Searching for the Young Kinematic Group Associated with HD 166191

Potravnov, I. S.; Еселевич, Максим; Kondratieva, T. E.; Sokolov, I. V.

doi:10.1134/s1063773718100079

Cited by 6 publications

(6 citation statements)

References 62 publications

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“…The quoted data show the disk parameters measured before 2009.bKennedy & Wyatt (2014) found that HD 166191 is comoving with the well known Herbig Ae star, HD 163296. Later,Potravnov et al (2018) identified some additional young stars showing similar kinematics and located close to HD 166191 and they argued that all these objects belong to a ∼10 Myr old kinematic group.…”

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confidence: 99%

A New Sample of Warm Extreme Debris Disks from the ALLWISE Catalog

Moór

Ábrahám

Szabó

et al. 2021

ApJ

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Extreme debris disks (EDDs) are rare systems with peculiarly large amounts of warm dust that may stem from recent giant impacts between planetary embryos during the final phases of terrestrial planet growth. Here we report on the identification and characterization of six new EDDs. These disks surround F5-G9 type main-sequence stars with ages >100 Myr, have dust temperatures higher than 300 K and fractional luminosities between 0.01 and 0.07. Using time-domain photometric data at 3.4 and 4.6 µm from the WISE all sky surveys, we conclude that four of these disks exhibited variable mid-infrared emission between 2010 and 2019. Analyzing the sample of all known EDDs, now expanded to 17 objects, we find that 14 of them showed changes at 3-5 µm over the past decade suggesting that mid-infrared variability is an inherent characteristic of EDDs. We also report that wide-orbit pairs are significantly more common in EDD systems than in the normal stellar population. While current models of rocky planet formation predict that the majority of giant collisions occur in the first 100 Myr, we find that the sample of EDDs is dominated by systems older than this age. This raises the possibility that the era of giant impacts may be longer than we think, or that some other mechanism(s) can also produce EDDs. We examine a scenario where the observed warm dust stems from the disruption and/or collisions of comets delivered from an outer reservoir into the inner regions, and explore what role the wide companions could play in this process.

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confidence: 99%

A New Sample of Warm Extreme Debris Disks from the ALLWISE Catalog

Moór

Ábrahám

Szabó

et al. 2021

ApJ

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“…This reference identified a group of five other stars that share similar kinematics and youth indicators (∼10 Myr) to HD 166191 and suggested they belong to the extended Corona Australis Association (Neuhäuser & Forbrich 2008). The radial velocities (−8.1 ± 1.3 km s −1 from Schneider et al (2013), −10.1 ± 1 km s −1 from Kennedy et al (2014), and −7.4 ± 2 km s −1 from Potravnov et al (2018)) indicate no close companion, and there is no in-dication of binarity on the sky. Potravnov et al (2018) estimate a rotation velocity vsini = 27±1 km s −1 .…”

Section: System Propertiesmentioning

confidence: 95%

“…The radial velocities (−8.1 ± 1.3 km s −1 from Schneider et al (2013), −10.1 ± 1 km s −1 from Kennedy et al (2014), and −7.4 ± 2 km s −1 from Potravnov et al (2018)) indicate no close companion, and there is no in-dication of binarity on the sky. Potravnov et al (2018) estimate a rotation velocity vsini = 27±1 km s −1 . Given that typical F5 main-sequence stars have rotation velocities of ∼30 km s −1 , the stellar rotation axis is then roughly perpendicular to the line of sight.…”

Section: System Propertiesmentioning

confidence: 95%

“…The properties of the central star in the HD 166191 system are reasonably well constrained. A number of high-resolution optical spectra (Schneider et al 2013;Kennedy et al 2014;Potravnov et al 2018) together indicate an effective temperature of 6000 K or slightly higher. The lack of optical and near infrared emission lines and optical spectroscopic variability suggest no active gas accretion onto the star.…”

Section: System Propertiesmentioning

confidence: 99%

“…The lack of optical and near infrared emission lines and optical spectroscopic variability suggest no active gas accretion onto the star. The age of the star has been muddled by its apparent association with the ∼5 Myr-old Herbig Ae star HD 163296, but the situation has been clarified by Potravnov et al (2018). This reference identified a group of five other stars that share similar kinematics and youth indicators (∼10 Myr) to HD 166191 and suggested they belong to the extended Corona Australis Association (Neuhäuser & Forbrich 2008).…”

Section: System Propertiesmentioning

confidence: 99%

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A Star-sized Impact-Produced Dust Clump in the Terrestrial Zone of the HD 166191 System

Su,

Kennedy,

Schlawin

et al. 2022

Preprint

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We report on five years of 3-5 µm photometry measurements obtained by warm Spitzer to track the dust debris emission in the terrestrial zone of HD 166191 in combination with simultaneous optical data. We show that the debris production in this young (∼10 Myr) system increased significantly in early 2018 and reached a record high level (almost double by mid 2019) by the end of the Spitzer mission (early 2020), suggesting intense collisional activity in its terrestrial zone likely due to either initial assembling of terrestrial planets through giant impacts or dynamical shake-up from unseen planet-mass objects or recent planet migration. This intense activity is further highlighted by detecting a star-size dust clump, passing in front of the star, in the midst of its infrared brightening. We constrain the minimum size and mass of the clump using multiwavelength transit profiles and conclude that the dust clump is most likely created by a large impact involving objects of several hundred kilometers in size with an apparent period of 142 days (i.e., 0.62 au assuming a circular orbit). The system's evolutionary state (right after the dispersal of its gas-rich disk) makes it extremely valuable to learn about the process of terrestrial-planet formation and planetary architecture through future observations.

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