Dynamical Masses of T Tauri Stars and Calibration of Pre–Main‐Sequence Evolution

Simon, M.; Dutrey, Anne; Guilloteau, S.

doi:10.1086/317838

Cited by 411 publications

(523 citation statements)

References 20 publications

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“…Although there have been recent advances in determining the masses of 1-2 M pre-main-sequence (PMS) stars, there exist only a few measurements of the masses of sub-solar mass PMS stars (Simon 2001). As a result, theoretical PMS evolutionary tracks have not been well calibrated at the low-mass end, where uncertainties in the models give rise to scatter as large as a factor of 3 in mass and 10 in age (Simon, Dutrey, & Guilloteau 2000). Dynamical measurements of the masses of close binary systems comprised of coeval components with a small mass ratio provide an initial step toward tests of the PMS tracks over a broad parameter range.…”

Section: Introductionmentioning

confidence: 99%

The Smallest Mass Ratio Young Star Spectroscopic Binaries

Prato

Simon

Mazeh

et al. 2002

ApJ

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101

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Using high-resolution near-infrared spectroscopy with the Keck Telescope, we have detected the radial velocity signatures of the cool secondary components in four optically identified pre-main-sequence, singlelined spectroscopic binaries. All are weak-lined T Tauri stars with well-defined center-of-mass velocities. The mass ratio for one young binary, NTTS 160905À1859, is M 2 /M 1 = 0.18 AE 0.01, the smallest yet measured dynamically for a pre-main-sequence spectroscopic binary. These new results demonstrate the power of infrared spectroscopy for the dynamical identification of cool secondaries. Visible-light spectroscopy, to date, has not revealed any pre-main-sequence secondary stars with masses <0.5 M , while two of the young systems reported here are in that range. We compare our targets with a compilation of the published young, double-lined spectroscopic binaries and discuss our unique contribution to this sample.

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Section: Introductionmentioning

confidence: 99%

The Smallest Mass Ratio Young Star Spectroscopic Binaries

Prato

Simon

Mazeh

et al. 2002

ApJ

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101

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“…By direct imaging, the incredible diversity of the disk morphology, such as spiral and gap structures, has been revealed (e.g., Hashimoto et al 2012). LkCa 15 (K5, 0.97 M⊙, 2−5 Myr old; Simon et al 2000), a young solar-like star located in the Taurus-Auriga region (∼140 pc), is one of the most intensively studied transitional disk systems around the T Tauri star. Espaillat et al (2007) conducted a detailed analysis of SED in LkCa 15 and suggested the existence of a gap structure at ∼46AU.…”

Section: Introductionmentioning

confidence: 99%

Near-infrared imaging polarimetry of LkCa 15: A possible warped inner disk

Hashimoto

Tamura

et al. 2016

Publications of the Astronomical Society of Japan

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We present high-contrast H-band polarized intensity images of the transitional disk around the young solar-like star LkCa 15. By utilizing Subaru/HiCIAO for polarimetric differential imaging, both the angular resolution and the inner working angle reach 0.07 ′′ and r=0.1 ′′ , respectively. We obtained a clearly resolved gap (width < ∼ 27 AU) at ∼ 48 AU from the central star. This gap is consistent with images reported in previous studies. We also confirmed the existence of a bright inner disk with a misaligned position angle of 13±4 • with respect to that of the outer disk, i.e., the inner disk is possibly warped. The large gap and the warped inner disk both point to the existence of a multiple planetary system with a mass of < ∼ 1M Jup .

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“…the competitive accretion ones (Bonnell & Bate 2006), or those proposing Bondi-Hoyle accretion (Keto 2007) predict the existence of a circumstellar accretion disk, in a sort of scaled-up version of low-mass star formation. However, while the existence of Keplerian rotating disks about low-mass young stellar objects (YSOs) and their importance have been assessed well (e.g., Burrows et al 1996;Simon et al 2000), the situation is less clear for higher mass protostars. In several cases, evidence of disks around high-mass YSOs have been reported in the literature (see Beltrán 2011 and references therein).…”

Section: Introductionmentioning

confidence: 99%

Filamentary structure and Keplerian rotation in the high-mass star-forming region G35.03+0.35 imaged with ALMA

Beltrán

Sánchez-Monge

Cesaroni

et al. 2014

A&A

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Context. Theoretical scenarios propose that high-mass stars are formed by disk-mediated accretion. Aims. To test the theoretical predictions on the formation of massive stars, we wish to make a thorough study at high-angular resolution of the structure and kinematics of the dust and gas emission toward the high-mass star-forming region G35.03+0.35, which harbors a disk candidate around a B-type (proto)star. Methods. We carried out ALMA Cycle 0 observations at 870 μm of dust of typical high-density, molecular outflow, and cloud tracers with resolutions of <0. 5. Complementary Subaru COMICS 25 μm observations were carried out to trace the mid-infrared emission toward this star-forming region. Results. The submillimeter continuum emission has revealed a filamentary structure fragmented into six cores, called A-F. The filament could be in quasi-equilibrium taking into account that the mass per unit length of the filament, 200-375 M /pc, is similar to the critical mass of a thermally and turbulently supported infinite cylinder, ∼335 M /pc. The cores, which are on average separated by ∼0.02 pc, have deconvolved sizes of 1300-3400 AU, temperatures of 35-240 K, H 2 densities >10 7 cm −3 , and masses in the range 1-5 M , and they are subcritical. Core A, which is associated with a hypercompact Hii region and could be the driving source of the molecular outflow observed in the region, is the most chemically rich source in G35.03+0.35 with strong emission of typical hot core tracers such as CH 3 CN. Tracers of high density and excitation show a clear velocity gradient along the major axis of the core, which is consistent with a disk rotating about the axis of the associated outflow. The PV plots along the SE-NW direction of the velocity gradient show clear signatures of Keplerian rotation, although infall could also be present, and they are consistent with the pattern of an edge-on Keplerian disk rotating about a star with a mass in the range 5-13 M . The high t ff /t rot ratio for core A suggests that the structure rotates fast and that the accreting material has time to settle into a centrifugally supported disk. Conclusions. G35.03+0.35 is one of the most convincing examples of Keplerian disks rotating about high-mass (proto)stars. This supports theoretical scenarios according to which high-mass stars, at least B-type stars, would form through disk-mediated accretion.

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Dynamical Masses of T Tauri Stars and Calibration of Pre–Main‐Sequence Evolution

Cited by 411 publications

References 20 publications

The Smallest Mass Ratio Young Star Spectroscopic Binaries

The Smallest Mass Ratio Young Star Spectroscopic Binaries

Near-infrared imaging polarimetry of LkCa 15: A possible warped inner disk

Filamentary structure and Keplerian rotation in the high-mass star-forming region G35.03+0.35 imaged with ALMA

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