A dynamical calibration of the mass–luminosity relation at very low stellar masses and young ages

Close, Laird M.; Lenzen, R.; Guirado, J. C.; Nielsen, Eric L.; Mamajek, Eric E.; Brandner, W.; Hartung, Markus; Lidman, C.; Biller, Beth

doi:10.1038/nature03225

Cited by 158 publications

(238 citation statements)

References 21 publications

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“…These include Close et al (2005) and Reiners et al (2005) who, with dynamical mass determinations and age estimates, find that commonly used M dwarf 2.1 Core Accretion-Gas Capture Model evolutionary tracks (e.g. Burrows et al, 1997;Chabrier et al, 2000) overestimate the luminosity of these objects at ages of ∼50 -100 Myr (for the Close et al work) and ∼5 Myr (for the Reiners et al work).…”

Section: Introductionmentioning

confidence: 99%

Young Jupiters are faint: new models of the early evolution of giant planets

Fortney¹,

Marley

Hubickyj

et al. 2005

Astron Nachr

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Abstract.Here we show preliminary calculations of the cooling and contraction of a 2 MJ planet. These calculations, which are being extended to 1-10 MJ, differ from other published "cooling tracks" in that they include a core accretion-gas capture formation scenario, the leading theory for the formation of gas giant planets. We find that the initial post-accretionary intrinsic luminosity of the planet is ∼3 times less than previously published models which use arbitrary initial conditions. These differences last a few tens of millions of years. Young giant planets are intrinsically fainter than has been previously appreciated. We also discuss how uncertainties in atmospheric chemistry and the duration of the formation time of giant planets lead to challenges in deriving planetary physical properties from comparison with tabulated model values.

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Section: Introductionmentioning

confidence: 99%

Young Jupiters are faint: new models of the early evolution of giant planets

Fortney¹,

Marley

Hubickyj

et al. 2005

Astron Nachr

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“…Atmospheric and evolutionary models are particularly poorly constrained for young ( 100 Myr) M dwarfs, of which only a handful of binaries have measured dynamical masses (see, e.g., Close et al 2005;Bonnefoy et al 2009). In order to better constrain multiplicity properties and identify young binaries suitable for dynamical mass measurements, we carried out the AstraLux large M dwarf survey: a Lucky Imaging multiplicity survey of 761 young, nearby late-K and M dwarfs (Bergfors et al 2010;Janson et al 2012), supplemented by 286 mid-to late-M dwarfs in an extension of the survey (Janson et al 2014a).…”

Section: Introductionmentioning

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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“…However, these models are not valid at the young age of GQ Lup, so that they are not applicable. According to both Mohanty et al (2004b) and Close et al (2005), the Baraffe et al (2002) models overestimate the masses of young sub-stellar objects below ∼ 30 M Jup , but may underestimate them above ∼ 40 M Jup . This is consistent with our results.…”

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confidence: 99%

GQLup and its common proper motion companion

Mugrauer¹,

Neuhaeuser²

2005

Astron. Nachr.

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Abstract. Recently, Neuhäuser et al. (2005a) presented evidence for a sub-stellar, common proper motion companion to GQ Lup. With two theoretical mass estimates, both below the Deuterium burning minimum mass limit, the companion is probably a planet imaged directly. We present here a more detailed astrometric analysis of the GQ Lup system, using all the (different) proper motions published for the primary. The common proper motion is significant in all cases, also when taking into account the error in parallax or distance (140 ± 50 pc). When using the weighted mean, the significance for common proper motion of GQ Lup and its companion is 7 σ + 4 σ for no change in separation plus 8 σ for no change in position angle. We also discuss the question, whether GQ Lup and its common-proper motion companion are not bound, but share the same or similar proper motion as two independent members of the Lupus T association, which is a moving group, where most members should have the same motion anyway. Given our discussion, this hypothesis can be rejected by several σ: The probability to find by chance an L-dwarf fainter than KS = 14 mag within 0. 7325 with (almost) the same proper motion of GQ Lup is only ≤ 3 · 10 −10 . The orbital motion of the system is not yet detected (1.4 ± 2.2 mas/yr), but is probably smaller than the escape velocity (5.3 ± 2.1 mas/yr), so that the system may well be gravitationally bound and stable. This is different for the 2MASSWJ 1207334-393254 system, as we also show.

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A dynamical calibration of the mass–luminosity relation at very low stellar masses and young ages

Cited by 158 publications

References 21 publications

Young Jupiters are faint: new models of the early evolution of giant planets

Young Jupiters are faint: new models of the early evolution of giant planets

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

GQLup and its common proper motion companion

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