SPIRAL ARMS IN THE DISK OF HD 142527 FROM CO EMISSION LINES WITH ALMA

In view of both the size of its gap and the previously reported asymmetries and near-infrared spiral arms, the transition disk of the Herbig Fe star HD 142527 constitutes a remarkable case study. This paper focuses on the morphology of the outer disk through ALMA observations of super(12)CO J = 2-1,...

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Bibliographic Details
Published in:Astrophysical journal. Letters 2014-04, Vol.785 (1), p.1-5
Main Authors: Christiaens, V, Casassus, S, Perez, S, van der Plas, G, Menard, F
Format: Article
Language:English
Subjects:
APPROXIMATIONS
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
ASYMMETRY
Aérospatiale, astronomie & astrophysique
BRIGHTNESS
CARBON MONOXIDE
COMPARATIVE EVALUATIONS
DENSITY
Disks
disques protoplanétaires
EXCITATION
GRAVITATIONAL INSTABILITY
HERBIG-HARO OBJECTS
interactions planètes-disque
Loci
Maxima
MORPHOLOGY
NEAR INFRARED RADIATION
Physical, chemical, mathematical & earth Sciences
Physique, chimie, mathématiques & sciences de la terre
planet-disk interactions
PLANETS
protoplanetary disks
PROTOPLANETS
SOUND WAVES
Space science, astronomy & astrophysics
Spirals
STARS
stars: individual (HD 142527)
étoiles: individuelle (HD 142527)
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Summary:In view of both the size of its gap and the previously reported asymmetries and near-infrared spiral arms, the transition disk of the Herbig Fe star HD 142527 constitutes a remarkable case study. This paper focuses on the morphology of the outer disk through ALMA observations of super(12)CO J = 2-1, super(12)CO J = 3-2, and super(13)CO J = 2-1. Both super(12)CO J = 2-1 and super(12)CO J = 3-2 show spiral features of different sizes. The innermost spiral arm (S1) is a radio counterpart of the first near-infrared spiral observed by Fukagawa, but it is shifted radially outward. However, the most conspicuous CO spiral arm (S2) lies at the outskirts of the disk and has not been detected before. It corresponds to a cold density structure, with both brightness and excitation temperatures of order 13+ or -2 K and conspicuous in the super(12)CO J = 2-1 peak-intensity map, but faint in super(12)CO J = 3-2. There is also a faint counterarm (S3), at a point-symmetric location of S2 with respect to the star. These three spirals are modeled separately with two different formulae that approximate the loci of density maxima in acoustic waves due to embedded planets. S1 could be fit relatively well with these formulae, compared to S2 and S3. Alternative scenarios such as gravitational instability or external tidal interaction are discussed. The impact of channelization on spectrally and spatially resolved peak intensity maps is also briefly addressed.
ISSN:2041-8205
2041-8213
2041-8213
DOI:10.1088/2041-8205/785/1/L12