A Multi-wavelength Analysis of Dust and Gas in the SR 24S Transition Disk

Pinilla, P.; Pérez, Laura; Andrews, Sean M.; Marel, Nienke van der; Dishoeck, E. F. van; Ataiee, Sareh; Benisty, M.; Birnstiel, T.; Juhász, A.; Natta, A.; Ricci, Luca; Testi, L.

doi:10.3847/1538-4357/aa6973

Cited by 38 publications

(34 citation statements)

References 69 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…Our model consists of a radially asymmetric Gaussian ring for the millimeter intensity (I(r))-that is, a Gaussian ring whose inner and outer widths (σ int and σ ext , respectively) can differ, such that where C is connected with the total flux of the disk as explained below. This profile was introduced in Pinilla et al (2017a) to fit the morphology of TDs and to mimic the effect of particle trapping in a radial pressure bump. From dust evolution models, it is expected that under the presence of a single pressure bump, the external width of the ring is larger than the internal because in the outer disk the particles take longer times to grow and drift toward the pressure maximum, creating a ring with an outer tail as discussed in Section 5.2.…”

Section: Data Analysis and Resultsmentioning

confidence: 99%

See 1 more Smart Citation

Homogeneous Analysis of the Dust Morphology of Transition Disks Observed with ALMA: Investigating Dust Trapping and the Origin of the Cavities

Pinilla

Tazzari

Pascucci

et al. 2018

ApJ

Self Cite

103

120

View full text Add to dashboard Cite

We analyze the dust morphology of 29 transition disks (TDs) observed with Atacama Large (sub-)Millimeter Array (ALMA) at (sub-)millimeter emission. We perform the analysis in the visibility plane to characterize the total flux, cavity size, and shape of the ring-like structure. First, we found that the M dust -M å relation is much flatter for TDs than the observed trends from samples of class II sources in different star-forming regions. This relation demonstrates that cavities open in high (dust) mass disks, independent of the stellar mass. The flatness of this relation contradicts the idea that TDs are a more evolved set of disks. Two potential reasons (not mutually exclusive) may explain this flat relation: the emission is optically thick or/and millimeter-sized particles are trapped in a pressure bump. Second, we discuss our results of the cavity size and ring width in the context of different physical processes for cavity formation. Photoevaporation is an unlikely leading mechanism for the origin of the cavity of any of the targets in the sample. Embedded giant planets or dead zones remain as potential explanations. Although both models predict correlations between the cavity size and the ring shape for different stellar and disk properties, we demonstrate that with the current resolution of the observations, it is difficult to obtain these correlations. Future observations with higher angular resolution observations of TDs with ALMA will help discern between different potential origins of cavities in TDs.

show abstract

Section: Data Analysis and Resultsmentioning

confidence: 99%

“…We used natural weighting for imaging (except for CIDA1 that uses uniform weighting; Pinilla et al 2018) to obtain as high sensitivity as possible. The final representative angular resolution is reported in Table 1.…”

Section: Observations and Sample Of Tdsmentioning

confidence: 99%

Homogeneous Analysis of the Dust Morphology of Transition Disks Observed with ALMA: Investigating Dust Trapping and the Origin of the Cavities

Pinilla

Tazzari

Pascucci

et al. 2018

ApJ

Self Cite

103

120

View full text Add to dashboard Cite

show abstract

“…The cycle 2 ALMA 1.3 mm continuum images of SR24 with a resolution of 0. ′′ 18 are reported by Pinilla et al (2017). The 1.3 mm continuum images of SR24S disk are described by ring-like emission with a central cavity.…”

Section: Andrewsmentioning

confidence: 92%

“…The 1.3 mm continuum images of SR24S disk are described by ring-like emission with a central cavity. Fitting by Pinilla et al (2017) showed that the PA, inclination, and peak radius for the SR24S disk are 24.30 • , 46.31 • , and 0. ′′ 3, respectively.…”

Section: Andrewsmentioning

confidence: 99%

Subaru Near-infrared Imaging Polarimetry of Misaligned Disks around the SR 24 Hierarchical Triple System*

