Ertel, Suitbert

[["dc.bibliographiccitation.artnumber","A11"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","555"],["dc.contributor.author","Eiroa, C."],["dc.contributor.author","Marshall, J. P."],["dc.contributor.author","Mora, A."],["dc.contributor.author","Montesinos, B."],["dc.contributor.author","Absil, O."],["dc.contributor.author","Augereau, J. Ch."],["dc.contributor.author","Bayo, A."],["dc.contributor.author","Bryden, G."],["dc.contributor.author","Danchi, W."],["dc.contributor.author","del Burgo, C."],["dc.contributor.author","Ertel, Suitbert"],["dc.contributor.author","Fridlund, M."],["dc.contributor.author","Heras, A. M."],["dc.contributor.author","Krivov, A. V."],["dc.contributor.author","Launhardt, R."],["dc.contributor.author","Liseau, R."],["dc.contributor.author","Loehne, T."],["dc.contributor.author","Maldonado, J."],["dc.contributor.author","Pilbratt, G. L."],["dc.contributor.author","Roberge, A."],["dc.contributor.author","Rodmann, Jens"],["dc.contributor.author","Sanz-Forcada, J."],["dc.contributor.author","Solano, E."],["dc.contributor.author","Stapelfeldt, K."],["dc.contributor.author","Thebault, P."],["dc.contributor.author","Wolf, S."],["dc.contributor.author","Ardila, D."],["dc.contributor.author","Arevalo, M."],["dc.contributor.author","Beichmann, C."],["dc.contributor.author","Faramaz, V."],["dc.contributor.author","Gonzalez-Garcia, B. M."],["dc.contributor.author","Gutierrez, R- A."],["dc.contributor.author","Lebreton, J."],["dc.contributor.author","Martinez-Arnaiz, R."],["dc.contributor.author","Meeus, G."],["dc.contributor.author","Montes, D."],["dc.contributor.author","Olofsson, G."],["dc.contributor.author","Su, K. Y. L."],["dc.contributor.author","White, G. J."],["dc.contributor.author","Barrado, D."],["dc.contributor.author","Fukagawa, M."],["dc.contributor.author","Gruen, E."],["dc.contributor.author","Kamp, I."],["dc.contributor.author","Lorente, R."],["dc.contributor.author","Morbidelli, A."],["dc.contributor.author","Mueller, S."],["dc.contributor.author","Mutschke, H."],["dc.contributor.author","Nakagawa, T."],["dc.contributor.author","Ribas, I."],["dc.contributor.author","Walker, H."],["dc.date.accessioned","2018-11-07T09:22:46Z"],["dc.date.available","2018-11-07T09:22:46Z"],["dc.date.issued","2013"],["dc.description.abstract","Context. Debris discs are a consequence of the planet formation process and constitute the fingerprints of planetesimal systems. Their solar system counterparts are the asteroid and Edgeworth-Kuiper belts. Aims. The DUNES survey aims at detecting extra-solar analogues to the Edgeworth-Kuiper belt around solar-type stars, putting in this way the solar system into context. The survey allows us to address some questions related to the prevalence and properties of planetesimal systems. Methods. We used Herschel/PACS to observe a sample of nearby FGK stars. Data at 100 and 160 mu m were obtained, complemented in some cases with observations at 70 mu m, and at 250, 350 and 500 mu m using SPIRE. The observing strategy was to integrate as deep as possible at 100 mu m to detect the stellar photosphere. Results. Debris discs have been detected at a fractional luminosity level down to several times that of the Edgeworth-Kuiper belt. The incidence rate of discs around the DUNES stars is increased from a rate of similar to 12.1% +/- 5% before Herschel to similar to 20.2% +/- 2%. A significant fraction (similar to 52%) of the discs are resolved, which represents an enormous step ahead from the previously known resolved discs. Some stars are associated with faint far-IR excesses attributed to a new class of cold discs. Although it cannot be excluded that these excesses are produced by coincidental alignment of background galaxies, statistical arguments suggest that at least some of them are true debris discs. Some discs display peculiar SEDs with spectral indexes in the 70-160 mu m range steeper than the Rayleigh-Jeans one. An analysis of the debris disc parameters suggests that a decrease might exist of the mean black body radius from the F-type to the K-type stars. In addition, a weak trend is suggested for a correlation of disc sizes and an anticorrelation of disc temperatures with the stellar age."],["dc.identifier.doi","10.1051/0004-6361/201321050"],["dc.identifier.fs","605000"],["dc.identifier.isi","000322008600011"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/10655"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/29427"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","1432-0746"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","DUst around NEarby Stars. The survey observational results"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A61"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","544"],["dc.contributor.author","Ertel, Suitbert"],["dc.contributor.author","Wolf, S."],["dc.contributor.author","Rodmann, Jens"],["dc.date.accessioned","2018-11-07T09:07:34Z"],["dc.date.available","2018-11-07T09:07:34Z"],["dc.date.issued","2012"],["dc.description.abstract","Context. Debris disks are commonly considered to be a by-product of planet formation. Structures in debris disks induced by planet-disk interaction are promising to provide valuable constraints on the existence and properties of embedded planets. Aims. We investigate the observability of structures in debris disks induced by planet-disk interaction with future facilities in a systematic way. High-sensitivity, high angular resolution observations with large (sub-) mm interferometers and large space-based telescopes operating in the near-to mid-infrared wavelength range are considered. Methods. The observability of debris disks with the Atacama LargeMillimeter/submillimeter Array (ALMA) is studied on the basis of a simple analytical disk model. Furthermore, N-body simulations are used to model the spatial dust distribution in debris disks under the influence of planet-disk interaction. From these simulations, images at optical scattered light to millimeter thermal re-emission are computed. Available information about the expected capabilities of ALMA and the James Webb Space Telescope (JWST) are used to investigate the observability of characteristic disk structures with these facilities through spatially resolved imaging. Results. Our simulations show that planet-disk interaction can result in prominent structures in the whole considered wavelength range. The exact result depends on the configuration of the planet-disk system and on the observing wavelength which provides the opportunity of detecting and characterizing extrasolar planets in a range of masses and radial distances from the star that is not accessible to other techniques. Facilities that will be available in the near future at both considered wavelength ranges are shown to provide the capabilities to spatially resolve and characterize structures in debris disks that arise because of planet-disk interaction. Limitations are revealed and suggestions for possible instrument setups and observing strategies are given. In particular, ALMA is limited by its sensitivity to surface brightness, which requires a trade-off between sensitivity and spatial resolution. Space-based mid-infrared observations will be able to detect and spatially resolve regions in debris disks even at a distance of several tens of AU from the star, where the emission from debris disks in this wavelength range is expected to be low. Conclusions. Both ALMA and the planned space-based near-to mid-infrared telescopes will provide unprecedented capabilities to study planet-disk interaction in debris disks. In particular, a combination of observations at both wavelengths will provide very strong constraints on the planetary/planetesimal systems."],["dc.identifier.doi","10.1051/0004-6361/201219236"],["dc.identifier.fs","596751"],["dc.identifier.isi","000308290100061"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9611"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/25826"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","Observing planet-disk interaction in debris disks"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]