SPHERE dynamical and spectroscopic characterization of HD 142527B

Claudi, R.; Maire, Anne-Lise; Mesa, D.; Cheetham, A.; Fontanive, C.; Gratton, R.; Zurlo, A.; Avenhaus, H.; Bhowmik, T.; Biller, Beth; Boccaletti, A.; Bonavita, M.; Bonnefoy, M.; Cascone, E.; Chauvin, G.; Delboulbé, A.; Desidera, S.; D’Orazi, V.; Feautrier, Philippe; Feldt, M.; Dotti, Francesco Flammini; Girard, J.; Giro, E.; Janson, Markus; Hagelberg, J.; Keppler, M.; Kopytova, T.; Lacour, S.; Lagrange, Anne-Marie; Langlois, M.; Lannier, J.; Coroller, H. Le; Ménard, F.; Messina, S.; Meyer, M.; Millward, M.; Olofsson, J.; Pavlov, A.; Peretti, S.; Perrot, C.; Pinte, C.; Pragt, J.; Ramos, J.; Rochat, S.; Rodet, L.; Roelfsema, R.; Rouan, D.; Salter, G.; Schmidt, Thomas; Sissa, E.; Thébault, P.; Udry, S.; Vigan, A.

doi:10.1051/0004-6361/201833990

Cited by 50 publications

(69 citation statements)

References 82 publications

(133 reference statements)

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“…Price et al (2018) suggest that the shape of the disk has been carved by the interaction with the binary. Claudi et al (2019) retrieved the orbit for the companion using all the astrometric data available to date, they found a period of P = 35-137 yr; an inclination of i = 121-130 deg, and two families of values for the eccentricity: 0.2-0.45 and 0.45-0.7. In our data, the astrometry for the stellar companion is as follows: separation of 63.0 ± 1.5 mas and PA 96.4 ± 1 deg, which is consistent with the previous results from Cugno et al (2019) and Claudi et al (2019).…”

Section: Hd 142527mentioning

confidence: 99%

The widest Hα survey of accreting protoplanets around nearby transition disks

Zurlo

Cugno

Montesinos

et al. 2020

A&A

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Context. The mechanisms of planet formation are still under debate. We know little about how planets form, even if more than 4000 exoplanets have been detected to date. Recent investigations target the cot of newly born planets: the protoplanetary disk. At the first stages of their life, exoplanets still accrete material from the gas-rich disk in which they are embedded. Transitional disks are indeed disks that show peculiarities, such as gaps, spiral arms, and rings, which can be connected to the presence of substellar companions. Aims. To investigate what is responsible for these features, we selected all the known transitional disks in the solar neighborhood (<200 pc) that are visible from the southern hemisphere. We conducted a survey of 11 transitional disks (TDs) with the SPHERE instrument at the Very Large Telescope. This is the largest Hα survey that has been conducted so far to look for protoplanets. The observations were performed with the Hα filter of ZIMPOL in order to target protoplanets that are still in the accretion stage. All the selected targets are very young stars, less than 20 Myr, and show low extinction in the visible. Methods. We reduced the ZIMPOL pupil stabilized data by applying the method of the angular spectral differential imaging (ASDI), which combines both techniques. The datacubes are composed of the Cnt_Hα and the narrow band filter Hα, which are taken simultaneously to permit the suppression of the speckle pattern. The principal component analysis (PCA) method was employed for the reduction of the data. For each dataset, we derived the 5σ contrast limit and converted it in upper limits on the accretion luminosity. Results. We do not detect any new accreting substellar companions around the targeted transition disks down to an average contrast of 12 magnitudes at 0 . 2 from the central star. We have recovered the signal of the accreting M star companion around the star HD 142527. We have detected and resolved, for the first time in visible light, the quadruple system HD 98800. For every other system, we can exclude the presence of massive actively accreting companions, assuming that the accretion is not episodic and that the extinction is negligible. The mean accretion luminosity limit is 10 −6 L at a separation of 0 . 2 from the host.

