Active asteroid belt causes the UXOR phenomenon in RZ Piscium

Wit, W. J. de; Гринин, В. П.; Potravnov, I. S.; Shakhovskoi, D. N.; Müller, André; Moerchen, Margaret M.

doi:10.1051/0004-6361/201220715

Cited by 28 publications

(43 citation statements)

References 35 publications

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“…It is evident that the star's flux remained constant in all four passbands during the observations. Based on V -band magnitude obtained with the OM we further conclude that, during our XMM observations, RZ Psc was not undergoing one of its rare, deep visual minima, which can be as dim as V ∼ 14 (de Wit et al 2013). Adopting the mean V -band magnitude obtained from the OM photometry and assuming bolometric corrections based on the adopted effective temperature and luminosity class of RZ Psc (see Section 3.2), we obtain F bol values that range from ∼ 6.7 × 10 −10 to ∼ 6.9 × 10 −10 erg s −1 cm −2 .…”

Section: Xmm-newton Optical Monitor Datasupporting

confidence: 60%

Is the Young Star RZ Piscium Consuming Its Own (Planetary) Offspring?

Punzi

Kastner

Melis

et al. 2017

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The erratically variable star RZ Piscium (RZ Psc) displays extreme optical dropout events and strikingly large excess infrared emission. To ascertain the evolutionary status of this intriguing star, we obtained observations of RZ Psc with the European Space Agency's X-ray Multi-Mirror Mission (XMM-Newton), as well as high-resolution optical spectroscopy with the Hamilton Echelle on the Lick Shane 3 m telescope and with HIRES on the Keck I 10 m telescope. The optical spectroscopy data demonstrate that RZ Psc is a pre-main sequence star with an effective temperature of 5600 ± 75 K and log g of 4.35 ± 0.10. The ratio of X-ray to bolometric luminosity, log L X /L bol , lies in the range −3.7 to −3.2, consistent with ratios typical of young, solar-mass stars, thereby providing strong support for the young-star status of RZ Psc. The Li absorption line strength of RZ Psc suggests an age in the range 30-50 Myr, which in turn implies RZ Psc lies at a distance of ∼170 pc. Adopting this estimated distance, we find the Galactic space velocity of RZ Psc to be similar to the space velocities of stars in young moving groups near the Sun. Optical spectral features indicative of activity and/or circumstellar material are present in our spectra over multiple epochs, which provide evidence for the presence of a significant mass of circumstellar gas associated with RZ Psc. We suggest that the destruction of one or more massive orbiting bodies has recently occurred within 1 au of the star, and we are viewing the aftermath of such an event along the plane of the orbiting debris. star expanded to become a red giant. Melis (2009) chose to call such dusty, first ascent giant stars "Phoenix Giants" because of their similarities to T Tauri stars (specifically, high Li abundance and strong infrared excess; Potravnov et al. 2014b). Furthermore, the strong IR excess associated with RZ Psc (L IR /L bol ∼ 8%, de Wit et al. 2013) would be very peculiar if the star is as old as ∼25 Myr.

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Section: Xmm-newton Optical Monitor Datasupporting

confidence: 60%

Is the Young Star RZ Piscium Consuming Its Own (Planetary) Offspring?

Punzi

Kastner

Melis

et al. 2017

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“…There are many ways to deposit new dust into an inner planetary system, such as collisions in a dense, active asteroid belt (de Wit et al 2013), breakups of "super" comets (Beichman et al 2005), and volcanic activities from a newly formed molten planet. Our proposed impact scenario for both ID8 and P1121 is related to dense, inner planetesimal belts, the first hypothesis.…”

Section: Radiation Pressure and Stellar Windmentioning

confidence: 99%

Extreme Debris Disk Variability: Exploring the Diverse Outcomes of Large Asteroid Impacts During the Era of Terrestrial Planet Formation

Jackson

Gáspár

et al. 2019

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The most dramatic phases of terrestrial planet formation are thought to be oligarchic and chaotic growth, on timescales of up to 100-200 Myr, when violent impacts occur between large planetesimals of sizes up to protoplanets. Such events are marked by the production of large amounts of debris, as has been observed in some exceptionally bright and young debris disks (termed extreme debris disks). Here we report five years of Spitzer measurements of such systems around two young solar-type stars: ID8 and P1121. The short-term (weekly to monthly) and long-term (yearly) disk variability is consistent with the aftermaths of large impacts involving large asteroid-sized bodies. We demonstrate that an impact-produced clump of optically thick dust, under the influence of the dynamical and viewing geometry effects, can produce short-term modulation in the disk light curves. The long-term disk flux variation is related to the collisional evolution within the impact-produced fragments once released into a circumstellar orbit. The time-variable behavior observed in the P1121 system is consistent with a hypervelocity impact prior to 2012 that produced vapor condensates as the dominant impact product. Two distinct short-term modulations in the ID8 system suggest two violent impacts at different times and locations. Its long-term variation is consistent with the collisional evolution of two different populations of impact-produced debris dominated by either vapor condensates or escaping boulders. The bright, variable emission from the dust produced in large impacts from extreme debris disks provides a unique opportunity to study violent events during the era of terrestrial planet formation. Subject headings: circumstellar matter -infrared: planetary systems -planets and satellites: dynamical evolution and stability -stars: individual (

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“…Another recently discovered and intriguing feature of RZ Psc is the comparatively large IR excess at λ > 5 µm: 8% from the star's bolometric luminosity (De Wit et al 2013). The origin of this excess associated with the presence of warm (T ≈ 500 K) dust produced presumably by the collisional activity in the star's debris disk.…”

Section: Introductionmentioning

confidence: 99%

An in-depth analysis of the RZ Piscium atmosphere

Potravnov

Гринин

Ilyin³

et al. 2014

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The star RZ Psc is one of the most unusual members of the UX Ori star family. It demonstrates all properties that are typical of these stars (the light variability, high linear polarization in deep minima, the blueing effect), but until recently there has been no obvious evidence of its youth. Recently, we have shown that RZ Psc is in the transitional evolutionary stage between stars with the primordial and debris disks. In this paper we present the results of the quantitative analysis of the star's spectrum. Using the high-resolution (R = 46 000) spectrum of RZ Psc obtained with Nordic Optical Telescope, we determined T eff = 5350 ± 150 K, log g = 4.2 ± 0.2, [M/H] = −0.3 ± 0.05. These parameters agree well with the same ones as for the stars recently passed the T Tauri star evolutionary stage. This supports our previous suggestion about the evolutionary status of RZ Psc as the post-T Tauri and post-UX Ori star.

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Active asteroid belt causes the UXOR phenomenon in RZ Piscium

Cited by 28 publications

References 35 publications

Is the Young Star RZ Piscium Consuming Its Own (Planetary) Offspring?

Is the Young Star RZ Piscium Consuming Its Own (Planetary) Offspring?

Extreme Debris Disk Variability: Exploring the Diverse Outcomes of Large Asteroid Impacts During the Era of Terrestrial Planet Formation

An in-depth analysis of the RZ Piscium atmosphere

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