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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 731518.0, MPI für Astronomie / Publikationen_mpia
Constraining the movement of the spiral features and the locations of planetary bodies within the AB Aur system
Authors:Lomax, J. R.; Wisniewski, J. P.; Grady, C. A.; McElwain, M. W.; Hashimoto, J.; Kudo, T.; Kusakabe, N.; Okamoto, Y. K.; Fukagawa, M.; Abe, L.; Brandner, W.; Brandt, T. D.; Carson, J. C.; Currie, T. M.; Egner, S.; Feldt, M.; Goto, M.; Guyon, O.; Hayano, Y.; Hayashi, M.; Hayashi, S. S.; Henning, T.; Hodapp, K. W.; Inoue, A.; Ishii, M.; Iye, M.; Janson, M.; Kandori, R.; Knapp, G. R.; Kuzuhara, M.; Kwon, J.; Matsuo, T.; Mayama, S.; Miyama, S.; Momose, M.; Morino, J.-I.; Moro-Martin, A.; Nishimura, T.; Pyo, T.-S.; Schneider, G. H.; Serabyn, E.; Sitko, M. L.; Suenaga, T.; Suto, H.; Suzuki, R.; Takahashi, Y. H.; Takami, M.; Takato, N.; Terada, H.; Thalmann, C.; Tomono, D.; Turner, E. L.; Watanabe, M.; Yamada, T.; Takami, H.; Usuda, T.; Tamura, M.
Date of Publication (YYYY-MM-DD):2016
Title of Journal:The Astrophysical Journal
Volume:828
Issue / Number:1
Start Page:id. 2 (8 pp)
Audience:Not Specified
Abstract / Description:We present a new analysis of multi-epoch, H-band, scattered light images of the AB Aur system. We use a Monte Carlo radiative transfer code to simultaneously model the system’s spectral energy distribution (SED) and H-band polarized intensity (PI) imagery. We find that a disk-dominated model, as opposed to one that is envelope-dominated, can plausibly reproduce AB Aur’s SED and near-IR imagery. This is consistent with previous modeling attempts presented in the literature and supports the idea that at least a subset of AB Aur’s spirals originate within the disk. In light of this, we also analyzed the movement of spiral structures in multi-epoch H-band total light and PI imagery of the disk. We detect no significant rotation or change in spatial location of the spiral structures in these data, which span a 5.8-year baseline. If such structures are caused by disk–planet interactions, the lack of observed rotation constrains the location of the orbit of planetary perturbers to be >47 au.
Free Keywords:planet–disk interactions; planetary systems; protoplanetary disks; radiative transfer; stars: individual: AB Aur; stars: pre-main sequence
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0004-637X %R 10.3847/0004-637X/828/1/2
URL:http://adsabs.harvard.edu/abs/2016ApJ...828....2L
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