Please note that eDoc will be permanently shut down in the first quarter of 2021!      Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Home
Search
Quick Search
Advanced
Fulltext
Browse
Collections
Persons
My eDoc
Session History
Login
Name:
Password:
Documentation
Help
Support Wiki
Direct access to
document ID:


          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
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.