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

Kennedy, Grant M.; Ginski, C.; Kenworthy, Matthew A.; Benisty, M.; Henning, Thomas; Holstein, R. van; Kral, Quentin; Ménard, F.; Milli, J.; Quiroga-Nuñez, Luis Henry; Rab, Ch.; Stolker, T.; Sturm, J. A.

doi:10.1093/mnrasl/slaa092

Cited by 8 publications

(7 citation statements)

References 46 publications

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“…This wide companion is classified as a white dwarf candidate with a mass of 0.48-0.58 M ⊙ (depending on whether a pure-He or pure-H atmosphere is supposed, Gentile Fusillo et al 2019). Recently, Kennedy et al (2020) reported the discovery of a low mass companion of RZ Psc at a projected separation of 23 au. The other three stars, HD 15407, HD 23514, and V488 Per, are all reported to have wide-orbit companions, the projected separations are ρ p = 1050, 365, and 12300 au, respectively (Melis et al 2010;Rodriguez et al 2012;Zuckerman 2015).…”

Section: Wide Separation Companionsmentioning

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: Wide Separation Companionsmentioning

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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“…The latter authors first suggested that RZ Psc is surrounded by circumstellar disk with the central cavity free (or almost free) of matter. This assumption was confirmed by de Wit et al (2013): a bright mid-IR excess was found in WISE observations of RZ Psc, fitted by black-body radiation with temperature ≈ 500 K. They assumed that the star is surrounded by the dusty ring with inner radius 0.4-0.7 AU and this assumption was recently confirmed by Kennedy et al (2020). They discovered that RZ Psc hosts a 0.12 M companion at a projected separation of 23 AU.…”

Section: Introductionmentioning

confidence: 74%

Magnetospheric accretion at the late phases of the Pre-Main-Sequence evolution. The case of RZ Psc

Dmitriev¹,

Grinin²,

Potravnov³

et al. 2023

Preprint

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It has been shown that during theburst of accretion activity observed in UX Ori type star RZ Psc in 2013, the accretion rate increased approximately by an order of magnitude. This means that the accretion process at the late stages of the Pre-Main Sequence evolution is very unstable. Using the spectra obtained during this episode we have studied the magnetospheric emission in the H𝛼 line. Models of magnetospheric accretion are calculated to obtain the parameters of the magnetosphere from this observation. In present work we have taken into account the influence of the recombination delay effect during gas motion in the stellar magnetosphere. The accounting for this effect and the presence of the magnetospheric absorption in the IR CaII triplet lines and its absence in D Na I resonance lines allowed us to place a lower limit on the temperature in the magnetosphere at ≈ 10000 K, which significantly improved precision of our estimate of accretion rate. According to the best fit model the logarithm of accretion rate is log 𝑀 = −10.1 ± 0.3 ( 𝑀 ≈ 7 × 10 −11 M yr −1 ) and the inclination angle of RZ Psc is 43 ± 3 • . It is less than the inclination, typical for the UX Ori stars (about 70 • ), that explains the weak photometric variability of this star. Using the obtained accretion rate and magnetosphere radius we estimate the strength of the dipole component of the magnetic field of RZ Psc ≈ 0.1 kGs.

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“…There is no sign of cold dust (debris outside tens of astronomical units), although its presence cannot be ruled out due to the lack of far-infrared/millimeter observations. High-contrast, ground-based imaging recently obtained with VLT/SPHERE shows that RZ Psc hosts a 0.12 M ☉ companion at a projected separation of 22 au and concludes that the disk (the source of the infrared excess) orbits the primary star (Kennedy et al 2020). The low-mass component is expected to have a significant impact on the disk itself, such as truncating the disk outer edge and heavily stirring the remaining planetesimals.…”

Section: Introductionmentioning

confidence: 96%

RZ Piscium Hosts a Compact and Highly Perturbed Debris Disk

Su,

Kennedy,

Rieke

et al. 2023

ApJ

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RZ Piscium (RZ Psc) is well known in the variable star field because of its numerous irregular optical dips in the past 5 decades, but the nature of the system is heavily debated in the literature. We present multiyear infrared monitoring data from Spitzer and WISE to track the activities of the inner debris production, revealing stochastic infrared variability as short as weekly timescales that is consistent with destroying a 90 km sized asteroid every year. ALMA 1.3 mm data combined with spectral energy distribution modeling show that the disk is compact (∼0.1–13 au radially) and lacks cold gas. The disk is found to be highly inclined and has a significant vertical scale height. These observations confirm that RZ Psc hosts a close to edge-on, highly perturbed debris disk possibly due to migration of recently formed giant planets that might be triggered by the low-mass companion RZ Psc B if the planets formed well beyond the snowlines.

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

Cited by 8 publications

References 46 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

Magnetospheric accretion at the late phases of the Pre-Main-Sequence evolution. The case of RZ Psc

RZ Piscium Hosts a Compact and Highly Perturbed Debris Disk

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