Accretion and outflow activity on the late phases of pre-main-sequence evolution

Potravnov, I. S.; Mkrtichian, D. E.; Гринин, В. П.; Ilyin, I.; Shakhovskoy, D. N.

doi:10.1051/0004-6361/201628926

Cited by 12 publications

(11 citation statements)

References 31 publications

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“…The low-velocity BACs are formed closer to the star, and the rapid changes on the timescale of ∼ 3 h reflect the non-stationary processes at the initial stages of the wind acceleration. The long-lived (up to several days, as was shown in Potravnov et al 2017) BAC at −110 km s −1 in contrast forms at distances of a few dozen stellar radii. This explains its absence in the November 16 spectrum at Ca ii 8542 Å lines due to the higher excitation potential of Ca ii in comparison with Na i D.…”

Section: Summary On the Circumstellar Lines In The Rz Psc Spectrasupporting

confidence: 53%

“…We adhere to the explanation that the RZ Psc disc still contains the depleted amount of the primordial gas, which is recycled by the propeller mechanism to the outflow observed in the low-excitation lines of the alkali metals (Grinin et al 2015;Potravnov et al 2017). The very weak residual emission at Hα led us to suspect the existence of accretion in the system and to estimate its upper limit as Ṁ ∼ 7 • 10 −12 M ⊙ yr −1 (Potravnov et al 2017). Unambiguous detection of the accreting material is essential to support our scenario because this gas should also be the raw material for the propeller mechanism.…”

Section: Introductionmentioning

confidence: 77%

“…Despite its age, RZ Psc demonstrates the spectroscopic footprints of circumstellar activity . The circumstellar gas is manifested in the RZ Psc spectra predominantly in the form of discrete BACs, which are observed in the lines of alkali metals Na i D, K i 7699 Å and lines of the Ca ii IR triplet (Potravnov et al 2017). Such spectroscopic variability could resemble what has been observed in a non-accreting star with a debris disc β Pic (Lagrange et al 1996, and references therein).…”

Section: Introductionmentioning

confidence: 88%

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

Potravnov

Гринин

Serebriakova

2019

A&A

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We discuss a revision of accretion activity and kinematics of the enigmatic isolated UX Ori type star RZ Psc. Previously, RZ Psc was known to possess only spectroscopic signatures of outflow in the low-excitation lines of alkali metals. The archival high-resolution spectra reveal a short-lived episode of magnetospheric accretion in the system observed via inverse P Cyg profiles at the Hα and Ca ii 8542 Å lines. The simultaneous presence of accretion and outflow signatures at Ca ii 8542 Å is suggestive of an accretion-driven origin of the RZ Psc wind. We argue that RZ Psc experiences matter ejection via the magnetic propeller mechanism but variable accretion episodes allow it to sometimes move in the magnetospheric accretion regime. The presence of the weak accretion in the system is also supported by the radiation of the hot accretion spot on the stellar surface observed spectroscopically at the deep photometric minimum of the star. The Galactic motion of RZ Psc calculated with new GAIA DR2 astrometric data suggests possible membership in Cas-Tau OB association with an age of t = 20 +3 −5 Myr.

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Section: Summary On the Circumstellar Lines In The Rz Psc Spectrasupporting

confidence: 53%

Section: Introductionmentioning

confidence: 77%

Section: Introductionmentioning

confidence: 88%

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

Potravnov

Гринин

Serebriakova

2019

A&A

Self Cite

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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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“…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: 63%

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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Accretion and outflow activity on the late phases of pre-main-sequence evolution

Cited by 12 publications

References 31 publications

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

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

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

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

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