2020A&A...641A..75L


C.D.S. - SIMBAD4 rel 1.7 - 2020.11.28CET20:52:49

2020A&A...641A..75L - Astronomy and Astrophysics, volume 641A, 75-75 (2020/9-1)

Relating grain size distributions in circumstellar discs to the spectral index at millimetre wavelengths.

LOHNE T.

Abstract (from CDS):

The excess emission seen in spectral energy distributions (SEDs) is commonly used to infer the properties of the emitting circumstellar dust in protoplanetary and debris discs. Most notably, dust size distributions and details of the collision physics are derived from SED slopes at long wavelengths. This paper reviews the approximations that are commonly used and contrasts them with numerical results for the thermal emission. The inferred size distribution indexes p are shown to be greater and more sensitive to the observed sub(mm) spectral indexes, αmm, than previously considered. This effect results from aspects of the transition from small grains with volumetric absorption to bigger grains that absorb and emit near to their surface, controlled by both the real and the imaginary part of the refractive index. The steeper size distributions indicate stronger size-dependence of material strengths or impact velocities or, otherwise, less efficient transport or erosion processes. Strong uncertainties remain because of insufficient knowledge of the material composition, porosity, and optical properties at long wavelengths.

Abstract Copyright: © ESO 2020

Journal keyword(s): opacity - planetary systems - circumstellar matter

Simbad objects: 18

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Number of rows : 18

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 HD 105 PM* 00 05 52.5449273706 -41 45 11.046016405   8.13 7.53     G0V 155 0
2 HD 377 PM* 00 08 25.7456097412 +06 37 00.488182642   8.22 7.59   6.90 G2V 120 0
3 * 49 Cet PM* 01 34 37.7788265080 -15 40 34.898112472   5.667 5.607   5.54 A1V 249 0
4 * q01 Eri PM* 01 42 29.3148822519 -53 44 26.991165270   6.05 5.52     F9V 273 1
5 HD 15115 PM* 02 26 16.2457708887 +06 17 33.187984874   7.15 6.80   6.33 F4IV 157 0
6 * eps Eri BY* 03 32 55.8449634 -09 27 29.731165 5.19 4.61 3.73 3.00 2.54 K2V 1721 1
7 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1678 1
8 HD 61005 PM* 07 35 47.4624262763 -32 12 14.042600581   8.96 8.22     G8Vk 176 0
9 HD 95086 * 10 57 03.0216129217 -68 40 02.446874288   7.60 7.36     A8III 130 1
10 HD 104860 PM* 12 04 33.7309194735 +66 20 11.714041465   8.50 7.91     G0/F9V 74 0
11 HD 107146 PM* 12 19 06.5022221429 +16 32 53.870713669   7.61   6.7   G2V 229 0
12 * eta Crv PM* 12 32 04.2265302 -16 11 45.616473   4.658 4.294     F2V 281 0
13 HD 109573 PM* 12 36 01.0317721349 -39 52 10.222698506   5.786 5.774 7.25 5.81 A0V 560 1
14 HD 131835 * 14 56 54.4676957121 -35 41 43.659216390   8.05 7.86     A2IV 87 0
15 V* AK Sco Ae* 16 54 44.8497760618 -36 53 18.560813962 9.80 9.63 9.00     F5V 240 1
16 HD 181327 PM* 19 22 58.9434412361 -54 32 16.979671096   7.50 7.04   6.49 F6V 234 0
17 V* AU Mic BY* 20 45 09.5323695486 -31 20 27.241710746   10.05 8.627 9.078 6.593 M1VeBa1 912 0
18 * alf PsA ** 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1129 3

    Equat.    Gal    SGal    Ecl

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2020.11.28-20:52:49

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