A bright inner disk and structures in the transition disk around the very low-mass star CIDA 1

Pinilla, P.; Kurtovic, Nicolás T.; Benisty, M.; Manara, C. F.; Natta, A.; Sanchís, E.; Tazzari, Marco; Stammler, Sebastian Markus; Ricci, Luca; Testi, L.

doi:10.1051/0004-6361/202140371

Cited by 26 publications

(59 citation statements)

References 80 publications

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“…As in Section 5, we used an X-ray luminosity of L x = 10 31 ergs −1 , α dz = 10 −4 , and r dz = 10 AU, but we take the snapshot at 1.2 Myr, since the gap opens earlier when using the initial condition from Equation A.1. The main difference is that now the surface brightness of the inner disk is comparable to that of the outer ring in the millimeter continuum, as observed in some transition disks (Hendler et al 2018;Pinilla et al 2021).…”

Section: Discussionmentioning

confidence: 93%

“…Through radiative transfer models, it has been possible to measure the radial extent of the dust cavity for a wide sample of transition disks (van der Marel et al 2016b), and observations at different wavelengths have also shown that some of these objects retain a compact dust component close to the star (e.g. Espaillat et al 2010;Benisty et al 2010;Olofsson et al 2013;Matter et al 2016;Kluska et al 2018;Pinilla et al 2019Pinilla et al , 2021, demonstrating that for some transition disks the gap is not completely devoid of dust.…”

Section: Introductionmentioning

confidence: 99%

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Large gaps and high accretion rates in photoevaporative transition disks with a dead zone

Gárate

Delage

Stadler

et al. 2021

A&A

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Context. Observations of young stars hosting transition disks show that several of them have high accretion rates, despite their disks presenting extended cavities in their dust component. This represents a challenge for theoretical models, which struggle to reproduce both features simultaneously. Aims. We aim to explore if a disk evolution model, including a dead zone and disk dispersal by X-ray photoevaporation, can explain the high accretion rates and large gaps (or cavities) measured in transition disks. Methods. We implemented a dead zone turbulence profile and a photoevaporative mass-loss profile into numerical simulations of gas and dust. We performed a population synthesis study of the gas component and obtained synthetic images and SEDs of the dust component through radiative transfer calculations. Results. This model results in long-lived inner disks and fast dispersing outer disks that can reproduce both the accretion rates and gap sizes observed in transition disks. For a dead zone of turbulence αdz = 10−4 and an extent rdz = 10 AU, our population synthesis study shows that 63% of our transition disks are still accreting with Ṁg ≥ 10−11 M⊙ yr−1 after opening a gap. Among those accreting transition disks, half display accretion rates higher than 5.0 × 10−10 M⊙ yr−1. The dust component in these disks is distributed in two regions: in a compact inner disk inside the dead zone, and in a ring at the outer edge of the photoevaporative gap, which can be located between 20 and 100 AU. Our radiative transfer calculations show that the disk displays an inner disk and an outer ring in the millimeter continuum, a feature that resembles some of the observed transition disks. Conclusions. A disk model considering X-ray photoevaporative dispersal in combination with dead zones can explain several of the observed properties in transition disks, including the high accretion rates, the large gaps, and a long-lived inner disk at millimeter emission.

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Section: Discussionmentioning

confidence: 93%

Section: Introductionmentioning

confidence: 99%

Large gaps and high accretion rates in photoevaporative transition disks with a dead zone

Gárate

Delage

Stadler

et al. 2021

A&A

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“…Indeed, Rigliaco et al (2012) and others (e.g., Alcalá et al 2017) have shown that the combination of accretion luminosity measured with a significant number of emission lines ( 5-6) leads to estimates of accretion luminosity with small uncertainties (∼0.2-0.3 dex) and good agreement with the values obtained from the fit of the Balmer continuum. Comparing accretion luminosity determinations from lines at different wavelengths also provides a way to independently determine extinction (e.g., Pinilla et al 2021). However, it should be noted that only a proper inclusion of the impact of extinction and of veiling due to accretion at all stages of the spectral analysis overcomes the degeneracies between these parameters, and that the UV-excess is key for determining the excess due to accretion (e.g., Manara et al 2013a;Herczeg and Hillenbrand 2014).…”

Section: Spectral Types Stellar and Accretion Luminositymentioning

confidence: 99%

Demographics of young stars and their protoplanetary disks: lessons learned on disk evolution and its connection to planet formation

