A dusty M5 binary in the<i>β</i>Pictoris moving group

Rodríguez, David; Zuckerman, B.; Faherty, Jacqueline K.; Vican, Laura

doi:10.1051/0004-6361/201423604

Cited by 18 publications

(12 citation statements)

References 55 publications

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“…Disregarding ∼10-20 Myr-old (and younger) systems whose disks may be primordial in nature (see, e.g., Rodriguez et al 2014, and references therein), the only other multiple system known to host two disks is that of Fomalhaut, also part of this survey (see Kennedy et al 2014). As a member of AB Dor (Malo et al 2013;Zuckerman et al 2011), HD 223352 has an age of ∼100 Myr and represents a rare opportunity to study the development and evolution of disks around a pair of co-eval stars.…”

Section: Individual Binary Debris-disk Systemsmentioning

confidence: 99%

Stellar multiplicity and debris discs: an unbiased sample

Rodríguez

Duchêne

Tom

et al. 2015

Monthly Notices of the Royal Astronomical Society

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Circumstellar dust disks have been observed around many nearby stars. However, many stars are part of binary or multiple stellar systems. A natural question arises regarding the presence and properties of such disks in systems with more than one star. To address this, we consider a sample of 449 systems (spectral types A-M) observed with the Herschel Space Observatory as part of the DEBRIS program. We have examined the stellar multiplicity of this sample by gathering information from the literature and performing an adaptive optics imaging survey at Lick Observatory. Five new companions were revealed with our program. In total, we identify 188 (42%) binary or multiple star systems. The multiplicity of the sample is examined with regards to the detection of circumstellar disks for stars of spectral types AFGK.In general, disks are less commonly detected around binaries than single stars, though the disk frequency is comparable among A stars regardless of multiplicity. However, this sample reveals the period distribution of disk-bearing binaries is consistent with that of non-disk binaries and with comparison field samples. We find that the properties of disks in binary systems are not statistically different from those around single stars. Although the frequency of disk-bearing FGK binaries may be lower than in single star systems, the processes behind disk formation and the characteristics of these disks are comparable among both populations.

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Section: Individual Binary Debris-disk Systemsmentioning

confidence: 99%

Stellar multiplicity and debris discs: an unbiased sample

Rodríguez

Duchêne

Tom

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…Far from being the exception, "old discs" that are still capable of growing planetary systems (Hughes at al. 2008, Moor et al 2011, Bergin et al 2013, Rodriguez et al 2014, Zuckerman 2014 might actually be the rule. The higher frequency of stars with relatively long-lived discs is also in line with the results of the HARPS exoplanet survey (Mayor et al 2011) in which >50% of stars host at least one planet, and the 14% of stars hosting gaseous planets seem to be only a lower limit as the percentage of gas giants increases steadily with the logarithm of the period (limited to 400 days).…”

Section: Discussionmentioning

confidence: 97%

Short Dissipation Times of Proto-Planetary Disks: An Artifact of Selection Effects?

Pfalzner

Steinhausen

Menten

2014

ApJ

118

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The frequency of discs around young stars, a key parameter for understanding planet formation, is most readily determined in young stellar clusters where many relatively coeval stars are located in close proximity. Observational studies seem to show that the disc frequency decreases rapidly with cluster age with <10% of cluster stars retaining their discs for longer than 2-6 Myr. Given that at least half of all stars in the field seem to harbor one or more planets, this would imply extremely fast disc dispersal and rapid planet growth. Here we question the validity of this constraint by demonstrating that the short disc dissipation times inferred to date might have been heavily underestimated by selection effects. Critically, for ages >3Myr only stars that originally populated the densest areas of very populous clusters, which are prone to disc erosion, are actually considered. This tiny sample may not be representative of the majority of stars. In fact, the higher disc fractions in co-moving groups indicate that it is likely that over 30% of all field stars retain their discs well beyond 10 Myr, leaving ample time for planet growth. Equally our solar system, with a likely formation time > 10 Myr, need no longer be an exception but in fact typical of planetary systems.

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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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A dusty M5 binary in theβPictoris moving group

Cited by 18 publications

References 55 publications

Stellar multiplicity and debris discs: an unbiased sample

Stellar multiplicity and debris discs: an unbiased sample

Short Dissipation Times of Proto-Planetary Disks: An Artifact of Selection Effects?

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

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