On the age of the β Pictoris moving group

Mamajek, Eric E.; Bell, Cameron P. M.

doi:10.1093/mnras/stu1894

Cited by 289 publications

(281 citation statements)

References 67 publications

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“…Through the identification of the lithium depletion boundary, Binks & Jeffries (2014) and Malo et al (2014) found BPMG ages of 21 ± 4 Myr and 26 ± 3 Myr, respectively. This agrees with traceback ages from Makarov (2007) and Mamajek & Bell (2014). The latter used revised H astrometry data and also derived an isochronal age of 22 ± 3 Myr.…”

Section: Introductionsupporting

confidence: 85%

Collisional modelling of the AU Microscopii debris disc

Schüppler

Löhne

Krivov

et al. 2015

A&A

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AU Microscopii's debris disc is one of the most famous and best-studied debris discs and one of only two resolved debris discs around M stars. We perform in-depth collisional modelling of the AU Mic disc including stellar radiative and corpuscular forces (stellar winds), aiming at a comprehensive understanding of the dust production and the dust and planetesimal dynamics in the system. Our models are compared to a suite of observational data for thermal and scattered light emission, ranging from the ALMA radial surface brightness profile at 1.3 mm to spatially resolved polarisation measurements in the visible. Most of the data are shown to be reproduced with dust production in a belt of planetesimals with an outer edge at around 40 au and subsequent inward transport of dust by stellar winds. A low dynamical excitation of the planetesimals with eccentricities up to 0.03 is preferred. The radial width of the planetesimal belt cannot be constrained tightly. Belts that are 5 au and 17 au wide, as well as a broad 44 au-wide belt, are consistent with observations. All models show surface density profiles that increase with distance from the star up to ≈40 au, as inferred from observations. The best model is achieved by assuming a stellar mass loss rate that exceeds the solar one by a factor of 50. The models reproduce the spectral energy distribution and the shape of the ALMA radial profile well, but deviate from the scattered light observations more strongly. The observations show a bluer disc colour and a lower degree of polarisation for projected distances <40 au than predicted by the models. These deviations may be reduced by taking irregularly shaped dust grains which have scattering properties different from the Mie spheres used in this work. From tests with a handful of selected dust materials, we favour mixtures of silicate, carbon, and ice of moderate porosity. We also address the origin of the unresolved central excess emission detected by ALMA and show that it cannot stem from an additional inner belt alone. Instead, it should derive, at least partly, from the chromosphere of the central star.

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Section: Introductionsupporting

confidence: 85%

Collisional modelling of the AU Microscopii debris disc

Schüppler

Löhne

Krivov

et al. 2015

A&A

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“…The star: β Pictoris is a bright (V = 3.85; Crifo et al 1997), southern (α = 05h47m17.08769s δ = −51 • 03 59.4412 ), nearby (d = 19.44 ± 0.05 pc; van Leeuwen 2007), young (23 ± 3 Myr; Mamajek & Bell 2014;Binks & Jeffries 2016), hot star (T eff = 8052 K; A6V; Gray et al 2006). The star has been reported to have δ Scuti like pulsations (Koen et al 2003).…”

Section: β Pictoris B and The Inferior Conjunction Of 2017mentioning

confidence: 99%

“…The young (∼23 Myr old; Mamajek & Bell 2014) star β Pictoris hosts a near edge-on dusty debris disk (first directly imaged by Smith & Terrile 1984) and a 13 M Jup planet (Lagrange et al 2009b,a;Chilcote et al 2017). The planet has been measured to have an orbital period of approximately 20 yr through astrometric monitoring (Chauvin et al 2012;Nielsen et al 2014;Millar-Blanchaer et al 2015), and the Hill sphere of the planet will transit from April 2017 to March 2018 (Wang et al 2016), lasting approximately 300 days, with an impact parameter of 20% of the Hill radius.…”

Section: Introductionmentioning

confidence: 99%

bRing: An observatory dedicated to monitoring the β Pictoris b Hill sphere transit

Stuik

Bailey

Dorval

et al. 2017

A&A

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Aims. We describe the design and first light observations from the β Pictoris b Ring ("bRing") project. The primary goal is to detect photometric variability from the young star β Pictoris due to circumplanetary material surrounding the directly imaged young extrasolar gas giant planet β Pictoris b. Methods. Over a nine month period centred on September 2017, the Hill sphere of the planet will cross in front of the star, providing a unique opportunity to directly probe the circumplanetary environment of a directly imaged planet through photometric and spectroscopic variations. We have built and installed the first of two bRing monitoring stations (one in South Africa and the other in Australia) that will measure the flux of β Pictoris, with a photometric precision of 0.5% over 5 min. Each station uses two wide field cameras to cover the declination of the star at all elevations. Detection of photometric fluctuations will trigger spectroscopic observations with large aperture telescopes in order to determine the gas and dust composition in a system at the end of the planet-forming era. Results. The first three months of operation demonstrate that bRing can obtain better than 0.5% photometry on β Pictoris in five minutes and is sensitive to nightly trends enabling the detection of any transiting material within the Hill sphere of the exoplanet.

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“…Various age estimates for the β Pic MG in the literature based on different methods such as the lithium depletion boundary, kinematics and ischronal fitting constrains the age to the range 10 − 40 Myr (see e.g. Mamajek & Bell 2014, for a summary). A system age in this interval can not be rejected from this analysis.…”

Section: Hertzsprung-russell Diagrammentioning

confidence: 99%

Characterization of close visual binaries from the AstraLux Large M Dwarf Survey

Bergfors¹,

Brandner²,

Bonnefoy³

et al. 2015

Mon. Not. R. Astron. Soc.

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We present VLT/SINFONI J, H + K spectra of seven close visual pairs in M dwarf binary/triple systems, discovered or observed by the AstraLux M dwarf survey. We determine the spectral types to within ±1.0 subclasses from comparison to template spectra and the strength of K-band water absorption, and derive effective temperatures. The results are compared to optical spectral types of the unresolved binary/multiple systems, and we confirm that our photometric method to derive spectral types in the AstraLux M dwarf survey is accurate. We look for signs of youth such as chromospheric activity and low surface gravity, and find an age in the range 0.25 − 1 Gyr for the GJ 852 system. Strong Li absorption is detected in optical spectra of the triple system J024902 obtained with FEROS at the ESO-MPG 2.2 m telescope. The equivalent width of the absorption suggests an age consistent with the β Pic moving group. However, further observations are needed to establish group membership. Ongoing orbital monitoring will provide dynamical masses and thus calibration of evolutionary models for low mass stars.

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On the age of the β Pictoris moving group

Cited by 289 publications

References 67 publications

Collisional modelling of the AU Microscopii debris disc

Collisional modelling of the AU Microscopii debris disc

bRing: An observatory dedicated to monitoring the β Pictoris b Hill sphere transit

Characterization of close visual binaries from the AstraLux Large M Dwarf Survey

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