Dynamical Masses of Low-mass Stars in the Taurus and Ophiuchus Star-forming Regions

Simon, M.; Guilloteau, S.; Folco, E. Di; Dutrey, Anne; Grosso, N.; Piétu, V.; Chapillon, E.; Prato, L.; Schaefer, Gail H.; Rice, Emily L.; Boehler, Yann

doi:10.3847/1538-4357/aa78f1

Cited by 67 publications

(64 citation statements)

References 36 publications

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“…The corresponding logarithmic luminosity relative to the Sun (log(L ⋆ /L ⊙ ) = 0.1±0.1) translates into a mass and radius of CI Tau equal to M ⋆ = 0.9 ± 0.1 M ⊙ and R ⋆ = 2.0 ± 0.3 R ⊙ respectively when using the PMS evolutionary models of Siess et al (2000, assuming solar metallicity and including convective overshooting); in this context, CI Tau is a 2 ± 1 Myr star that has not yet started to develop an inner radiative core. Our mass estimate is in very good agreement with the dynamic value derived from radio interferometry (equal to 0.90 ± 0.02 M ⊙ , Simon et al 2017Simon et al , 2019, which we use hereafter); our luminosity estimate is larger than the literature values (Andrews et al 2013;Herczeg & Hillenbrand 2014), reflecting both the revised distance and our choice to compensate for the contribution of spots at the stellar surface.…”

Section: Evolutionary Status Of CI Tausupporting

confidence: 87%

The magnetic field and accretion regime of CI Tau

Donati

Bouvier

Alencar

et al. 2019

Monthly Notices of the Royal Astronomical Society

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This paper exploits spectropolarimetric data of the classical T Tauri star CI Tau collected with ESPaDOnS at the Canada-France-Hawaii Telescope, with the aims of detecting and characterizing the large-scale magnetic field that the star hosts, and of investigating how the star interacts with the inner regions of its accretion disc through this field. Our data unambiguously show that CI Tau has a rotation period of 9.0 d, and that it hosts a strong, mainly poloidal large-scale field. Accretion at the surface of the star concentrates within a bright high-latitude chromospheric region that spatially overlaps with a large dark photospheric spot, in which the radial magnetic field reaches −3.7 kG. With a polar strength of −1.7 kG, the dipole component of the large-scale field is able to evacuate the central regions of the disc up to about 50% of the co-rotation radius (at which the Keplerian orbital period equals the stellar rotation period) throughout our observations, during which the average accretion rate was found to be unusually high. We speculate that the magnetic field of CI Tau is strong enough to sustain most of the time a magnetospheric gap extending to at least 70% of the co-rotation radius, which would explain why the rotation period of CI Tau is as long as 9 d. Our results also imply that the 9-d radial velocity (RV) modulation that CI Tau exhibits is attributable to stellar activity, and thus that the existence of the candidate close-in massive planet CI Tau b to which these RV fluctuations were first attributed needs to be reassessed with new evidence.

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Section: Evolutionary Status Of CI Tausupporting

confidence: 87%

The magnetic field and accretion regime of CI Tau

Donati

Bouvier

Alencar

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…we calculate a stellar mass from the isochrone of the average age in the full Taurus sample (∼ 2 Myr). We adopt the stellar dynamical mass measurements from the CO gas rotation for the two spectroscopic binaries (UZ Tau E, Simon et al 2000 andDQ Tau, Czekala et al 2016) and two relatively edge-on disks (HN Tau A and HK Tau B, Simon et al 2017), all corrected for the Gaia DR2 distance. In Lodato et al (2019), we analyzed the putative population of hidden planets in the subset of sources with substructures.…”

Section: Host Star Propertiesmentioning

confidence: 99%

Compact Disks in a High-resolution ALMA Survey of Dust Structures in the Taurus Molecular Cloud

