Cold DUst around NEarby Stars (DUNES). First results

Eiroa, C.; Fedele, D.; Maldonado, J.; González-García, B. M.; Rodmann, J.; Heras, A. M.; Pilbratt, G. L.; Augereau, J.-C.; Mora, A.; Montesinos, B.; Ardila, D. R.; Bryden, G.; Liseau, R.; Stapelfeldt, K.; Launhardt, R.; Solano, E.; Bayo, A.; Absil, Olivier; Arévalo, M. J.; Barrado, D.; Beichmann, C.; Danchi, W. C.; Burgo, C. del; Ertel, S.; Fridlund, M.; Fukagawa, Misato; Gutiérrez, Raúl; Grün, E.; Kamp, I.; Krivov, A. V.; Lebreton, J.; Löhne, T.; Lorente, R.; Marshall, Jonathan P.; Martínez-Arnáiz, R.; Meeus, G.; Montes, D.; Morbidelli, A.; Müller, Sebastian; Mutschke, H.; Nakagawa, Takao; Olofsson, G.; Ribas, I.; Roberge, Aki; Sanz-Forcada, J.; Thébault, P.; Walker, H. J.; White, G. J.; Wolf, S.

doi:10.1051/0004-6361/201014594

Cited by 64 publications

(76 citation statements)

References 18 publications

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“…The disc extent, ∼140 AU, is larger than other DUNES resolved discs, e.g. q 1 Eri (85 AU, Liseau et al 2010) or ζ 2 Ret (70-120 AU, Eiroa et al 2010), but the derived black body temperature is also large, ∼50 K, cf 60 K for the q 1 Eri disc which is around an F star and 30-40 K for the ζ 2 Ret disc which has a smaller extent around a star of similar spectral type.…”

Section: Discussionmentioning

confidence: 75%

AHerschelresolved far-infrared dust ring around HD 207129

Marshall

Löhne

Montesinos

et al. 2011

A&A

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Context. Dusty debris discs around main sequence stars are thought to be the result of continuous collisional grinding of planetesimals in the system. The majority of these systems are unresolved and analysis of the dust properties is limited by the lack of information regarding the dust location. Aims. The Herschel DUNES key program is observing 133 nearby, Sun-like stars (<20 pc, FGK spectral type) in a volume limited survey to constrain the absolute incidence of cold dust around these stars by detection of far infrared excess emission at flux levels comparable to the Edgeworth-Kuiper belt (EKB). Methods. We have observed the Sun-like star HD 207129 with Herschel PACS and SPIRE. In all three PACS bands we resolve a ringlike structure consistent with scattered light observations. Using α Boötis as a reference point spread function (PSF), we deconvolved the images, clearly resolving the inner gap in the disc at both 70 and 100 μm. Results. We have resolved the dust-producing planetesimal belt of a debris disc at 100 μm for the first time. We measure the radial profile and fractional luminosity of the disc, and compare the values to those of discs around stars of similar age and/or spectral type, placing this disc in context of other resolved discs observed by Herschel/DUNES.

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Section: Discussionmentioning

confidence: 75%

AHerschelresolved far-infrared dust ring around HD 207129

Marshall

Löhne

Montesinos

et al. 2011

A&A

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“…Similarly, the structure of the known debris disk of Eri suggests an outer planet (Quillen & Thorndike 2002). But then for HR 8501 that has an RV trend likely due to its wide stellar companion, Eiroa et al (2010) exclude a cold debris disk. Notes.…”

