A New M Dwarf Debris Disk Candidate in a Young Moving Group Discovered With Disk Detective

Silverberg, Steven M.; Kuchner, Marc J.; Wisniewski, John P.; Gagné, Jonathan; Bans, Alissa S.; Bhattacharjee, Shambo; Currie, Thayne; Debes, John H.; Biggs, Joseph R.; Bosch, Milton K. D.; Doll, Katharina; Luca, Hugo A. Durantini; Enachioaie, Alexandru; Griffith, Philip; Hyogo, Michiharu; Piñiero, Fernanda

doi:10.3847/2041-8205/830/2/l28

Cited by 33 publications

(50 citation statements)

References 42 publications

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“…Haisch et al 2001). However, discoveries of some young, very low-mass stars hosting gaseous accretion disks at ages as old as ∼20 -50 Myr (Murphy et al 2017;Silverberg et al 2016;Rodriguez et al 2014, and references therein) force a reconsideration of these timescales and may shed light on the circumstances of the TRAPPIST-1 system's formation and evolution. Possible consequences of long term disk retention are eccentricity dampening and convergent migration (Ogihara & Ida 2009), potentially yielding compact systems in resonant chains like TRAPPIST-1.…”

Section: Trappist-1 In Context: Planetary Systemsmentioning

confidence: 99%

Plausible Compositions of the Seven TRAPPIST-1 Planets Using Long-term Dynamical Simulations

Quarles

Quintana

Lopez

et al. 2017

ApJL

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TRAPPIST-1 is a nearby ultra-cool dwarf that is host to a remarkable planetary system consisting of seven transiting planets. The orbital properties and radii of the planets have been well-constrained, and recently the masses of the inner six planets have been measured with additional ground and spacebased photometric observations. Large uncertainties in these mass measurements have prevented a robust analysis of the planetary compositions. Here we perform many thousands of N-body dynamical simulations with planet properties perturbed from the observed values and identify those that are stable for millions of years. This allows us to identify self-consistent orbital solutions that can be used in future studies. From our range of dynamical masses, we find that most of the planets are consistent with an Earth-like composition, where TRAPPIST-1f is likely to have a volatile-rich envelope.

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Section: Trappist-1 In Context: Planetary Systemsmentioning

confidence: 99%

Plausible Compositions of the Seven TRAPPIST-1 Planets Using Long-term Dynamical Simulations

Quarles

Quintana

Lopez

et al. 2017

ApJL

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“…Recently, several examples of circumstellar disc accretion at ages greater than ∼10 Myr have been identified (e.g., PDS 66-20 Myr; Mamajek et al 2002, HD 21197-30 Myr;Moór et al 2011, 49 Ceti-40 Myr;Zuckerman & Song 2012, WISE J080822.18-644357.3-45 Myr;Silverberg et al 2016;Murphy et al 2018, J0446A & B, J0949A & B;, and they have been treated as unusual anomalies without delving into the problem of prolonged gas accretion at extreme ages. In spite of the small number of cases, such E-mail: song@uga.edu old pre-MS stars hosting accretion discs can be challenging to the hypothesis for the rapid planet formation (Pfalzner & Bannister 2019;Manara et al 2018;Najita & Kenyon 2014;Greaves & Rice 2010) and provide the upper limit on the life times of gas-rich discs.…”

Section: Introductionmentioning

confidence: 99%

2MASS J15460752−6258042: a mid-M dwarf hosting a prolonged accretion disc

Lee

Song

Murphy

2020

Monthly Notices of the Royal Astronomical Society

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We report the discovery of the oldest (∼55 Myr) mid-M type star known to host on-going accretion. 2MASS J15460752−6258042 (2M1546, spectral type M5, 59.2 pc) shows spectroscopic signs of accretion such as strong Hα, He i, and [O i] emission lines, from which we estimate an accretion rate of ∼10 −10 M yr −1 . Considering the clearly detected infrared excess in all WISE bands, the shape of its spectral energy distribution and its age, we believe the star is surrounded by a transitional disc, clearly with some gas still present at inner radii. The position and kinematics of the star from Gaia DR2 and our own radial velocity measurements suggest membership in the nearby ∼55 Myr-old Argus moving group. At only 59pc from Earth, 2M1546 is one of the nearest accreting mid-M dwarfs, making it an ideal target for studying the upper limit on the lifetimes of gas-rich discs around low mass stars.