Mayama

Pérez

Kusakabe

et al. 2019

View full text Add to dashboard Cite

The SR24 multi-star system hosts both circumprimary and circumsecondary disks, which are strongly misaligned with each other. The circumsecondary disk is circumbinary in nature. Interestingly, both disks are interacting, and they possibly rotate in opposite directions. To investigate the nature of this unique twin disk system, we present 0. ′′ 1 resolution near-infrared polarized intensity images of the circumstellar structures around SR24, obtained with HiCIAO mounted on the Subaru 8.2 m telescope. Both the circumprimary disk and the circumsecondary disk are resolved and have elongated features. While the position angle of the major axis and radius of the near-IR(NIR) polarization disk around SR24S are 55 • and 137 au, respectively, those around SR24N are 110 • and 34 au, respectively. With regard to overall morphology, the circumprimary disk around SR24S shows strong asymmetry, whereas the circumsecondary disk around SR24N shows relatively strong symmetry. Our NIR observations confirm the previous claim that the circumprimary and circumsecondary disks are misaligned from each other. Both the circumprimary and circumsecondary disks show similar structures in 12 CO observations in terms of its size and elongation direction. This consistency is because both NIR and 12 CO are tracing surface layers of the flared disks. As the radius of the polarization disk around SR24N is roughly consistent with the size of the outer Roche lobe, it is natural to interpret the polarization disk around SR24N as a circumbinary disk surrounding the SR24Nb-Nc system.

show abstract

“…However, some objects display a lack of emission in the near and mid-infrared (NIR and MIR) compared to full disk systems' spectral energy distributions (SEDs; e.g., Calvet et al 2005). These objects have a disk with a large dust-depleted inner cavity that has been spatially resolved with sub-mm interferometry for individual objects (e.g., Andrews et al 2011;van der Marel et al 2013van der Marel et al , 2016Canovas et al 2015;Pinilla et al 2015Pinilla et al , 2017Dong et al 2017;Sheehan & Eisner 2017) and are called transition disks because they are believed to undergo the process of disk clearing. Between the full disk and the transitional disk stage, pretransitional objects show a depletion in the MIR but still have an excess of NIR emission, likely caused by the presence of an inner disk interior to the cavity, forming a gapped disk (e.g., Espaillat et al 2014;Kraus et al 2017).…”

Section: Introductionmentioning

confidence: 99%

A Multi-instrument and Multi-wavelength High Angular Resolution Study of MWC 614: Quantum Heated Particles Inside the Disk Cavity*

Kluska

Kraus

Davies

et al. 2018

ApJ

View full text Add to dashboard Cite

High angular resolution observations of young stellar objects are required to study the inner astronomical units of protoplanetary disks in which the majority of planets form. As they evolve, gaps open up in the inner disk regions and the disks are fully dispersed within ∼10 Myr. MWC614 is a pretransitional object with a ∼10 au radius gap. We present a set of high angular resolution observations of this object including SPHERE/ZIMPOL polarimetric and coronagraphic images in the visible, Keck/NIRC2 near-infrared (NIR) aperture masking observations, and Very Large Telescope Interferometer (AMBER, MIDI, and PIONIER) and Center for High Angular Resolution Astronomy (CLASSIC and CLIMB) long-baseline interferometry at infrared wavelengths. We find that all the observations are compatible with an inclined disk (i∼55°at a position angle of ∼20°-30°). The mid-infrared data set confirms that the disk inner rim is at 12.3±0.4 au from the central star. We determined an upper mass limit of 0.34 M e for a companion inside the cavity. Within the cavity, the NIR emission, usually associated with the dust sublimation region, is unusually extended (∼10 au, 30 times larger than the theoretical sublimation radius) and indicates a high dust temperature (T∼1800 K). As a possible result of companion-induced dust segregation, quantum heated dust grains could explain the extended NIR emission with this high temperature. Our observations confirm the peculiar state of this object where the inner disk has already been accreted onto the star, exposing small particles inside the cavity to direct stellar radiation.

show abstract

A Multi-wavelength Analysis of Dust and Gas in the SR 24S Transition Disk

Cited by 38 publications

References 69 publications

Homogeneous Analysis of the Dust Morphology of Transition Disks Observed with ALMA: Investigating Dust Trapping and the Origin of the Cavities

Homogeneous Analysis of the Dust Morphology of Transition Disks Observed with ALMA: Investigating Dust Trapping and the Origin of the Cavities

Subaru Near-infrared Imaging Polarimetry of Misaligned Disks around the SR 24 Hierarchical Triple System*

A Multi-instrument and Multi-wavelength High Angular Resolution Study of MWC 614: Quantum Heated Particles Inside the Disk Cavity*

Contact Info

Product

Resources

About