2017AJ....153..226S


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.17CEST04:25:17

2017AJ....153..226S - Astron. J., 153, 226-226 (2017/May-0)

The inner 25 au Debris distribution in the ε Eri system.

SU K.Y.L., DE BUIZER J.M., RIEKE G.H., KRIVOV A.V., LOHNE T., MARENGO M., STAPELFELDT K.R., BALLERING N.P. and VACCA W.D.

Abstract (from CDS):

Debris disk morphology is wavelength dependent due to the wide range of particle sizes and size-dependent dynamics influenced by various forces. Resolved images of nearby debris disks reveal complex disk structures that are difficult to distinguish from their spectral energy distributions. Therefore, multi-wavelength resolved images of nearby debris systems provide an essential foundation to understand the intricate interplay between collisional, gravitational, and radiative forces that govern debris disk structures. We present the Stratospheric Observatory for Infrared Astronomy (SOFIA) 35 µm resolved disk image of ε Eri, the closest debris disk around a star similar to the early Sun. Combining with the Spitzer resolved image at 24 µm and 15-38 µm excess spectrum, we examine two proposed origins of the inner debris in ε Eri: (1) in situ planetesimal belt(s) and (2) dragged-in grains from the cold outer belt. We find that the presence of in situ dust-producing planetesmial belt(s) is the most likely source of the excess emission in the inner 25 au region. Although a small amount of dragged-in grains from the cold belt could contribute to the excess emission in the inner region, the resolution of the SOFIA data is high enough to rule out the possibility that the entire inner warm excess results from dragged-in grains, but not enough to distinguish one broad inner disk from two narrow belts.

Abstract Copyright: © 2017. The American Astronomical Society. All rights reserved.

Journal keyword(s): circumstellar matter - infrared: stars - planetary systems - stars: individual: ε Eri - stars: individual: ε Eri

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 - 2019
#notes
1 * tau Cet PM* 01 44 04.0834226 -15 56 14.926552 4.43 4.22 3.50 2.88 2.41 G8V 1062 1
2 * eps Eri b Pl 03 32 55.84496 -09 27 29.7312           ~ 102 1
3 * eps Eri BY* 03 32 55.8449634 -09 27 29.731165 5.19 4.61 3.73 3.00 2.54 K2V 1658 1
4 NAME Eri Region reg 04 00 -20.0           ~ 37 0
5 * alf Tau LP? 04 35 55.23907 +16 30 33.4885 4.32 2.40 0.86 -0.37 -1.31 K5+III 1167 1
6 * 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 2090 0
7 * bet UMi V* 14 50 42.32580 +74 09 19.8142 5.32 3.55 2.08 0.97 0.21 K4-III 297 1
8 * gam Dra * 17 56 36.36988 +51 29 20.0242 5.630 3.760 2.230 1.08 0.23 K5III 511 0
9 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2472 0
10 V* AU Mic BY* 20 45 09.5323695486 -31 20 27.241710746   10.05 8.627 9.078 6.593 M1VeBa1 868 0
11 * alf PsA ** 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1099 3

    Equat.    Gal    SGal    Ecl

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2019.10.17-04:25:17

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