Complex Magnetospheric Accretion Flows in the Low Accretor CVSO 1335

Thanathibodee, Thanawuth; Calvet, Nuria; Muzerolle, James; Hernández, Ramiro Franco; Maucó, Karina

doi:10.3847/1538-4357/ab4127

Cited by 14 publications

(20 citation statements)

References 65 publications

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“…The environment of a CTTS can be more complex than a single accretion column in each hemisphere, with several components contributing to the line profile. Thanathibodee et al (2019) analyzed the accretion process of the CTTS CVSO 1335. The Hα and Hβ lines of this system present two redshifted absorptions, one close to the line center and another at high velocity.…”

Section: New Environment Configurationmentioning

confidence: 99%

“…A Keplerian period of 6.0 days would locate the base of the inner accretion column at ∼7.3 R * (∼0.071 au) from the star, that is, slightly below the corotation radius. As pointed out by Thanathibodee et al (2019), a configuration with two accretion flows may still be a simplification of a more complex accretion topology governed by different magnetic field components.…”

Section: New Environment Configurationmentioning

confidence: 99%

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Star-disk interaction in the T Tauri star V2129 Ophiuchi: An evolving accretion-ejection structure

Sousa¹,

Bouvier²,

Alencar³

et al. 2021

A&A

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Context. Classical T Tauri stars are young low-mass systems still accreting material from their disks. These systems are dynamic on timescales of hours to years. The observed variability can help us infer the physical processes that occur in the circumstellar environment. Aims. In this work, we aim at understanding the dynamics of the magnetic interaction between the star and the inner accretion disk in young stellar objects. We present the case of the young stellar system V2129 Oph, which is a well-known T Tauri star with a K5 spectral type that is located in the ρ Oph star formation region at a distance of 130 ± 1 pc. Methods. We performed a time series analysis of this star using high-resolution spectroscopic data at optical wavelengths from CFHT/ESPaDOnS and ESO/HARPS and at infrared wavelengths from CFHT/SPIRou. We also obtained simultaneous photometry from REM and ASAS-SN. The new data sets allowed us to characterize the accretion-ejection structure in this system and to investigate its evolution over a timescale of a decade via comparisons to previous observational campaigns. Results. We measure radial velocity variations and recover a stellar rotation period of 6.53 days. However, we do not recover the stellar rotation period in the variability of various circumstellar lines, such as Hα and Hβ in the optical or HeI 10830 Å and Paβ in the infrared. Instead, we show that the optical and infrared line profile variations are consistent with a magnetospheric accretion scenario that shows variability with a period of about 6.0 days, shorter than the stellar rotation period. Additionally, we find a period of 8.5 days in Hα and Hβ lines, probably due to a structure located beyond the corotation radius, at a distance of ∼0.09 au. We investigate whether this could be accounted for by a wind component, twisted or multiple accretion funnel flows, or an external disturbance in the inner disk. Conclusions. We conclude that the dynamics of the accretion-ejection process can vary significantly on a timescale of just a few years in this source, presumably reflecting the evolving magnetic field topology at the stellar surface.

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Section: New Environment Configurationmentioning

confidence: 99%

Section: New Environment Configurationmentioning

confidence: 99%

Star-disk interaction in the T Tauri star V2129 Ophiuchi: An evolving accretion-ejection structure

Sousa¹,

Bouvier²,

Alencar³

et al. 2021

A&A

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“…C.1 in Manara et al 2016), which translates into an upper limit of −10.34 (rescaled to the Gaia DR2 distance, Manara et al 2019) for logṀ acc (M yr −1 ), and considered it as a doubtful accretor, at a level compatible with the typical chromospheric emission line activity. We note that the profiles of the Balmer lines and Ca ii K line are all rather narrow and symmetric (see .1) with no sign of redshifted absorption components or reversals that are frequently observed in the line profiles of accretors (e.g., Thanathibodee et al 2019;de Albuquerque et al 2020). The only notable feature is a wing emission, which is stronger on the red side of the Hβ and Hγ profiles and extends up to 200 km s −1 .…”

Section: Stellar Parameters and Accretion Diagnosticsmentioning

confidence: 66%

“…A further category of objects has recently emerged with apparently very little or no evidence for accretion in optical (λ > 3400 Å) spectra, but with the near-IR (NIR) emission characteristic of optically thick dust in the inner (few AU) regions of the disk, so that their spectral energy distribution resembles that of class II sources (e.g., Wahhaj et al 2010;Alcalá et al 2019;Thanathibodee et al 2019). The existence of such objects might be explained by slightly different timescales for the decline of disk and accretion processes in young stars (e.g., Fedele et al 2010).…”

