DOES THE PRESENCE OF PLANETS AFFECT THE FREQUENCY AND PROPERTIES OF EXTRASOLAR KUIPER BELTS? RESULTS FROM THE<i>HERSCHEL</i>DEBRIS AND DUNES SURVEYS

Moro‐Martín, Amaya; Marshall, Jonathan P.; Kennedy, Grant M.; Sibthorpe, B.; Matthews, B. C.; Eiroa, C.; Wyatt, M. C.; Lestrade, J. F.; Maldonado, J.; Rodríguez, David; Greaves, J. S.; Montesinos, B.; Mora, A.; Booth, Mark; Duchêne, Gaspard; Wilner, David J.; Horner, Jonathan

doi:10.1088/0004-637x/801/2/143

Cited by 87 publications

(77 citation statements)

References 85 publications

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“…In fact, additional evidence of the correlation between the presence of dust, low-mass planets, and lower stellar metallicities has been recently found by Marshall et al (2014). However, we caution that there are several biases that might prevent us from finding a clear statistically significant correlation (Moro-Martín et al 2015).…”

Section: Abundance Patterns and The Presence Of Discs And Planetsmentioning

confidence: 68%

“…Further analysis of the Herschel data by Marshall et al (2014) in a sample of 37 solar-type exoplanet hosts reveals a correlation between the presence of dust, low-mass planets, and low stellar metallicities. However, the detailed statistical analysis of 204 FGK stars by Moro-Martín et al (2015) does not find evidence of debris discs being more common around lowmass planet hosts, although the authors caution about possible contamination of the control sample by possible undetected low-mass planets and relatively small sample sizes.…”

Section: Introductionmentioning

confidence: 95%

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Searching for signatures of planet formation in stars with circumstellar debris discs

Maldonado

Eiroa

Villaver

et al. 2015

A&A

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Context. Tentative correlations between the presence of dusty circumstellar debris discs and low-mass planets have recently been presented. In parallel, detailed chemical abundance studies have reported different trends between samples of planet and non-planet hosts. Whether these chemical differences are indeed related to the presence of planets is still strongly debated. Aims. We aim to test whether solar-type stars with debris discs show any chemical peculiarity that could be related to the planet formation process. Methods. We determine in a homogeneous way the metallicity, [Fe/H], and abundances of individual elements of a sample of 251 stars including stars with known debris discs, stars harbouring simultaneously debris discs and planets, stars hosting exclusively planets, and a comparison sample of stars without known discs or planets. High-resolution échelle spectra (R ∼ 57 000) from 2−3 m class telescopes are used. Our methodology includes the calculation of the fundamental stellar parameters (T eff , log g, microturbulent velocity, and metallicity) by applying the iron ionisation and equilibrium conditions to several isolated Fe i and Fe ii lines, as well as individual abundances of C, O, Na, Mg, Al, Si, S, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, Cu, and Zn. Results. No significant differences have been found in metallicity, individual abundances or abundance-condensation temperature trends between stars with debris discs and stars with neither debris nor planets. Stars with debris discs and planets have the same metallicity behaviour as stars hosting planets, and they also show a similar [X/Fe] −T C trend. Different behaviour in the [X/Fe] −T C trends is found between the samples of stars without planets and the samples of planet hosts. In particular, when considering only refractory elements, negative slopes are shown in cool giant planet hosts, whilst positive ones are shown in stars hosting low-mass planets. The statistical significance of the derived slopes is low, however, probably because of the wide range of stellar parameters of our samples. Stars hosting exclusively close-in giant planets behave in a different way, showing higher metallicities and positive [X/Fe] −T C slope. A search for correlations between the [X/Fe] −T C slopes and the stellar properties reveals a moderate but significant correlation with the stellar radius and a weak correlation with the stellar age, which remain even if Galactic chemical evolution effects are considered. No correlation between the [X/Fe] −T C slopes and the disc/planet properties are found. Conclusions. The fact that stars with debris discs and stars with low-mass planets do not show either metal enhancement or a different [X/Fe] −T C trend might indicate a correlation between the presence of debris discs and the presence of low-mass planets. We extend results from previous works based mainly on solar analogues with reported differences in the [X/Fe] −T C trends between planet hosts and non-hosts to a wider range of parameters. However, these differences ...

