ASPITZERMIPS STUDY OF 2.5-2.0M☉STARS IN SCORPIUS-CENTAURUS

Chen, Christine; Pecaut, Mark J.; Mamajek, Eric E.; Su, K. Y. L.; Bitner, Martin A.

doi:10.1088/0004-637x/756/2/133

Cited by 94 publications

(87 citation statements)

References 40 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We therefore focus on a sample of Herbig IMS within this volume, that is, Herbig sources within 200 pc that have spectral type F6 or earlier, M å >1.5 M e , and no known stellar companion within 5″. Table 2 compiles a list of sources from the literature meeting these criteria (Walker & Wolstencroft 1988;Malfait et al 1998;Vieira et al 2003;Erickson et al 2011;Chen et al 2012). Generally, these stars are identified by their association with star-forming regions or a reflection nebula and the presence of hydrogen emission lines (particularly Hα).…”

Section: A Volume-limited Sample Of Herbig Starsmentioning

confidence: 99%

Spiral Arms in Disks: Planets or Gravitational Instability?

Dong

Najita

Brittain

2018

ApJ

View full text Add to dashboard Cite

Spiral arm structures seen in scattered-light observations of protoplanetary disks can potentially serve as signposts of planetary companions. They can also lend unique insights into disk masses, which are critical in setting the mass budget for planet formation but are difficult to determine directly. A surprisingly high fraction of disks that have been well studied in scattered light have spiral arms of some kind (8/29), as do a high fraction (6/11) of wellstudied Herbig intermediate-mass stars (i.e., Herbig stars >1.5 M e ). Here we explore the origin of spiral arms in Herbig systems by studying their occurrence rates, disk properties, and stellar accretion rates. We find that two-arm spirals are more common in disks surrounding Herbig intermediate-mass stars than are directly imaged giant planet companions to mature A and B stars. If two-arm spirals are produced by such giant planets, this discrepancy suggests that giant planets are much fainter than predicted by hot-start models. In addition, the high stellar accretion rates of Herbig stars, if sustained over a reasonable fraction of their lifetimes, suggest that disk masses are much larger than inferred from their submillimeter continuum emission. As a result, gravitational instability is a possible explanation for multiarm spirals. Future observations can lend insights into the issues raised here.

show abstract

Section: A Volume-limited Sample Of Herbig Starsmentioning

confidence: 99%

Spiral Arms in Disks: Planets or Gravitational Instability?

Dong

Najita

Brittain

2018

ApJ

View full text Add to dashboard Cite

show abstract

“…The IR emission of HIP 73145 was first reported by Moór et al (2006) after a search through ISO and IRAS databases, establishing the presence of a debris disk in the system. Chen et al (2012) rably high excess. Moór et al (2015) presented Herschel observations of the object.…”

Section: Introductionmentioning

confidence: 97%

SPHERE/SHINE reveals concentric rings in the debris disk of HIP 73145

Feldt

Olofsson

Boccaletti

et al. 2017

A&A

View full text Add to dashboard Cite

Context. Debris disks correspond to the final evolutionary stage of circumstellar disks around young stars. Gas-deprived structures seen in debris disks are normally, but not always, attributed to dynamical interactions in young planetary systems. Aims. The debris disk of HIP 73145 has been detected in scattered light in the near-IR, and at far-IR wavelengths before, but no substructure has been seen so far. Detection of such substructures in combination with detailed modeling can hint at the presence of perturbing planetary bodies, or reveal other mechanisms acting to replenish gas and dust reservoirs and forming structures such as spirals or rings. Methods. We obtained multiwavelength images with SPHERE in the near-IR in the H2 and H3 bands with the IRDIS camera and a 0.95-1.35 µm spectral cube with the IFS. Data were acquired in pupil-tracking mode, thus allowing for angular differential imaging. The SPHERE standard suite of angular differential imaging algorithms was applied. ALMA Band 6 observations complement the SPHERE data. Results. We detect a bright ring of scattered light plus some secondary structures inside, at least one of them forming a secondary, concentric ring with the first. This is the first detection of this disk in total-intensity scattered light. A second object is detected in the field at high contrast but concluded to be a background star. Forward modeling yields information on the primary parameters of the disk and confirms that the detected substructures are not due to the data analysis approach, which sometimes leads to spurious structures. Conclusions. We detect a series of concentric rings in the disk around HIP 73145. This is one of the rare cases where multiple components are necessary to fit the SED and are also detected in scattered light. The presence of such ring structures somewhat questions the nature of the object as a pure debris disk, but the gas and dust content would presumably offer sufficient explanations for such structures to form.

show abstract

“…Its IR emission was discovered by the Infrared Astronomical Satellite (Moór et al 2006). Chen et al (2012) presented MIPS observations and showed that it is one of only four UCL/Lower Centaurus Crux A-type stars with L L 10 IR 3 * > -, comparable to β Pic. Recently, Hung et al (2015) resolved the debris disk around HD 131835 at 11.7 and 18.3 μm using Gemini/T-ReCS.…”

Section: Introductionmentioning

confidence: 99%