Section: Introductionmentioning

confidence: 99%

“…Weak accretion is in general difficult to detect in the region of the Balmer jump. Other diagnostics such as modeling of the Hα line profile (e.g., Espaillat et al 2008;Thanathibodee et al 2019) and/or measures of excess emission in near-UV or far-UV spectra (e.g., Alcalá et al 2019, and references therein) are therefore necessary in these cases of very low accretion rates.…”

Section: Introductionmentioning

confidence: 99%

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ISO-ChaI 52: a weakly accreting young stellar object with a dipper light curve

Frasca

Manara

Alcalá

et al. 2020

A&A

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We report the discovery of periodic dips in the multiband light curve of ISO-ChaI 52, a young stellar object in the Chamaeleon I dark cloud. This is one of the peculiar objects that display very low or negligible accretion in their UV continuum and spectral lines, although they present a remarkable infrared excess emission characteristic of optically thick circumstellar disks. We have analyzed a spectrum obtained at the Very Large Telescope with the X-shooter spectrograph with the tool ROTFIT to determine the stellar parameters. The latter, along with photometry from our campaign with the Rapid Eye Mount telescope and from the literature, have allowed us to model the spectral energy distribution and to estimate the size and temperature of the inner and outer disk. Based on the rotational period of the star-disk system of 3.45 days, we estimate a disk inclination of 36°. The depth of the dips in different bands has been used to gain information about the occulting material. A single extinction law is not able to fit the observed behavior, while a two-component model of a disk warp composed of a dense region with a gray extinction and an upper layer with an extinction as in the interstellar medium provides a better fit to the data.

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PENELLOPE: The ESO data legacy program to complement the Hubble UV Legacy Library of Young Stars (ULLYSES)

Manara

Frasca

Venuti

et al. 2021

A&A

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The evolution of young stars and disks is driven by the interplay of several processes, notably the accretion and ejection of material. These processes, critical to correctly describe the conditions of planet formation, are best probed spectroscopically. Between 2020 and 2022, about 500orbits of the Hubble Space Telescope (HST) are being devoted in to the ULLYSES public survey of about 70 low-mass (M⋆ ≤ 2 M⊙) young (age < 10 Myr) stars at UV wavelengths. Here, we present the PENELLOPE Large Program carried out with the ESO Very Large Telescope (VLT) with the aim of acquiring, contemporaneously to the HST, optical ESPRESSO/UVES high-resolution spectra for the purpose of investigating the kinematics of the emitting gas, along with UV-to-NIR X-shooter medium-resolution flux-calibrated spectra to provide the fundamental parameters that HST data alone cannot provide, such as extinction and stellar properties. The data obtained by PENELLOPE have no proprietary time and the fully reduced spectra are being made available to the whole community. Here, we describe the data and the first scientific analysis of the accretion properties for the sample of 13 targets located in the Orion OB1 association and in the σ-Orionis cluster, observed in November–December 2020. We find that the accretion rates are in line with those observed previously in similarly young star-forming regions, with a variability on a timescale of days (≲3). The comparison of the fits to the continuum excess emission obtained with a slab model on the X-shooter spectra and the HST/STIS spectra shows a shortcoming in the X-shooter estimates of ≲10%, which is well within the assumed uncertainty. Its origin can be either due to an erroneous UV extinction curve or to the simplicity of the modeling and, thus, this question will form the basis of the investigation undertaken over the course of the PENELLOPE program. The combined ULLYSES and PENELLOPE data will be key in attaining a better understanding of the accretion and ejection mechanisms in young stars.

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Complex Magnetospheric Accretion Flows in the Low Accretor CVSO 1335

Cited by 14 publications

References 65 publications

Star-disk interaction in the T Tauri star V2129 Ophiuchi: An evolving accretion-ejection structure

Star-disk interaction in the T Tauri star V2129 Ophiuchi: An evolving accretion-ejection structure

ISO-ChaI 52: a weakly accreting young stellar object with a dipper light curve

PENELLOPE: The ESO data legacy program to complement the Hubble UV Legacy Library of Young Stars (ULLYSES)

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