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Section: Hd 142527mentioning

confidence: 99%

The widest Hα survey of accreting protoplanets around nearby transition disks

Zurlo

Cugno

Montesinos

et al. 2020

A&A

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“…Alternatively, secular precession resonances can lead to large misalignments between the inner and outer disks if the companion is quite massive and no viscosity is considered (0.1-0.01 M , Owen & Lai 2017). In the case of the transition disk HD 142527, that shows two shadows in scattered light images, a stellar companion was detected (0.2-0.3 M , Biller et al 2012), likely on an inclined and eccentric orbit (Lacour et al 2016;Claudi et al 2019), which would explain the misalignment of the inner disk (Price et al 2018). However, apart from HD 142527, none of the disks with scattered light shadows are known to host a massive inclined companion.…”

Section: Origin Of the Misalignmentsmentioning

confidence: 99%

Shadowing and multiple rings in the protoplanetary disk of HD 139614

Muro-Arena

Benisty

Ginski

et al. 2020

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Context. Shadows in scattered light images of protoplanetary disks are a common feature and support the presence of warps or misalignments between disk regions. These warps are possibly due to an inclined (sub-)stellar companion embedded in the disk. Aims. We study the morphology of the protoplanetary disk around the Herbig Ae star HD 139614 based on the first scattered light observations of this disk, which we model with the radiative transfer code MCMax3D. Methods. We obtained J-and H-band observations in polarized scattered light with VLT/SPHERE that show strong azimuthal asymmetries. In the outer disk, beyond ∼30 au, a broad shadow spans a range of ∼240 deg in position angle, in the East. A bright ring at ∼16 au also shows an azimuthally asymmetric brightness, with the faintest side roughly coincidental with the brightest region of the outer disk. Additionally, two arcs are detected at ∼34 au and ∼50 au. We created a simple 4-zone approximation to a warped disk model of HD 139614 in order to qualitatively reproduce these features. The location and misalignment of the disk components were constrained from the shape and location of the shadows they cast. Results. We find that the shadow on the outer disk covers a range of position angle too wide to be explained by a single inner misaligned component. Our model requires a minimum of two separate misaligned zones -or a continuously warped region -to cast this broad shadow on the outer disk. A small misalignment of ∼4 • between adjacent components can reproduce most of the observed shadow features. Conclusions. Multiple misaligned disk zones, potentially mimicing a warp, can explain the observed broad shadows in the HD 139614 disk. A planetary mass companion in the disk, located on an inclined orbit, could be responsible for such a feature and for the dust depleted gap responsible for a dip in the SED.

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“…The stellar masses in HD 142527 are 1.8 M (Gaia Collaboration et al 2016) and 0.4 M (Christiaens et al 2018), so it is an unequal-mass binary. Further studies focused on the companion's orbital motion (Lacour et al 2016;Claudi et al 2019) indicating that the binary is eccentric and likely inclined with respect with the disc. Based on these constraints, Price et al (2018b) presented a consistent hydrodynamical model of HD 142527 where the CBD is periodically perturbed by the inner binary.…”

Section: Introductionmentioning

confidence: 99%

Dusty clumps in circumbinary discs

Poblete

Cuello

Cuadra

2019

Monthly Notices of the Royal Astronomical Society

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Recent observations have revealed that protoplanetary discs often exhibit cavities and azimuthal asymmetries such as dust traps and clumps. The presence of a stellar binary system in the inner disc regions has been proposed to explain the formation of these structures. Here, we study the dust and gas dynamics in circumbinary discs around eccentric and inclined binaries. This is done through two-fluid simulations of circumbinary discs, considering different values of the binary eccentricity and inclination. We find that two kinds of dust structures can form in the disc: a single horseshoe-shaped clump, on top of a similar gaseous over-density; or numerous clumps, distributed along the inner disc rim. The latter features form through the complex interplay between the dust particles and the gaseous spirals caused by the binary. All these clumps survive between one and several tens of orbital periods at the feature location. We show that their evolution strongly depends on the gas-dust coupling and the binary parameters. Interestingly, these asymmetric features could in principle be used to infer or constrain the orbital parameters of a stellar companion -potentially unseen -inside the inner disc cavity. Finally, we apply our findings to the disc around AB Aurigae.

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SPHERE dynamical and spectroscopic characterization of HD 142527B

Cited by 50 publications

References 82 publications

The widest Hα survey of accreting protoplanets around nearby transition disks

The widest Hα survey of accreting protoplanets around nearby transition disks

Shadowing and multiple rings in the protoplanetary disk of HD 139614

Dusty clumps in circumbinary discs

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