<i>WISE</i>DETECTIONS OF DUST IN THE HABITABLE ZONES OF PLANET-BEARING STARS

Morales, Farisa Y.; Padgett, Deborah; Bryden, G.; Werner, M. W.; Furlan, Elise

doi:10.1088/0004-637x/757/1/7

Cited by 49 publications

(31 citation statements)

References 40 publications

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“…At a 3σ sensitivity level of about 1000 times the level of the zodiacal emission in the short IRS wavelength band (8.5-12 µm), the authors found a success rate for excesses of about 1%. This occurrence rate, recently confirmed by WISE mid-infrared photometry (Morales et al 2012;Padgett et al 2013), is in stark contrast to the present study, and points again to a non-solar system morphology for the exozodiacal discs detected at K band.…”

Section: Sensitivity Of Fluor and Comparison With Other Studiescontrasting

confidence: 52%

A near-infrared interferometric survey of debris-disc stars

Absil

Defrère

Foresto

et al. 2013

A&A

111

197

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Context. Dust is expected to be ubiquitous in extrasolar planetary systems owing to the dynamical activity of minor bodies. Inner dust populations are, however, still poorly known because of the high contrast and small angular separation with respect to their host star, and yet, a proper characterisation of exozodiacal dust is mandatory for the design of future Earth-like planet imaging missions. Aims. We aim to determine the level of near-infrared exozodiacal dust emission around a sample of 42 nearby main sequence stars with spectral types ranging from A to K and to investigate its correlation with various stellar parameters and with the presence of cold dust belts. Methods. We use high-precision K-band visibilities obtained with the FLUOR interferometer on the shortest baseline of the CHARA array. The calibrated visibilities are compared with the expected visibility of the stellar photosphere to assess whether there is an additional, fully resolved circumstellar emission source. Results. Near-infrared circumstellar emission amounting to about 1% of the stellar flux is detected around 13 of our 42 target stars. Follow-up observations showed that one of them (eps Cep) is associated with a stellar companion, while another one was detected around what turned out to be a giant star (kap CrB). The remaining 11 excesses found around single main sequence stars are most probably associated with hot circumstellar dust, yielding an overall occurrence rate of 28 +8 −6 % for our (biased) sample. We show that the occurrence rate of bright exozodiacal discs correlates with spectral type, K-band excesses being more frequent around A-type stars. It also correlates with the presence of detectable far-infrared excess emission in the case of solar-type stars. Conclusions. This study provides new insight into the phenomenon of bright exozodiacal discs, showing that hot dust populations are probably linked to outer dust reservoirs in the case of solar-type stars. For A-type stars, no clear conclusion can be made regarding the origin of the detected near-infrared excesses.

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Section: Sensitivity Of Fluor and Comparison With Other Studiescontrasting

confidence: 52%

A near-infrared interferometric survey of debris-disc stars

Absil

Defrère

Foresto

et al. 2013

A&A

111

197

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“…Photometric monitoring indicated that it has an inclination of  27 and a rotation period of 8.45 days (Broeg et al 2007). It is one of the most studied CTTSs due to many features indicative of active accretion onto the star from a circumstellar disk, such as brightness variations (e.g., Friedrich & Schöffel 1971;Appenzeller et al 1978;Broeg et al 2007;Donati et al 2012), inverse P-Cygni profiles (e.g., Appenzeller et al 1978;Bertout et al 1982;Batalha et al 2001), optical veiling (e.g., Batalha et al 2001;Seperuelo Duarte et al 2008), very intense magnetic field (e.g., Donati et al 2012;JohnsKrull et al 2013), and strong excess from near-to far-infrared (e.g., Mendoza 1968;Hughes et al 1994;Kessler-Silacci et al 2006;McClure et al 2012;Morales et al 2012). The accretion disk was first imaged at 1.3 mm dust continuum emission by Dai et al (2010) using the Submillimeter Array.…”

Section: Gq Lup a And Bmentioning

confidence: 99%

An ALMA and MagAO Study of the Substellar Companion GQ Lup B^∗

Sheehan

Males

et al. 2017

ApJ

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Multi-wavelength observations provide a complementary view of the formation of young, directly imaged planetmass companions. We report the ALMA 1.3 mm and Magellan adaptive optics Hα, ¢ i , ¢ z , and Y S observations of the GQ Lup system, a classical T Tauri star with a -M 10 40 Jup substellar companion at ∼110 au projected separation. We estimate the accretion rates for both components from the observed Hα fluxes. In our ∼0 05 resolution ALMA map, we resolve GQ Lup A's disk in thedust continuum, but no signal is found from the companion. The disk is compact, with a radius of ∼22 au, a dust mass of ∼6 M ⊕ , an inclination angle of ∼56°, and a very flat surface density profile indicative of a radial variation in dust grain sizes. No gaps or inner cavity are found in the disk, so there is unlikely a massive inner companion to scatter GQ Lup B outward. Thus, GQ Lup B might have formed in situ via disk fragmentation or prestellar core collapse. We also show that GQ Lup A's disk is misaligned with its spin axis, and possibly with GQ Lup B's orbit. Our analysis on the tidal truncation radius of GQ Lup A's disk suggests that GQ Lup B's orbit might have a low eccentricity.

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“…Among these stars, a few dozen are also known to harbor planets (Lawler and Gladman 2012;Morales et al 2012;Bonsor et al 2013). …”

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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WISEDETECTIONS OF DUST IN THE HABITABLE ZONES OF PLANET-BEARING STARS

Cited by 49 publications

References 40 publications

A near-infrared interferometric survey of debris-disc stars

A near-infrared interferometric survey of debris-disc stars

An ALMA and MagAO Study of the Substellar Companion GQ Lup B^∗

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

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WISEDETECTIONS OF DUST IN THE HABITABLE ZONES OF PLANET-BEARING STARS

Cited by 49 publications

References 40 publications

A near-infrared interferometric survey of debris-disc stars

A near-infrared interferometric survey of debris-disc stars

An ALMA and MagAO Study of the Substellar Companion GQ Lup B∗

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

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An ALMA and MagAO Study of the Substellar Companion GQ Lup B^∗