Long

Herczeg

Harsono

et al. 2019

ApJ

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226

317

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We present a high-resolution (∼ 0. 12, ∼ 16 au, mean sensitivity of 50 µJy beam −1 at 225 GHz) snapshot survey of 32 protoplanetary disks around young stars with spectral type earlier than M3 in the Taurus star-forming region using Atacama Large Millimeter Array (ALMA). This sample includes most mid-infrared excess members that were not previously imaged at high spatial resolution, excluding close binaries and highly extincted objects, thereby providing a more representative look at disk properties at 1-2 Myr. Our 1.3 mm continuum maps reveal 12 disks with prominent dust gaps and rings, 2 of which are around primary stars in wide binaries, and 20 disks with no resolved features at the observed resolution (hereafter smooth disks), 8 of which are around the primary star in wide binaries. The smooth disks were classified based on their lack of resolved substructures, but their most prominent property is that they are all compact with small effective emission radii (R eff,95% 50 au). In contrast, all disks with R eff,95% of at least 55 au in our sample show detectable substructures. Nevertheless, their inner emission cores (inside the resolved gaps) have similar peak brightness, power law profiles, and transition radii to the compact smooth disks, so the primary difference between these two categories is the lack of outer substructures in the latter. These compact disks may lose their outer disk through arXiv:1906.10809v1 [astro-ph.SR] 26 Jun 2019 2 Long et al.fast radial drift without dust trapping, or they might be born with small sizes. The compact dust disks, as well as the inner disk cores of extended ring disks, that look smooth at the current resolution will likely show small-scale or low-contrast substructures at higher resolution. The correlation between disk size and disk luminosity correlation demonstrates that some of the compact disks are optically thick at millimeter wavelengths.

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“…Also, classical T Tauri SBs challenge our understanding of mass transfer from circumbinary to circumstellar disks and may represent a transitory evolutionary phase. Finally, SBs with circumbinary material potentially provide precise component stellar mass measurements (e.g., Simon et al 2017), as well as disk mass estimates (Andrews & Williams 2005), which would greatly inform our understanding of the star-disk interaction.…”

Section: Introductionmentioning

confidence: 99%

Orbital Solution for the Spectroscopic Binary in the GW Ori Hierarchical Triple

Prato

Ruíz-Rodríguez

Wasserman

2018

ApJ

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We present the first double-lined orbital solution for the close binary in the GW Ori triple system. Using 12 epochs of infrared spectroscopy, we detected the lines of both stars in the inner pair, previously known as single-lined only. Our preliminary infrared orbital solution has an eccentricity of e = 0.21 ± 0.10, a period of P = 241.15 ± 0.72 days, and a mass ratio of q = 0.66 ± 0.13. We find a larger semi-amplitude for the primary star, K1 = 6.57 ± 1.00 km s −1 , with an infrared-only solution compared to K1 = 4.41 ± 0.33 km s −1 with optical data from the literature, likely the result of line blending and veiling in the optical. The component spectral types correspond to G3 and K0 stars, with v sin i values of 43 km s −1 and 50 km s −1 , respectively. We obtained a flux ratio of α = 0.58 ± 0.14 in the H-band, allowing us to estimate individual masses of 3.2 and 2.7 M for the primary and secondary, respectively, using evolutionary tracks. The tracks also yield a coeval age of 1 Myr for both components to within 1σ. GW Ori is surrounded by a circumbinary/circumtriple disk. A tertiary component has been detected in previous studies; however, we did not detect this component in our near-infrared spectra, probably the result of its relative faintness and blending in the absorption lines of these rapidly rotating stars. With these results, GW Ori joins the small number of classical T Tauri, double-lined spectroscopic binaries.

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Dynamical Masses of Low-mass Stars in the Taurus and Ophiuchus Star-forming Regions

Cited by 67 publications

References 36 publications

The magnetic field and accretion regime of CI Tau

The magnetic field and accretion regime of CI Tau

Compact Disks in a High-resolution ALMA Survey of Dust Structures in the Taurus Molecular Cloud

Orbital Solution for the Spectroscopic Binary in the GW Ori Hierarchical Triple

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