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

Punzi, Kristina; Kastner, Joel H.; Melis, Carl; Zuckerman, B.; Pilachowski, Catherine A.; Gingerich, Lydia; Knapp, Tori

doi:10.3847/1538-3881/aa9524

Cited by 39 publications

(20 citation statements)

References 68 publications

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“…These are similar in lightcurve behavior to the "dipper" behavior seen for protoplanetary disk systems (e.g., Morales-Calderón et al 2011;Cody et al 2014, and references therein), although their circumstellar material is thought to be secondary in nature (generated by the collisional breakdown of mature planetesimals/planets). Such systems are typically young ( 100 Myr) and in at least one case are also host to gaseous material (e.g., Punzi et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Highly structured inner planetary system debris around the intermediate age Sun-like star TYC 8830 410 1

Melis,

Olofsson,

Song

et al. 2021

Preprint

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We present detailed characterization of the extremely dusty main sequence star TYC 8830 410 1. This system hosts inner planetary system dust (T dust ≈300 K) with a fractional infrared luminosity of ∼1%. Mid-infrared spectroscopy reveals a strong, mildy-crystalline solid-state emission feature. TYC 8830 410 1 (spectral type G9 V) has a 49.5 ′′ separation M4-type companion co-moving and co-distant with it, and we estimate a system age of ∼600 Myr. TYC 8830 410 1 also experiences "dipper"-like dimming events as detected by ASAS-SN, TESS, and characterized in more detail with the LCOGT. These recurring eclipses suggest at least one roughly star-sized cloud of dust orbits the star in addition to assorted smaller dust structures. The extreme properties of the material orbiting TYC 8830 410 1 point to dramatic dust-production mechanisms that likely included something similar to the giant-impact event thought to have formed the Earth-Moon system, although hundreds of millions of years after such processes are thought to have concluded in the solar system. TYC 8830 410 1 holds promise to deliver significant advances in our understanding of the origin, structure, and evolution of extremely dusty inner planetary systems. 2 C. Melis et al.

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Section: Introductionmentioning

confidence: 99%

Highly structured inner planetary system debris around the intermediate age Sun-like star TYC 8830 410 1

Melis,

Olofsson,

Song

et al. 2021

Preprint

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“…The transitional era between the YSO and mature stellar phases, populated by ∼100 Myr-old stars near the zeroage main sequence, could also illuminate the dipper phenomenon. An example is RZ Piscium, an isolated, post-T Tauri star that is pre-main sequence but older than most dipper stars (30-50 Myr Grinin et al 2010;Punzi et al 2018), has both UX Ori-like dimming and a substantial infrared excess from circumstellar dust (de Wit et al 2013). Its identification as a UX Ori-like variable was serendipitous since it lies well above the Galactic plane, far from any known star-forming region or known cluster, and lacks the defining attributes of a YSO.…”

Section: Introductionmentioning

confidence: 99%

Planetesimals around stars with TESS (PAST) – I. Transient dimming of a binary solar analogue at the end of the planet accretion era

Gaidos

Jacobs

LaCourse³

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We report detection of quasi-periodic (1.5-day) dimming of HD 240779, the solar-mass primary in a 5" visual binary (also TIC 284730577), by the Transiting Exoplanet Survey Satellite. This dimming, as has been shown for other "dipper" stars, is likely due to occultation by circumstellar dust. The barycentric space motion, lithium abundance, rotation, and chromospheric emission of the stars in this system point to an age of ≈125 Myr, and possible membership in the AB Doradus moving group. As such it occupies an important but poorly explored intermediate regime of stars with transient dimming between young stellar objects in star forming regions and main sequence stars, and between UX Orionis-type Ae/Be stars and M-type "dippers". HD 240779, but not its companion BD+10 714B, has WISE -detected excess infrared emission at 12 and 22 µm indicative of circumstellar dust. We propose that infrared emission is produced by collisions of planetesimals during clearing of a residual disk at the end of rocky planet formation, and that quasi-periodic dimming is produced by the rapid disintegration of a 100 km planetesimal near the silicate evaporation radius. Further studies of this and similar systems will illuminate a poorly understood final phase of rocky planet formation like that which produced the inner Solar System.

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“…A lower limit to desorption from such debris is provided in Table 5 as M 0 d , which also serves as a lower limit for a desorbing Trojan source with negligible tidal heating. Dust signatures from a catastrophically disintegrating body appear to be rare as is the case for the planetary systems at the anomalous stars KIC12557548, KIC 8462852, RZ Piscium and WD 1145+017 (Rappaport et al (2012); Boyajian et al (2016); Punzi et al (2018); Vanderburg et al (2015)). Nonetheless, the fact that all strongly outgassing alkaline systems have sub-Saturnian densities ( Table 3: ) may suggest a close-in torus of exogenic material (Zuluaga et al 2015).…”

Section: Exo-iomentioning

confidence: 99%

Sodium and Potassium Signatures of Volcanic Satellites Orbiting Close-in Gas Giant Exoplanets

Oza

Johnson

Lellouch

et al. 2019

ApJ

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Extrasolar satellites are generally too small to be detected by nominal searches. By analogy to the most active body in the Solar System, Io, we describe how sodium (Na I) and potassium (K I) gas could be a signature of the geological activity venting from an otherwise hidden exo-Io. Analyzing ∼ a dozen close-in gas giants hosting robust alkaline detections, we show that an Io-sized satellite can be stable against orbital decay below a planetary tidal Q p 10 11 . This tidal energy is focused into the satellite driving a ∼ 10 5±2 higher mass loss rate than Io's supply to Jupiter's Na exosphere, based on simple atmospheric loss estimates. The remarkable consequence is that several exo-Io column densities are on average more than sufficient to provide the ∼ 10 10±1 Na cm −2 required by the equivalent width of exoplanet transmission spectra. Furthermore, the benchmark observations of both Jupiter's extended (∼ 1000 R J ) Na exosphere and Jupiter's atmosphere in transmission spectroscopy yield similar Na column densities that are purely exogenic in nature. As a proof of concept, we fit the "high-altitude" Na at WASP 49-b with an ionization-limited cloud similar to the observed Na profile about Io. Moving forward, we strongly encourage time-dependent ingress and egress monitoring along with spectroscopic searches for other volcanic volatiles.

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

Cited by 39 publications

References 68 publications

Highly structured inner planetary system debris around the intermediate age Sun-like star TYC 8830 410 1

Highly structured inner planetary system debris around the intermediate age Sun-like star TYC 8830 410 1

Planetesimals around stars with TESS (PAST) – I. Transient dimming of a binary solar analogue at the end of the planet accretion era

Sodium and Potassium Signatures of Volcanic Satellites Orbiting Close-in Gas Giant Exoplanets

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