Flares of accretion activity of the 20 Myr old UXOR RZ Psc

Potravnov, I. S.; Гринин, В. П.; Serebriakova, N. A.

doi:10.1051/0004-6361/201935492

Cited by 11 publications

(11 citation statements)

References 67 publications

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“…The nature of two of these additional disks is still debated. RZ Psc was found to exhibit a weak accretion signature, suggesting that the disk may be of primordial nature rather than EDD (Potravnov et al 2017(Potravnov et al , 2019. Concerning HD 166191, Kennedy & Wyatt (2014) raised the possibility that it is not a secondary disk but a primordial transition disk.…”

Section: The Nature Of the Edd Phenomenonmentioning

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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Section: The Nature Of the Edd Phenomenonmentioning

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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“…Grady et al 1996). Recent work finds that RZ Psc shows a weak Hα accretion signature, which is more consistent with a long-lived protoplanetary disc scenario (Potravnov et al 2017(Potravnov et al , 2019.…”

Section: Introductionmentioning

confidence: 60%

“…Bohn et al 2020). If we assume an age of 20 Myr for RZ Psc (Potravnov et al 2019), then using the BT-Settl isochrones (Allard et al 2012) we find a companion mass of 0.12±0.01 M for the H-band and 0.11±0.02 M for the K s -band. The systematic uncertainty in the mass due to an uncertain age is of course larger (on the order of 0.05 M if the age changes by 10 Myr).…”

Section: Discussionmentioning

confidence: 98%

A low-mass stellar companion to the young variable star RZ Psc

Kennedy

Ginski

Kenworthy

et al. 2020

Monthly Notices of the Royal Astronomical Society: Letters

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RZ Psc is a young Sun-like star with a bright and warm infrared excess that is occasionally dimmed significantly by circumstellar dust structures. Optical depth arguments suggest that the dimming events do not probe a typical sightline through the circumstellar dust, and are instead caused by structures that appear above an optically thick mid-plane. This system may therefore be similar to systems where an outer disc is shadowed by material closer to the star. Here, we report the discovery that RZ Psc hosts a $0.12\, \mathrm{ M}_\odot$ companion at a projected separation of 23 au. We conclude that the disc must orbit the primary star. While we do not detect orbital motion, comparison of the angle of linear polarization of the primary with the companion’s on-sky position angle provides circumstantial evidence that the companion and disc may not share the same orbital plane. Whether the companion severely disrupts the disc, truncates it, or has little effect at all will require further observations of both the companion and disc.

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Section: Discussionmentioning

confidence: 93%

A low-mass stellar companion to the young variable star RZ Psc

Kennedy,

Ginski,

Kenworthy

et al. 2020

Preprint

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RZ Psc is a young Sun-like star with a bright and warm infrared excess that is occasionally dimmed significantly by circumstellar dust structures. Optical depth arguments suggest that the dimming events do not probe a typical sight line through the circumstellar dust, and are instead caused by structures that appear above an optically thick mid-plane. This system may therefore be similar to systems where an outer disk is shadowed by material closer to the star. Here we report the discovery that RZ Psc hosts a 0.12 M companion at a projected separation of 23 au. We conclude that the disk must orbit the primary star. While we do not detect orbital motion, comparison of the angle of linear polarization of the primary with the companion's on-sky position angle provides circumstantial evidence that the companion and disc may not share the same orbital plane. Whether the companion severely disrupts the disc, truncates it, or has little effect at all, will require further observations of both the companion and disc.

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Flares of accretion activity of the 20 Myr old UXOR RZ Psc

Cited by 11 publications

References 67 publications

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

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

A low-mass stellar companion to the young variable star RZ Psc

A low-mass stellar companion to the young variable star RZ Psc

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