063348511 -08 20 31.335294003 11.578 10.552 9.372 8.602 7.930 K5Ve 327 0
8 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2549 0
9 * alf PsA b Pl 22 57 39.04625 -29 37 20.0533           ~ 189 1
10 * alf PsA ** 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1146 3
11 HD 218396 El* 23 07 28.7156905667 +21 08 03.302133882   6.21 5.953     F0+VkA5mA5 967 0

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2021.08.06-05:21:42

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