Section: Discussionmentioning

confidence: 99%

The planet search programme at the ESO CES and HARPS

Zechmeister

Kürster

Endl³

et al. 2013

A&A

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Context. In 1992 we began a precision radial velocity survey for planets around solar-like stars with the Coudé Echelle Spectrograph and the Long Camera (CES LC) at the 1.4 m telescope in La Silla (Chile) resulting in the discovery of the planet ι Hor b. We have continued the survey with the upgraded CES Very Long Camera (VLC) and the HARPS spectrographs, both at the 3.6 m telescope, until 2007. Aims. In this paper we present additional radial velocities for 31 stars of the original sample with higher precision. The observations cover a time span of up to 15 years and permit a search for Jupiter analogues. Methods. The survey was carried out with three different instruments/instrument configurations using the iodine absorption cell and the ThAr methods for wavelength calibration. We combine the data sets and perform a joint analysis for variability, trends, and periodicities. We compute Keplerian orbits for companions and detection limits in case of non-detections. Moreover, the HARPS radial velocities are analysed for correlations with activity indicators (CaII H&K and cross-correlation function shape). Results. We achieve a long-term RV precision of 15 m/s (CES+LC, 1992-1998, 9 m/s (CES+VLC, 1999, and 2.8 m/s (HARPS, 2003(HARPS, -2009, including archive data), respectively. This enables us to confirm the known planetary signals in ι Hor and HR 506 as well as the three known planets around HR 3259. A steady RV trend for Ind A can be explained by a planetary companion and calls for direct imaging campaigns. On the other hand, we find previously reported trends to be smaller for β Hyi and not present for α Men. The candidate planet Eri b was not detected despite our better precision. Also the planet announced for HR 4523 cannot be confirmed. Long-term trends in several of our stars are compatible with known stellar companions. We provide a spectroscopic orbital solution for the binary HR 2400 and refined solutions for the planets around HR 506 and ι Hor. For some other stars the variations could be attributed to stellar activity, as e.g. the magnetic cycle in the case of HR 8323. Conclusions. The occurrence of two Jupiter-mass planets in our sample is in line with the estimate of 10% for the frequency of giant planets with periods smaller than 10 yr around solar-like stars. We have not detected a Jupiter analogue, while the detections limits for circular orbits indicate at 5 AU a sensitivity for minimum mass of at least 1M Jup (2M Jup ) for 13% (61%) of the stars.

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“…The observed frequency of debris disks around FGK stars of 16% (Trilling et al 2008) represents a lower limit for the frequency of outer planetesimal disks. Preliminary results from the Herschel DUNES survey (Eiroa et al 2010) suggest that roughly 1/3 of stars have debris disks (C. Eiroa, pers. comm.…”

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confidence: 99%

Debris disks as signposts of terrestrial planet formation

Raymond

Armitage

Moro‐Martín

et al. 2011

A&A

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There exists strong circumstantial evidence from their eccentric orbits that most of the known extra-solar planetary systems are the survivors of violent dynamical instabilities. Here we explore the effect of giant planet instabilities on the formation and survival of terrestrial planets. We numerically simulate the evolution of planetary systems around Sun-like stars that include three components: (i) an inner disk of planetesimals and planetary embryos; (ii) three giant planets at Jupiter-Saturn distances; and (iii) an outer disk of planetesimals comparable to estimates of the primitive Kuiper belt. We calculate the dust production and spectral energy distribution of each system by assuming that each planetesimal particle represents an ensemble of smaller bodies in collisional equilibrium. Our main result is a strong correlation between the evolution of the inner and outer parts of planetary systems, i.e. between the presence of terrestrial planets and debris disks. Strong giant planet instabilities -that produce very eccentric surviving planetsdestroy all rocky material in the system, including fully-formed terrestrial planets if the instabilities occur late, and also destroy the icy planetesimal population. Stable or weakly unstable systems allow terrestrial planets to accrete in their inner regions and significant dust to be produced in their outer regions, detectable at mid-infrared wavelengths as debris disks. Stars older than ∼100 Myr with bright cold dust emission (in particular at λ ∼ 70 μm) signpost dynamically calm environments that were conducive to efficient terrestrial accretion. Such emission is present around ∼16% of billion-year old Solar-type stars. Our simulations yield numerous secondary results: 1) the typical eccentricities of as-yet undetected terrestrial planets are ∼0.1 but there exists a novel class of terrestrial planet system whose single planet undergoes large amplitude oscillations in orbital eccentricity and inclination; 2) by scaling our systems to match the observed semimajor axis distribution of giant exoplanets, we predict that terrestrial exoplanets in the same systems should be a few times more abundant at ∼0.5 AU than giant or terrestrial exoplanets at 1 AU; 3) the Solar System appears to be unusual in terms of its combination of a rich terrestrial planet system and a low dust content. This may be explained by the weak, outward-directed instability that is thought to have caused the late heavy bombardment.Key words. planets and satellites: formation -methods: numerical -planets and satellites: dynamical evolution and stabilitycircumstellar matter -infrared: planetary systems -astrobiology IntroductionCircumstellar disks of gas and dust are expected to produce three broad classes of planets in radially-segregated zones (Kokubo & Ida 2002). The inner disk forms terrestrial (rocky) planets because it contains too little solid mass to rapidly accrete giant planet cores, which are thought to form preferentially beyond the snow line where the surface density in solids is ...

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Cold DUst around NEarby Stars (DUNES). First results

Cited by 64 publications

References 18 publications

AHerschelresolved far-infrared dust ring around HD 207129

AHerschelresolved far-infrared dust ring around HD 207129

The planet search programme at the ESO CES and HARPS

Debris disks as signposts of terrestrial planet formation

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