Potential multi-component structure of the debris disk around HIP 17439 revealed by Herschel/DUNES
Artikel i vetenskaplig tidskrift, 2014

Context. The dust observed in debris disks is produced through collisions of larger bodies left over from the planet/planetesimal formation process. Spatially resolving these disks permits to constrain their architecture and thus that of the underlying planetary/planetesimal system. Aims. Our Herschel open time key program DUNES aims at detecting and characterizing debris disks around nearby, sun-like stars. In addition to the statistical analysis of the data, the detailed study of single objects through spatially resolving the disk and detailed modeling of the data is a main goal of the project. Methods. We obtained the first observations spatially resolving the debris disk around the sun-like star HIP 17439 (HD23484) using the instruments PACS and SPIRE on board the Herschel Space Observatory. Simultaneous multi-wavelength modeling of these data together with ancillary data from the literature is presented. Results. A standard single component disk model fails to reproduce the major axis radial profiles at 70 mu m, 100 mu m, and 160 mu m simultaneously. Moreover, the best-fit parameters derived from such a model suggest a very broad disk extending from few au up to few hundreds of au from the star with a nearly constant surface density which seems physically unlikely. However, the constraints from both the data and our limited theoretical investigation are not strong enough to completely rule out this model. An alternative, more plausible, and better fitting model of the system consists of two rings of dust at approx. 30 au and 90 au, respectively, while the constraints on the parameters of this model are weak due to its complexity and intrinsic degeneracies. Conclusions. The disk is probably composed of at least two components with different spatial locations (but not necessarily detached), while a single, broad disk is possible, but less likely. The two spatially well-separated rings of dust in our best-fit model suggest the presence of at least one high mass planet or several low-mass planets clearing the region between the two rings from planetesimals and dust.

nearby stars

circumstellar matter


solar-type stars

circumstellar material

icy planet



stars: individual: HIP 17439


infrared: stars



main-sequence stars

multiband imaging photometer


S. Ertel

Universite Grenoble Alpes

J. P. Marshall

Universidad Autonoma de Madrid

J. C. Augereau

Universite Grenoble Alpes

A. Krivov

Friedrich Schiller Universitat Jena

T. Lohne

Friedrich Schiller Universitat Jena

C. Eiroa

Universidad Autonoma de Madrid

A. Mora

European Space Astronomy Centre

C. del Burgo

Instituto Nacional de Astrofisica Optica y Electronica

B. Montesinos

European Space Observatory

G. Bryden

Jet Propulsion Laboratory, California Institute of Technology

W. Danchi

NASA Goddard Space Flight Center

F. Kirchschlager

Christian-Albrechts-Universitat zu Kiel

René Liseau

Chalmers, Rymd- och geovetenskap, Radioastronomi och astrofysik

J. Maldonado

Universidad Autonoma de Madrid

G.L. Pilbratt

ESTEC - European Space Research and Technology Centre

C. Schuppler

Friedrich Schiller Universitat Jena

P. Thebault

GEPI - Galaxies, Etoiles, Physique, Instrumentation

G. J. White

Rutherford Appleton Laboratory

Open University

S. Wolf

Christian-Albrechts-Universitat zu Kiel

Astronomy and Astrophysics

0004-6361 (ISSN) 1432-0746 (eISSN)

Vol. 561 Article no. A114- A114


Astronomi, astrofysik och kosmologi