Two accreting protoplanets around the young star PDS 70

Haffert, Sebastiaan Y.; Bohn, A. J.; Boer, J. de; Snellen, I. A. G.; Brinchmann, Jarle; Girard, J.; Keller, Christoph U.; Bacon, Roland

doi:10.1038/s41550-019-0780-5

Cited by 477 publications

(617 citation statements)

References 38 publications

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“…For instance, part of the Brγ emission could arise from an accreting planet orbiting close to the star. Hydrogen emission has been directly detected in the circumstellar disks of young systems at the location of wide-orbit planets (e.g., Haffert et al 2019). Compact close-in planetary systems, such as those revealed by Kepler with orbital periods of a few days (e.g., Winn et al 2018), could conceivably yield these kinds of signatures when still embedded in the inner disk.…”

Section: Discussionmentioning

confidence: 99%

Probing the magnetospheric accretion region of the young pre-transitional disk system DoAr 44 using VLTI/GRAVITY

Bouvier

Perraut

Bouquin

et al. 2020

A&A

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Context. Young stellar objects are thought to accrete material from their circumstellar disks through their strong stellar magnetospheres. Aims. We aim to directly probe the magnetospheric accretion region on a scale of a few 0.01 au in a young stellar system using long-baseline optical interferometry. Methods. We observed the pre-transitional disk system DoAr 44 with VLTI/GRAVITY on two consecutive nights in the K-band. We computed interferometric visibilities and phases in the continuum and in the Brγ line in order to constrain the extent and geometry of the emitting regions. Results. We resolve the continuum emission of the inner dusty disk and measure a half-flux radius of 0.14 au. We derive the inclination and position angle of the inner disk, which provides direct evidence that the inner and outer disks are misaligned in this pre-transitional system. This may account for the shadows previously detected in the outer disk. We show that Brγ emission arises from an even more compact region than the inner disk, with an upper limit of 0.047 au (∼5 R ). Differential phase measurements between the Brγ line and the continuum allow us to measure the astrometric displacement of the Brγ line-emitting region relative to the continuum on a scale of a few tens of microarcsec, corresponding to a fraction of the stellar radius. Conclusions. Our results can be accounted for by a simple geometric model where the Brγ line emission arises from a compact region interior to the inner disk edge, on a scale of a few stellar radii, fully consistent with the concept of magnetospheric accretion process in low-mass young stellar systems.

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Section: Discussionmentioning

confidence: 99%

Probing the magnetospheric accretion region of the young pre-transitional disk system DoAr 44 using VLTI/GRAVITY

Bouvier

Perraut

Bouquin

et al. 2020

A&A

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“…tions of circumplanetary disks around PDS 70 b and c (73 ± 19 µJy and 106 ± 19 µJy; Isella et al 2019), with planet masses adopted from Keppler et al (2018) and Haffert et al (2019). Disk fluxes of stars and brown dwarfs are compiled from millimeter studies of starforming regions, including Taurus (Andrews et al 2013;Ricci et al 2014;Ward-Duong et al 2018), Chamaeleon I (Pascucci et al 2016;Long et al 2018), Lupus (Ansdell et al 2016;Sanchis et al 2020), and Upper Scorpius 1 (Barenfeld et al 2016;van der Plas et al 2016).…”

Section: Disk Flux-host Mass Relationshipmentioning

confidence: 99%

ALMA 0.88 mm Survey of Disks around Planetary-mass Companions

Bowler

Sheehan

et al. 2020

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Characterizing the physical properties and compositions of circumplanetary disks can provide important insights into the formation of giant planets and satellites. We report ALMA 0.88 mm (Band 7) continuum observations of six planetary-mass (10-20 M Jup ) companions: CT Cha b, 1RXS 1609 b, ROXs 12 b, ROXs 42B b, DH Tau b, and FU Tau b. No continuum sources are detected at the locations of the companions down to 3σ limits of 120-210 µJy. Given these non-detections, it is not clear whether disks around planetary-mass companions indeed follow the disk flux-host mass trend in the stellar regime. The faint radio brightness of these companion disks may result from a combination of fast radial drift and a lack of dust traps. Alternatively, as disks in binary systems are known to have significantly lower millimeter fluxes due to tidal interactions, these companion disks may instead follow the relationship of moderate-separation binary stars. This scenario can be tested with sensitive continuum imaging at rms levels of 10 µJy.

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“…A good example of robustly detected accreting planets at tens of au from a central star is the PDS 70 planetary system. This system includes a weakly accreting young star (spectral type of K7, mass of 0.8 M ⊙ , accretion rate of 6 × 10 −11 M ⊙ yr −1 , age of 5 Myr, distance of 113 pc; Pecaut & Mamajek 2016;Keppler et al 2019;Haffert et al 2019;Müller et al 2018;Gaia Collaboration et al 2018) associated with two planetary-mass companions (Haffert et al 2019;Isella et al 2019;Christiaens et al 2019a,b;Keppler et al 2018;Müller et al 2018;Wagner et al 2018). Aoyama & Ikoma (2019) estimated that PDS 70b's mass and mass accretion rate are ∼12 M Jup and ∼4 × 10 −8 M Jup yr −1 , respectively, while the values for PDS 70c are ∼10 M Jup and ∼1 × 10 −8 M Jup yr −1 .…”

Section: Introductionmentioning

confidence: 99%

“…In this paper, we revisit the accretion properties of PDS 70b by re-analyzing archive data used in Haffert et al (2019). We aim to estimate the physical quantities related to planetary mass accretion with the help of the theoretical study by Aoyama & Ikoma (2019).…”

Section: Introductionmentioning

confidence: 99%

Accretion Properties of PDS 70b with MUSE*

et al. 2020

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We report a new evaluation of the accretion properties of PDS 70b obtained with VLT/MUSE. The main difference from previous studies in Haffert et al. (2019) and Aoyama & Ikoma (2019) is in the mass accretion rate. Simultaneous multiple line observations, such as Hα and Hβ, can better constrain the physical properties of an accreting planet. While we clearly detected Hα emissions from PDS 70b, no Hβ emissions were detected. We estimate the line flux of Hβ with a 3-σ upper limit to be 2.3 × 10 −16 erg s −1 cm −2 . The flux ratio F Hβ /F Hα for PDS 70b is < 0.28. Numerical investigations by Aoyama et al. (2018) suggest that F Hβ /F Hα should be close to unity if the extinction is negligible. We attribute the reduction of the flux ratio to the extinction, and estimate the extinction of Hα (A Hα ) for PDS 70b to be > 2.0 mag using the interstellar extinction value. By combining with the Hα linewidth and the dereddening line luminosity of Hα, we derive the PDS 70b mass accretion rate to be 5 × 10 −7 M Jup yr −1 . The PDS 70b mass accretion rate is an order of magnitude larger than that of PDS 70. We found that the filling factor f f (the fractional area of the planetary surface emitting Hα) is 0.01, which is similar to the typical stellar value. The small value of f f indicates that the Hα emitting areas are localized at the surface of PDS 70b.

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Two accreting protoplanets around the young star PDS 70

Cited by 477 publications

References 38 publications

Probing the magnetospheric accretion region of the young pre-transitional disk system DoAr 44 using VLTI/GRAVITY

Probing the magnetospheric accretion region of the young pre-transitional disk system DoAr 44 using VLTI/GRAVITY

ALMA 0.88 mm Survey of Disks around Planetary-mass Companions

Accretion Properties of PDS 70b with MUSE*

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