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Section: Abundance Patterns and The Presence Of Discs And Planetsmentioning

confidence: 68%

Section: Introductionmentioning

confidence: 95%

Searching for signatures of planet formation in stars with circumstellar debris discs

Maldonado

Eiroa

Villaver

et al. 2015

A&A

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“…Bryden et al (2009) found little correlation between planet hosts and detection of an IR excess (the typical age of stars in their sample was ∼6 Gyr, whereas the stars in our sample are significantly younger). More recently, Moro-Martín et al (2015) examined a large (>200 star) sample of Herschel-observed stars to look for correlations between the presence of a debris disk and: (1) the presence of low-mass planets, (2) the presence of high-mass planets, (3) metallicity, and (3) the presence of one or more stellar companions. Even with their large sample size, Moro-Martín et al (2015) found no significant correlations between any of the aforementioned parameters.…”

Section: Planet Stirringmentioning

confidence: 99%

Herschel Observations of Dusty Debris Disks

Vican

Schneider

Bryden

et al. 2016

ApJ

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We present results from two Herschel observing programs using the Photodetector Array Camera and Spectrometer. During three separate campaigns, we obtained Herschel data for 24 stars at 70, 100, and 160 µm. We chose stars that were already known or suspected to have circumstellar dust based on excess infrared emission previously measured with IRAS or Spitzer, and used Herschel to examine long-wavelength properties of the dust. Fifteen stars were found to be uncontaminated by background sources, and possess infrared emission most likely due to a circumstellar debris disk. We analyzed the properties of these debris disks to better understand the physical mechanisms responsible for dust production and removal. Seven targets were spatially resolved in the Herschel images. Based on fits to their spectral energy distributions, nine disks appear to have two temperature components. Of these nine, in three cases, the warmer dust component is likely the result of a transient process rather than a steady state collisional cascade. The dust belts at four stars are likely stirred by an unseen planet, and merit further investigation.

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“…If the composition of the star reflects the composition of the planet-forming disk, one explanation could be that the dust grains that eventually build up the planetesimals are more easily formed in an environment enriched in heavier elements. The picture is far from clear, however, since a correlation with host star metallicity is observed for gas giants, but not for small exoplanets (Buchhave et al 2014) or for the tracers of planetesimal formation known as debris disks (Greaves et al 2006;Wyatt et al 2007;Moro-Martín et al 2015).…”

Section: Introductionmentioning

confidence: 97%

Herscheldetects oxygen in theβPictoris debris disk

Brandeker

Cataldi

Olofsson

et al. 2016

A&A

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The young star β Pictoris is well known for its dusty debris disk produced through collisional grinding of planetesimals, kilometre-sized bodies in orbit around the star. In addition to dust, small amounts of gas are also known to orbit the star; this gas is likely the result of vaporisation of violently colliding dust grains. The disk is seen edge on and from previous absorption spectroscopy we know that the gas is very rich in carbon relative to other elements. The oxygen content has been more difficult to assess, however, with early estimates finding very little oxygen in the gas at a C/O ratio that is 20× higher than the cosmic value. A C/O ratio that high is difficult to explain and would have far-reaching consequences for planet formation. Here we report on observations by the far-infrared space telescope Herschel, using PACS, of emission lines from ionised carbon and neutral oxygen. The detected emission from C + is consistent with that previously reported observed by the HIFI instrument on Herschel, while the emission from O is hard to explain without assuming a higher density region in the disk, perhaps in the shape of a clump or a dense torus required to sufficiently excite the O atoms. A possible scenario is that the C/O gas is produced by the same process responsible for the CO clump recently observed by the Atacama Large Millimeter/submillimeter Array in the disk and that the redistribution of the gas takes longer than previously assumed. A more detailed estimate of the C/O ratio and the mass of O will have to await better constraints on the C/O gas spatial distribution.

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DOES THE PRESENCE OF PLANETS AFFECT THE FREQUENCY AND PROPERTIES OF EXTRASOLAR KUIPER BELTS? RESULTS FROM THEHERSCHELDEBRIS AND DUNES SURVEYS

Cited by 87 publications

References 85 publications

Searching for signatures of planet formation in stars with circumstellar debris discs

Searching for signatures of planet formation in stars with circumstellar debris discs

Herschel Observations of Dusty Debris Disks

Herscheldetects oxygen in theβPictoris debris disk

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