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“…Clearly, the discovery of additional 'old' pre-MS stars hosting primordial discs and showing signs of accretion would be useful in better understanding the evolution and dissipation of discs, especially extreme examples much older than 10 Myr. Through the work of the NASA Disk Detective citizen science project 1 (described in Kuchner et al 2016), Silverberg et al (2016) recently identified WISE J080822.18-644357.3 (hereafter WISE J0808−6443) as an M dwarf exhibiting significant excess emission in the 12 and 22 µm bands of the Widefield Infrared Survey Explorer (WISE) survey (Wright et al 2010 Malo et al 2013;Gagné et al 2014) to establish whether the star was associated with any of the seven nearest young moving groups in the Solar neighbourhood (see reviews by Zuckerman & Song 2004;Torres et al 2008;Mamajek 2016), finding a 93.9 per cent probability that it is a member of the 45 Myr-old Carina association at a distance of ∼65 pc. Silverberg et al (2016) classified the star as hosting a second-generation debris disc, whereas the strength of its infrared excess (L IR /L 0.1) appears to be more consistent with a young primordial disc (Wyatt 2008).…”

Section: Introductionmentioning

confidence: 99%

WISE J080822.18−644357.3 – a 45 Myr-old accreting M dwarf hosting a primordial disc

Murphy

Mamajek

Bell

2018

Monthly Notices of the Royal Astronomical Society

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WISE J080822.18-644357.3 (WISE J0808-6443) was recently identified as a new M dwarf debris disc system and a candidate member of the 45 Myr-old Carina association. Given that the strength of its infrared excess (L IR /L 0.1) appears to be more consistent with a young protoplanetary disc, we present the first optical spectra of the star and reassess its evolutionary and membership status. We find WISE J0808−6443 to be a Li-rich M5 star with strong Hα emission (−125 < EW < −65 Å over 4 epochs) whose strength and broad width are consistent with accretion at a low level (∼10 −10 M yr −1 ) from its disc. The spectral energy distribution of the star is consistent with a primordial disc and is well-fit using a two-temperature blackbody model with T inner 1100 K and T outer 240 K. AllWISE multi-epoch photometry shows the system exhibits significant variability in the 3.4 µm and 4.6 µm bands. We calculate an improved proper motion based on archival astrometry, and combined with a new radial velocity, the kinematics of the star are consistent with membership in Carina at a kinematic distance of 90 ± 9 pc. The spectroscopic and photometric data are consistent with WISE J0808−6443 being a ∼0.1 M Classical T-Tauri star and one of the oldest known accreting M-type stars. These results provide further evidence that the upper limit on the lifetimes of gas-rich discsand hence the timescales to form and evolve protoplanetary systems -around the lowest mass stars may be longer than previously recognised, or some mechanism may be responsible for regenerating short-lived discs at later stages of pre-main sequence evolution.

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A New M Dwarf Debris Disk Candidate in a Young Moving Group Discovered With Disk Detective

Cited by 33 publications

References 42 publications

Plausible Compositions of the Seven TRAPPIST-1 Planets Using Long-term Dynamical Simulations

Plausible Compositions of the Seven TRAPPIST-1 Planets Using Long-term Dynamical Simulations

2MASS J15460752−6258042: a mid-M dwarf hosting a prolonged accretion disc

WISE J080822.18−644357.3 – a 45 Myr-old accreting M dwarf hosting a primordial disc

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