Manara¹,

Ansdell²,

Rosotti³

et al. 2022

Preprint

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Since Protostars and Planets VI (PPVI), our knowledge of the global properties of protoplanetary and debris disks, as well as of young stars, has dramatically improved. At the time of PPVI, mm-observations and optical to near-infrared spectroscopic surveys were largely limited to the Taurus star-forming region, especially of its most massive disk and stellar population. Now, near-complete surveys of multiple star-forming regions cover both spectroscopy of young stars and mm interferometry of their protoplanetary disks. This provides an unprecedented statistical sample of stellar masses and mass accretion rates, as well as disk masses and radii, for almost 1000 young stellar objects within 300 pc from us, while also sampling different evolutionary stages, ages, and environments. At the same time, surveys of debris disks are revealing the bulk properties of this class of more evolved objects. This chapter reviews the statistics of these measured global star and disk properties and discusses their constraints on theoretical models describing global disk evolution. Our comparisons of observations to theoretical model predictions extends beyond the traditional viscous evolution framework to include analytical descriptions of magnetic wind effects. Finally, we discuss how recent observational results can provide a framework for models of planet population synthesis and planet formation.

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“…1. ALMA observation in Band 7 (0.9 mm) of the system CIDA 1 (Pinilla et al 2021), with a beam size of 0.050 × 0.034 (FWHM) indicated by the white ellipse in the bottom left corner.…”

Section: Introductionmentioning

confidence: 99%

“…In this work, we aim to reproduce the observed dust and gas emission of the disk, to evaluate whether the presence of the observed substructures can be explained by the interactions of the disk with an embedded planet. While Pinilla et al (2021) assume an analytical gap shape, we obtain it from hydrodynamical simulations. We employ full 3D modeling to take into account the dynamical and radiative aspects of the disk, along with the effects introduced by interferometric observations with ALMA.…”

Section: Introductionmentioning

confidence: 99%

A giant planet shaping the disk around the very low mass star CIDA 1

Curone,

Izquierdo,

Testi

et al. 2022

Preprint

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Context. Exoplanetary research has provided us with exciting discoveries of planets around very low mass (VLM) stars (0.08 M M 0.3 M ; e.g., TRAPPIST-1 and Proxima Centauri). However, current theoretical models still strive to explain planet formation in these conditions and do not predict the development of giant planets. Recent high-resolution observations from the Atacama Large Millimeter/submillimeter Array (ALMA) of the disk around CIDA 1, a VLM star in Taurus, show substructures hinting at the presence of a massive planet. Aims. We aim to reproduce the dust ring of CIDA 1, observed in the dust continuum emission in ALMA Band 7 (0.9 mm) and Band 4 (2.1 mm), along with its 12 CO (J = 3 − 2) and 13 CO (J = 3 − 2) channel maps, assuming the structures are shaped by the interaction of the disk with a massive planet. We seek to retrieve the mass and position of the putative planet, through a global simulation assessing planet-disk interaction to quantitatively reproduce protoplanetary disk observations of both dust and gas emission in a self-consistent way. Methods. We model the protoplanetary disk with a set of hydrodynamical simulations, hosting an embedded planet with a starting mass between 0.1 and 4.0 M Jup initially located at a distance between 9 and 11 au from the central star. We compute the dust and gas emission using radiative transfer simulations, and, finally, we obtain the synthetic observations treating the images as the actual ALMA observations. Results. Our models indicate that a planet with a minimum mass of ∼ 1.4 M Jup orbiting at a distance of ∼ 9 − 10 au can explain the morphology and location of the observed dust ring at Band 7 and Band 4. We match the flux of the dust emission observation with a dust-to-gas mass ratio in the disk of ∼ 10 −2 . We are able to reproduce the low spectral index (∼ 2) observed where the dust ring is detected, with a ∼ 40 − 50% fraction of optically thick emission. Assuming a 12 CO abundance of 5 × 10 −5 and a 13 CO abundance 70 times lower, our synthetic images reproduce the morphology of the 12 CO (J = 3 − 2) and 13 CO (J = 3 − 2) observed channel maps where the cloud absorption allowed a detection. From our simulations, we estimate that a stellar mass M = 0.2 M and a systemic velocity sys = 6.25 km s −1 are needed to reproduce the gas rotation as retrieved from molecular line observations. Applying an empirical relation between planet mass and gap width in the dust, we predict a maximum planet mass of ∼ 4 − 8 M Jup . Conclusions. Our results suggest the presence of a massive planet orbiting CIDA 1, thus challenging our understanding of planet formation around VLM stars.

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A bright inner disk and structures in the transition disk around the very low-mass star CIDA 1

Cited by 26 publications

References 80 publications

Large gaps and high accretion rates in photoevaporative transition disks with a dead zone

Large gaps and high accretion rates in photoevaporative transition disks with a dead zone

Demographics of young stars and their protoplanetary disks: lessons learned on disk evolution and its connection to planet formation

A giant planet shaping the disk around the very low mass star CIDA 1

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