2014A&A...567A.127S


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.19CEST20:57:09

2014A&A...567A.127S - Astronomy and Astrophysics, volume 567A, 127-127 (2014/7-1)

Collisional modelling of the debris disc around HIP 17439.

SCHUEPPLER C., LOEHNE T., KRIVOV A.V., ERTEL S., MARSHALL J.P. and EIROA C.

Abstract (from CDS):

We present an analysis of the debris disc around the nearby K2 V star HIP 17439. In the context of the Herschel DUNES key programme, the disc was observed and spatially resolved in the far-IR with the Herschel PACS and SPIRE instruments. In a previous study, we assumed that the size and radial distribution of the circumstellar dust are independent power laws. There, several scenarios capable of explaining the observations were suggested after exploring a very broad range of possible model parameters. In this paper, we perform a follow-up in-depth collisional modelling of these scenarios to further distinguish between them. In our models we consider collisions, direct radiation pressure, and drag forces, which are the actual physical processes operating in debris discs. We find that all scenarios discussed in the first paper are physically reasonable and can reproduce the observed spectral energy distribution along with the PACS surface brightness profiles reasonably well. In one model, the dust is produced beyond 120au in a narrow planetesimal belt and is transported inwards by Poynting-Robertson and stellar wind drag. Good agreement with the observed radial profiles would require stellar winds by about an order of magnitude stronger than the solar value, which is not confirmed - although not ruled out - by observations. Another model consists of two spatially separated planetesimal belts, a warm inner and a cold outer one. This scenario would probably imply the presence of planets clearing the gap between the two components. Finally, we show qualitatively that the observations can be explained by assuming the dust is produced in a single, but broad planetesimal disc with a surface density of solids rising outwards, as expected for an extended disc that experiences a natural inside-out collisional depletion. Prospects of distinguishing between the competing scenarios by future observations are discussed.

Abstract Copyright:

Journal keyword(s): circumstellar matter - stars: individual: HIP 17439 - infrared: planetary systems - methods: numerical

Simbad objects: 5

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Number of rows : 5

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 * eps Eri BY* 03 32 55.8449634 -09 27 29.731165 5.19 4.61 3.73 3.00 2.54 K2V 1658 1
2 HD 23484 PM* 03 44 09.1731527402 -38 16 54.372038074 8.449 7.875 6.996 6.516 6.09 K2V 104 0
3 HD 107146 PM* 12 19 06.5022221429 +16 32 53.870713669   7.61   6.7   G2V 211 0
4 HD 202628 PM* 21 18 27.2693236958 -43 20 04.746121764   7.39 6.742     G5V 135 0
5 HD 207129 PM* 21 48 15.7510673466 -47 18 13.020109072   6.18 5.58     G2V 280 0

    Equat.    Gal    SGal    Ecl

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2019.10.19-20:57:09

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