Warm debris disks candidates in transiting planets systems

Ribas, Álvaro; Merın, Bruno; Ardila, D. R.; Bouy, H.

doi:10.1051/0004-6361/201118306

Cited by 24 publications

(32 citation statements)

References 28 publications

(60 reference statements)

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“…Its planet is slightly hotter ( K) than HD 209458 b so it is on the border of the pL and pM classes. Krivov et al (2011) found a flux excess at 12 and 22 m indicative of the presence of dust rings at a distance of several astronomical units from the parent star, but this has been disputed by Ribas et al (2012). In this work we present the first follow‐up transit photometry of HAT‐P‐5 obtained since the discovery paper, covering four optical passbands.…”

Section: Introductionmentioning

confidence: 94%

Physical properties and radius variations in the HAT-P-5 planetary system from simultaneous four-colour photometry

Southworth¹,

Mancini²,

Maxted³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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The radii of giant planets, as measured from transit observations, may vary with wavelength due to Rayleigh scattering or variations in opacity. Such an effect is predicted to be large enough to detect using ground‐based observations at multiple wavelengths. We present the defocused photometry of a transit in the HAT‐P‐5 system, obtained simultaneously through Strömgren u, Gunn g and r, and Johnson I filters. Two more transit events were observed through a Gunn r filter. We detect a substantially larger planetary radius in u, but the effect is greater than predicted using theoretical model atmospheres of gaseous planets. This phenomenon is most likely to be due to systematic errors present in the u‐band photometry, stemming from variations in the transparency of Earth’s atmosphere at these short wavelengths. We use our data to calculate an improved orbital ephemeris and to refine the measured physical properties of the system. The planet HAT‐P‐5 b has a mass of and a radius of (statistical and systematic errors, respectively), making it slightly larger than expected according to standard models of coreless gas‐giant planets. Its equilibrium temperature of 1517 ± 29 K is within 60 K of that of the extensively studied planet HD 209458 b.

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Section: Introductionmentioning

confidence: 94%

Physical properties and radius variations in the HAT-P-5 planetary system from simultaneous four-colour photometry

Southworth¹,

Mancini²,

Maxted³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…Many other studies also conclude that warm excesses from debris disks around solar-type stars are extremely rare (e.g., Moór et al 2009;Stauffer et al 2010;Beichman et al 2011;Smith et al 2011;Zuckerman et al 2011;Ribas et al 2012;Urban et al 2012;Zuckerman et al 2012;Jackson & Wyatt 2012;Kennedy & Wyatt 2012;Ballering et al 2013;Vican & Schneider 2014). Although IRAS, Spitzer, and Herschel data suggest 10% to 30% of solartype main sequence stars have IR excesses (e.g., Lagrange et al 2000;Eiroa et al 2013;Ballering et al 2013, and references therein), nearly all sources have color temperatures characteristic of cold dust (T d 300 K) at a 1 AU.…”

Section: Warm Excesses From Debris Disks Are Rarementioning

confidence: 99%

Rocky Planet Formation: Quick and Neat

Kenyon

Najita

Bromley

2016

ApJ

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We reconsider the commonly held assumption that warm debris disks are tracers of terrestrial planet formation. The high occurrence rate inferred for Earthmass planets around mature solar-type stars based on exoplanet surveys (∼ 20%) stands in stark contrast to the low incidence rate (≤ 2%-3%) of warm dusty debris around solar-type stars during the expected epoch of terrestrial planet assembly (∼ 10 Myr). If Earth-mass planets at AU distances are a common outcome of the planet formation process, this discrepancy suggests that rocky planet formation occurs more quickly and/or is much neater than traditionally believed, leaving behind little in the way of a dust signature. Alternatively, the incidence rate of terrestrial planets has been overestimated or some previously unrecognized physical mechanism removes warm dust efficiently from the terrestrial planet region. A promising removal mechanism is gas drag in a residual gaseous disk with a surface density 10 −5 of the minimum mass solar nebula.

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“…The errors in the photospheric theoretical fluxes corresponding to the fit performed using VOSA are considered insignificant and were not used (Ribas et al 2012). The distribution histograms of χ λ values for the four WISE bands are shown in Fig.…”

Section: Introductionmentioning

confidence: 99%

On the Incidence of Wise Infrared Excess Among Solar Analog, Twin, and Sibling Stars

Costa

Martins

Leão

et al. 2017

ApJ

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This study presents a search for IR excess in the 3.4, 4.6, 12 and 22 µm bands in a sample of 216 targets, composed of solar sibling, twin and analog stars observed by the WISE mission. In general, an infrared excess suggests the existence of warm dust around a star. We detected 12 µm and/or 22 µm excesses at the 3σ level of confidence in five solar analog stars, corresponding to a frequency of 4.1 % of the entire sample of solar analogs analyzed, and in one out of 29 solar sibling candidates, confirming previous studies. The estimation of the dust properties shows that the sources with infrared excesses possess circumstellar material with temperatures that, within the uncertainties, are similar to that of the material found in the asteroid belt in our solar system. No photospheric flux excess was identified at the W1 (3.4 µm) and W2 (4.6 µm) WISE bands, indicating that, in the majority of stars of the present sample, no detectable dust is generated. Interestingly, among the sixty solar twin stars analyzed in this work, no WISE photospheric flux excess was detected. However, a null-detection excess does not necessarily indicate the absence of dust around a star because different causes, including dynamic processes and instrument limitations, can mask its presence.

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Warm debris disks candidates in transiting planets systems

Cited by 24 publications

References 28 publications

Physical properties and radius variations in the HAT-P-5 planetary system from simultaneous four-colour photometry

Physical properties and radius variations in the HAT-P-5 planetary system from simultaneous four-colour photometry

Rocky Planet Formation: Quick and Neat

On the Incidence of Wise Infrared Excess Among Solar Analog, Twin, and Sibling Stars

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